document_title: Star

question_text: what is the true power source for the sun and other main sequence stars

question_tokens: what is the true power source for the sun and other main sequence stars

text: Star

text: Observation history

text: Historically, stars have been important to civilizations throughout the world. They have been part of religious practices and used for celestial navigation and orientation. Many ancient astronomers believed that stars were permanently affixed to a heavenly sphere and that they were immutable. By convention, astronomers grouped stars into constellations and used them to track the motions of the planets and the inferred position of the Sun.[5] The motion of the Sun against the background stars (and the horizon) was used to create calendars, which could be used to regulate agricultural practices.[7] The Gregorian calendar, currently used nearly everywhere in the world, is a solar calendar based on the angle of the Earth's rotational axis relative to its local star, the Sun.

text: The oldest accurately dated star chart was the result of ancient Egyptian astronomy in 1534 BC.[8] The earliest known star catalogues were compiled by the ancient Babylonian astronomers of Mesopotamia in the late 2nd millennium BC, during the Kassite Period (ca. 1531–1155 BC).[9]

text: The first star catalogue in Greek astronomy was created by Aristillus in approximately 300 BC, with the help of Timocharis.[10] The star catalog of Hipparchus (2nd century BC) included 1020 stars, and was used to assemble Ptolemy's star catalogue.[11] Hipparchus is known for the discovery of the first recorded nova (new star).[12] Many of the constellations and star names in use today derive from Greek astronomy.

text: In spite of the apparent immutability of the heavens, Chinese astronomers were aware that new stars could appear.[13] In 185 AD, they were the first to observe and write about a supernova, now known as the SN 185.[14] The brightest stellar event in recorded history was the SN 1006 supernova, which was observed in 1006 and written about by the Egyptian astronomer Ali ibn Ridwan and several Chinese astronomers.[15] The SN 1054 supernova, which gave birth to the Crab Nebula, was also observed by Chinese and Islamic astronomers.[16][17][18]

text: Medieval Islamic astronomers gave Arabic names to many stars that are still used today and they invented numerous astronomical instruments that could compute the positions of the stars. They built the first large observatory research institutes, mainly for the purpose of producing Zij star catalogues.[19] Among these, the Book of Fixed Stars (964) was written by the Persian astronomer Abd al-Rahman al-Sufi, who observed a number of stars, star clusters (including the Omicron Velorum and Brocchi's Clusters) and galaxies (including the Andromeda Galaxy).[20] According to A. Zahoor, in the 11th century, the Persian polymath scholar Abu Rayhan Biruni described the Milky Way galaxy as a multitude of fragments having the properties of nebulous stars, and also gave the latitudes of various stars during a lunar eclipse in 1019.[21]

text:
According to Josep Puig, the Andalusian astronomer Ibn Bajjah proposed that the Milky Way was made up of many stars that almost touched one another and appeared to be a continuous image due to the effect of refraction from sublunary material, citing his observation of the conjunction of Jupiter and Mars on 500 AH (1106/1107 AD) as evidence.[22]
Early European astronomers such as Tycho Brahe identified new stars in the night sky (later termed novae), suggesting that the heavens were not immutable. In 1584, Giordano Bruno suggested that the stars were like the Sun, and may have other planets, possibly even Earth-like, in orbit around them,[23] an idea that had been suggested earlier by the ancient Greek philosophers, Democritus and Epicurus,[24] and by medieval Islamic cosmologists[25] such as Fakhr al-Din al-Razi.[26] By the following century, the idea of the stars being the same as the Sun was reaching a consensus among astronomers. To explain why these stars exerted no net gravitational pull on the Solar System, Isaac Newton suggested that the stars were equally distributed in every direction, an idea prompted by the theologian Richard Bentley.[27]

text: The Italian astronomer Geminiano Montanari recorded observing variations in luminosity of the star Algol in 1667. Edmond Halley published the first measurements of the proper motion of a pair of nearby "fixed" stars, demonstrating that they had changed positions since the time of the ancient Greek astronomers Ptolemy and Hipparchus.[23]

text: William Herschel was the first astronomer to attempt to determine the distribution of stars in the sky. During the 1780s, he established a series of gauges in 600 directions and counted the stars observed along each line of sight. From this he deduced that the number of stars steadily increased toward one side of the sky, in the direction of the Milky Way core. His son John Herschel repeated this study in the southern hemisphere and found a corresponding increase in the same direction.[28] In addition to his other accomplishments, William Herschel is also noted for his discovery that some stars do not merely lie along the same line of sight, but are also physical companions that form binary star systems.

text: The science of stellar spectroscopy was pioneered by Joseph von Fraunhofer and Angelo Secchi. By comparing the spectra of stars such as Sirius to the Sun, they found differences in the strength and number of their absorption lines—the dark lines in stellar spectra caused by the atmosphere's absorption of specific frequencies. In 1865, Secchi began classifying stars into spectral types.[29] However, the modern version of the stellar classification scheme was developed by Annie J. Cannon during the 1900s.

text:
The first direct measurement of the distance to a star (61 Cygni at 11.4 light-years) was made in 1838 by Friedrich Bessel using the parallax technique. Parallax measurements demonstrated the vast separation of the stars in the heavens.[23] Observation of double stars gained increasing importance during the 19th century. In 1834, Friedrich Bessel observed changes in the proper motion of the star Sirius and inferred a hidden companion. Edward Pickering discovered the first spectroscopic binary in 1899 when he observed the periodic splitting of the spectral lines of the star Mizar in a 104-day period. Detailed observations of many binary star systems were collected by astronomers such as Friedrich Georg Wilhelm von Struve and S. W. Burnham, allowing the masses of stars to be determined from computation of orbital elements. The first solution to the problem of deriving an orbit of binary stars from telescope observations was made by Felix Savary in 1827.[30]
The twentieth century saw increasingly rapid advances in the scientific study of stars. The photograph became a valuable astronomical tool. Karl Schwarzschild discovered that the color of a star and, hence, its temperature, could be determined by comparing the visual magnitude against the photographic magnitude. The development of the photoelectric photometer allowed precise measurements of magnitude at multiple wavelength intervals. In 1921 Albert A. Michelson made the first measurements of a stellar diameter using an interferometer on the Hooker telescope at Mount Wilson Observatory.[31]

text: Important theoretical work on the physical structure of stars occurred during the first decades of the twentieth century. In 1913, the Hertzsprung-Russell diagram was developed, propelling the astrophysical study of stars. Successful models were developed to explain the interiors of stars and stellar evolution. Cecilia Payne-Gaposchkin first proposed that stars were made primarily of hydrogen and helium in her 1925 PhD thesis.[32] The spectra of stars were further understood through advances in quantum physics. This allowed the chemical composition of the stellar atmosphere to be determined.[33]

text:
With the exception of supernovae, individual stars have primarily been observed in the Local Group,[34] and especially in the visible part of the Milky Way (as demonstrated by the detailed star catalogues available for our
galaxy).[35] But some stars have been observed in the M100 galaxy of the Virgo Cluster, about 100 million light years from the Earth.[36]
In the Local Supercluster it is possible to see star clusters, and current telescopes could in principle observe faint individual stars in the Local Group[37] (see Cepheids). However, outside the Local Supercluster of galaxies, neither individual stars nor clusters of stars have been observed. The only exception is a faint image of a large star cluster containing hundreds of thousands of stars located at a distance of one billion light years[38]—ten times further than the most distant star cluster previously observed.

text: In February 2018, astronomers reported, for the first time, a signal of the reionization epoch, an indirect detection of light from the earliest stars formed - about 180 million years after the Big Bang.[39]

text: In April, 2018, astronomers reported the detection of the most distant "ordinary" (i.e., main sequence) star, named Icarus (formally, MACS J1149 Lensed Star 1), at 9 billion light-years away from Earth.[40][41]

text: In May 2018, astronomers reported the detection of the most distant oxygen ever detected in the Universe - and the most distant galaxy every observed by Atacama Large Millimeter Array or the Very Large Telescope - with the team inferring that the signal was emitted 13.3 billion years ago (or 500 million years after the Big Bang. They found that the observed brightness of the galaxy is well-explained by a model where the onset of star formation corresponds to only 250 million years after the Universe began, corresponding to a redshift of about 15.[42]

text: Designations

text: The concept of a constellation was known to exist during the Babylonian period. Ancient sky watchers imagined that prominent arrangements of stars formed patterns, and they associated these with particular aspects of nature or their myths. Twelve of these formations lay along the band of the ecliptic and these became the basis of astrology.[43] Many of the more prominent individual stars were also given names, particularly with Arabic or Latin designations.

text: As well as certain constellations and the Sun itself, individual stars have their own myths.[44] To the Ancient Greeks, some "stars", known as planets (Greek πλανήτης (planētēs), meaning "wanderer"), represented various important deities, from which the names of the planets Mercury, Venus, Mars, Jupiter and Saturn were taken.[44] (Uranus and Neptune were also Greek and Roman gods, but neither planet was known in Antiquity because of their low brightness. Their names were assigned by later astronomers.)

text: Circa 1600, the names of the constellations were used to name the stars in the corresponding regions of the sky. The German astronomer Johann Bayer created a series of star maps and applied Greek letters as designations to the stars in each constellation. Later a numbering system based on the star's right ascension was invented and added to John Flamsteed's star catalogue in his book "Historia coelestis Britannica" (the 1712 edition), whereby this numbering system came to be called Flamsteed designation or Flamsteed numbering.[45][46]

text: The only internationally recognized authority for naming celestial bodies is the International Astronomical Union (IAU).[47] The International Astronomical Union maintains the Working Group on Star Names (WGSN)[48] which catalogs and standardizes proper names for stars. A number of private companies sell names of stars, which the British Library calls an unregulated commercial enterprise.[49][50] The IAU has disassociated itself from this commercial practice, and these names are neither recognized by the IAU, professional astronomers, nor the amateur astronomy community.[51] One such star-naming company is the International Star Registry, which, during the 1980s, was accused of deceptive practice for making it appear that the assigned name was official. This now-discontinued ISR practice was informally labeled a scam and a fraud,[52][53][54][55] and the New York City Department of Consumer Affairs issued a violation against ISR for engaging in a deceptive trade practice.[56][57]

text: Units of measurement

text: Although stellar parameters can be expressed in SI units or CGS units, it is often most convenient to express mass, luminosity, and radii in solar units, based on the characteristics of the Sun. In 2015, the IAU defined a set of nominal solar values (defined as SI constants, without uncertainties) which can be used for quoting stellar parameters:

text:
nominal solar luminosity:

L⊙ = 3.828 × 1026 W [58]

nominal solar radius

R⊙ = 6.957 × 108 m [58]

text:
The solar mass M⊙ was not explicitly defined by the IAU due to the large relative uncertainty (10−4) of the Newtonian gravitational constant G. However, since the product of the Newtonian gravitational constant and solar mass
together (GM⊙) has been determined to much greater precision, the IAU defined the nominal solar mass parameter to be:

text:
nominal solar mass parameter:

GM⊙ = 1.3271244 × 1020 m3 s−2 [58]

text: However, one can combine the nominal solar mass parameter with the most recent (2014) CODATA estimate of the Newtonian gravitational constant G to derive the solar mass to be approximately 1.9885 × 1030 kg. Although the exact values for the luminosity, radius, mass parameter, and mass may vary slightly in the future due to observational uncertainties, the 2015 IAU nominal constants will remain the same SI values as they remain useful measures for quoting stellar parameters.

text: Large lengths, such as the radius of a giant star or the semi-major axis of a binary star system, are often expressed in terms of the astronomical unit — approximately equal to the mean distance between the Earth and the Sun (150 million km or approximately 93 million miles). In 2012, the IAU defined the astronomical constant to be an exact length in meters: 149,597,870,700 m.[58]

text: Formation and evolution

text:
Stars condense from regions of space of higher matter density, yet those regions are less dense than within a vacuum chamber. These regions – known as molecular clouds – consist mostly of hydrogen, with about 23 to 28 percent helium and a few percent heavier elements. One example of such a star-forming region is the Orion Nebula.[59] Most stars form in groups of dozens to hundreds of thousands of stars.[60]
Massive stars in these groups may powerfully illuminate those clouds, ionizing the hydrogen, and creating H II regions. Such feedback effects, from star formation, may ultimately disrupt the cloud and prevent further star formation.

text: All stars spend the majority of their existence as main sequence stars, fueled primarily by the nuclear fusion of hydrogen into helium within their cores. However, stars of different masses have markedly different properties at various stages of their development. The ultimate fate of more massive stars differs from that of less massive stars, as do their luminosities and the impact they have on their environment. Accordingly, astronomers often group stars by their mass:[61]

text:
Very low mass stars, with masses below 0.5 M☉, are fully convective and distribute helium evenly throughout the whole star while on the main sequence. Therefore, they never undergo shell burning, never become red giants, which cease fusing and become helium white dwarfs and slowly cool after exhausting their hydrogen.[62] However, as the lifetime of 0.5 M☉ stars is longer than the age of the universe, no such star has yet reached the white dwarf stage.
Low mass stars (including the Sun), with a mass between 0.5 M☉ and 1.8–2.5 M☉  depending on composition, do become red giants as their core hydrogen is depleted and they begin to burn helium in core in a helium flash; they develop a degenerate carbon-oxygen core later on the asymptotic giant branch; they finally blow off their outer shell as a planetary nebula and leave behind their core in the form of a white dwarf.
Intermediate-mass stars, between 1.8–2.5 M☉ and 5–10 M☉, pass through evolutionary stages similar to low mass stars, but after a relatively short period on the red giant branch they ignite helium without a flash and spend an extended period in the red clump before forming a degenerate carbon-oxygen core.
Massive stars generally have a minimum mass of 7–10 M☉ (possibly as low as 5–6 M☉). After exhausting the hydrogen at the core these stars become supergiants and go on to fuse elements heavier than helium. They end their lives when their cores collapse and they explode as supernovae.

text: Star formation

text: The formation of a star begins with gravitational instability within a molecular cloud, caused by regions of higher density – often triggered by compression of clouds by radiation from massive stars, expanding bubbles in the interstellar medium, the collision of different molecular clouds, or the collision of galaxies (as in a starburst galaxy).[63][64] When a region reaches a sufficient density of matter to satisfy the criteria for Jeans instability, it begins to collapse under its own gravitational force.[65]

text: As the cloud collapses, individual conglomerations of dense dust and gas form "Bok globules". As a globule collapses and the density increases, the gravitational energy converts into heat and the temperature rises. When the protostellar cloud has approximately reached the stable condition of hydrostatic equilibrium, a protostar forms at the core.[66] These pre-main-sequence stars are often surrounded by a protoplanetary disk and powered mainly by the conversion of gravitational energy. The period of gravitational contraction lasts about 10 to 15 million years.

text:
Early stars of less than 2 M☉ are called T Tauri stars, while those with greater mass are Herbig Ae/Be stars. These newly formed stars emit jets of gas along their axis of rotation, which may reduce the angular momentum of the collapsing star and result in small patches of nebulosity known as Herbig–Haro objects.[67][68]
These jets, in combination with radiation from nearby massive stars, may help to drive away the surrounding cloud from which the star was formed.[69]

text: Early in their development, T Tauri stars follow the Hayashi track—they contract and decrease in luminosity while remaining at roughly the same temperature. Less massive T Tauri stars follow this track to the main sequence, while more massive stars turn onto the Henyey track.

text: Most stars are observed to be members of binary star systems, and the properties of those binaries are the result of the conditions in which they formed.[70] A gas cloud must lose its angular momentum in order to collapse and form a star. The fragmentation of the cloud into multiple stars distributes some of that angular momentum. The primordial binaries transfer some angular momentum by gravitational interactions during close encounters with other stars in young stellar clusters. These interactions tend to split apart more widely separated (soft) binaries while causing hard binaries to become more tightly bound. This produces the separation of binaries into their two observed populations distributions.

text: Main sequence

text:
Stars spend about 90% of their existence fusing hydrogen into helium in high-temperature and high-pressure reactions near the core. Such stars are said to be on the main sequence, and are called dwarf stars. Starting at zero-age main sequence, the proportion of helium in a star's core will steadily increase, the rate of nuclear fusion at the core will slowly increase, as will the star's temperature and luminosity.[71]
The Sun, for example, is estimated to have increased in luminosity by about 40% since it reached the main sequence 4.6 billion (4.6 × 109) years ago.[72]

text: Every star generates a stellar wind of particles that causes a continual outflow of gas into space. For most stars, the mass lost is negligible. The Sun loses 10−14 M☉ every year,[73] or about 0.01% of its total mass over its entire lifespan. However, very massive stars can lose 10−7 to 10−5 M☉ each year, significantly affecting their evolution.[74] Stars that begin with more than 50 M☉ can lose over half their total mass while on the main sequence.[75]

text: The time a star spends on the main sequence depends primarily on the amount of fuel it has and the rate at which it fuses it. The Sun is expected to live 10 billion (1010) years. Massive stars consume their fuel very rapidly and are short-lived. Low mass stars consume their fuel very slowly. Stars less massive than 0.25 M☉, called red dwarfs, are able to fuse nearly all of their mass while stars of about 1 M☉ can only fuse about 10% of their mass. The combination of their slow fuel-consumption and relatively large usable fuel supply allows low mass stars to last about one trillion (1012) years; the most extreme of 0.08 M☉) will last for about 12 trillion years. Red dwarfs become hotter and more luminous as they accumulate helium. When they eventually run out of hydrogen, they contract into a white dwarf and decline in temperature.[62] However, since the lifespan of such stars is greater than the current age of the universe (13.8 billion years), no stars under about 0.85 M☉[76] are expected to have moved off the main sequence.

text: Besides mass, the elements heavier than helium can play a significant role in the evolution of stars. Astronomers label all elements heavier than helium "metals", and call the chemical concentration of these elements in a star, its metallicity. A star's metallicity can influence the time the star takes to burn its fuel, and controls the formation of its magnetic fields,[77] which affects the strength of its stellar wind.[78] Older, population II stars have substantially less metallicity than the younger, population I stars due to the composition of the molecular clouds from which they formed. Over time, such clouds become increasingly enriched in heavier elements as older stars die and shed portions of their atmospheres.

text: Post–main sequence

text: As stars of at least 0.4 M☉[2] exhaust their supply of hydrogen at their core, they start to fuse hydrogen in a shell outside the helium core. Their outer layers expand and cool greatly as they form a red giant. In about 5 billion years, when the Sun enters the helium burning phase, it will expand to a maximum radius of roughly 1 astronomical unit (150 million kilometres), 250 times its present size, and lose 30% of its current mass.[72][79]

text: As the hydrogen shell burning produces more helium, the core increases in mass and temperature. In a red giant of up to 2.25 M☉, the mass of the helium core becomes degenerate prior to helium fusion. Finally, when the temperature increases sufficiently, helium fusion begins explosively in what is called a helium flash, and the star rapidly shrinks in radius, increases its surface temperature, and moves to the horizontal branch of the HR diagram. For more massive stars, helium core fusion starts before the core becomes degenerate, and the star spends some time in the red clump, slowly burning helium, before the outer convective envelope collapses and the star then moves to the horizontal branch.[4]

text: After the star has fused the helium of its core, the carbon product fuses producing a hot core with an outer shell of fusing helium. The star then follows an evolutionary path called the asymptotic giant branch (AGB) that parallels the other described red giant phase, but with a higher luminosity. The more massive AGB stars may undergo a brief period of carbon fusion before the core becomes degenerate.

text: Massive stars

text: During their helium-burning phase, a star of more than 9 solar masses expands to form first a blue and then a red supergiant. Particularly massive stars may evolve to a Wolf-Rayet star, characterised by spectra dominated by emission lines of elements heavier than hydrogen, which have reached the surface due to strong convection and intense mass loss.

text: When helium is exhausted at the core of a massive star, the core contracts and the temperature and pressure rises enough to fuse carbon (see Carbon-burning process). This process continues, with the successive stages being fueled by neon (see neon-burning process), oxygen (see oxygen-burning process), and silicon (see silicon-burning process). Near the end of the star's life, fusion continues along a series of onion-layer shells within a massive star. Each shell fuses a different element, with the outermost shell fusing hydrogen; the next shell fusing helium, and so forth.[80]

text: The final stage occurs when a massive star begins producing iron. Since iron nuclei are more tightly bound than any heavier nuclei, any fusion beyond iron does not produce a net release of energy. To a very limited degree such a process proceeds, but it consumes energy. Likewise, since they are more tightly bound than all lighter nuclei, such energy cannot be released by fission.[81]

text: Collapse

text: As a star's core shrinks, the intensity of radiation from that surface increases, creating such radiation pressure on the outer shell of gas that it will push those layers away, forming a planetary nebula. If what remains after the outer atmosphere has been shed is less than 1.4 M☉, it shrinks to a relatively tiny object about the size of Earth, known as a white dwarf. White dwarfs lack the mass for further gravitational compression to take place.[82] The electron-degenerate matter inside a white dwarf is no longer a plasma, even though stars are generally referred to as being spheres of plasma. Eventually, white dwarfs fade into black dwarfs over a very long period of time.

text: In massive stars, fusion continues until the iron core has grown so large (more than 1.4 M☉) that it can no longer support its own mass. This core will suddenly collapse as its electrons are driven into its protons, forming neutrons, neutrinos, and gamma rays in a burst of electron capture and inverse beta decay. The shockwave formed by this sudden collapse causes the rest of the star to explode in a supernova. Supernovae become so bright that they may briefly outshine the star's entire home galaxy. When they occur within the Milky Way, supernovae have historically been observed by naked-eye observers as "new stars" where none seemingly existed before.[83]

text: A supernova explosion blows away the star's outer layers, leaving a remnant such as the Crab Nebula.[83] The core is compressed into a neutron star, which sometimes manifests itself as a pulsar or X-ray burster. In the case of the largest stars, the remnant is a black hole greater than  4 M☉.[84] In a neutron star the matter is in a state known as neutron-degenerate matter, with a more exotic form of degenerate matter, QCD matter, possibly present in the core. Within a black hole, the matter is in a state that is not currently understood.

text: The blown-off outer layers of dying stars include heavy elements, which may be recycled during the formation of new stars. These heavy elements allow the formation of rocky planets. The outflow from supernovae and the stellar wind of large stars play an important part in shaping the interstellar medium.[83]

text: Binary stars

text: The post–main-sequence evolution of binary stars may be significantly different from the evolution of single stars of the same mass. If stars in a binary system are sufficiently close, when one of the stars expands to become a red giant it may overflow its Roche lobe, the region around a star where material is gravitationally bound to that star, leading to transfer of material to the other. When the Roche lobe is violated, a variety of phenomena can result, including contact binaries, common-envelope binaries, cataclysmic variables, and type Ia supernovae.

text: Distribution

text: Stars are not spread uniformly across the universe, but are normally grouped into galaxies along with interstellar gas and dust. A typical galaxy contains hundreds of billions of stars, and there are more than 100 billion (1011) galaxies in the observable universe.[85] In 2010, one estimate of the number of stars in the observable universe was 300 sextillion (3 × 1023).[86][87] While it is often believed that stars only exist within galaxies, intergalactic stars have been discovered.[88]

text: A multi-star system consists of two or more gravitationally bound stars that orbit each other. The simplest and most common multi-star system is a binary star, but systems of three or more stars are also found. For reasons of orbital stability, such multi-star systems are often organized into hierarchical sets of binary stars.[89] Larger groups called star clusters also exist. These range from loose stellar associations with only a few stars, up to enormous globular clusters with hundreds of thousands of stars. Such systems orbit their host galaxy.

text: It has been a long-held assumption that the majority of stars occur in gravitationally bound, multiple-star systems. This is particularly true for very massive O and B class stars, where 80% of the stars are believed to be part of multiple-star systems. The proportion of single star systems increases with decreasing star mass, so that only 25% of red dwarfs are known to have stellar companions. As 85% of all stars are red dwarfs, most stars in the Milky Way are likely single from birth.[90]

text: The nearest star to the Earth, apart from the Sun, is Proxima Centauri, which is 39.9 trillion kilometres, or 4.2 light-years. Travelling at the orbital speed of the Space Shuttle (8 kilometres per second—almost 30,000 kilometres per hour), it would take about 150,000 years to arrive.[91] This is typical of stellar separations in galactic discs.[92] Stars can be much closer to each other in the centres of galaxies and in globular clusters, or much farther apart in galactic halos.

text: Due to the relatively vast distances between stars outside the galactic nucleus, collisions between stars are thought to be rare. In denser regions such as the core of globular clusters or the galactic center, collisions can be more common.[93] Such collisions can produce what are known as blue stragglers. These abnormal stars have a higher surface temperature than the other main sequence stars with the same luminosity of the cluster to which it belongs.[94]

text: Characteristics

text: Almost everything about a star is determined by its initial mass, including such characteristics as luminosity, size, evolution, lifespan, and its eventual fate.

text: Age

text: Most stars are between 1 billion and 10 billion years old. Some stars may even be close to 13.8 billion years old—the observed age of the universe. The oldest star yet discovered, HD 140283, nicknamed Methuselah star, is an estimated 14.46 ± 0.8 billion years old.[95] (Due to the uncertainty in the value, this age for the star does not conflict with the age of the Universe, determined by the Planck satellite as 13.799 ± 0.021).[95][96]

text: The more massive the star, the shorter its lifespan, primarily because massive stars have greater pressure on their cores, causing them to burn hydrogen more rapidly. The most massive stars last an average of a few million years, while stars of minimum mass (red dwarfs) burn their fuel very slowly and can last tens to hundreds of billions of years.[97][98]

text: Chemical composition

text: When stars form in the present Milky Way galaxy they are composed of about 71% hydrogen and 27% helium,[99] as measured by mass, with a small fraction of heavier elements. Typically the portion of heavy elements is measured in terms of the iron content of the stellar atmosphere, as iron is a common element and its absorption lines are relatively easy to measure. The portion of heavier elements may be an indicator of the likelihood that the star has a planetary system.[100]

text: The star with the lowest iron content ever measured is the dwarf HE1327-2326, with only 1/200,000th the iron content of the Sun.[101] By contrast, the super-metal-rich star μ Leonis has nearly double the abundance of iron as the Sun, while the planet-bearing star 14 Herculis has nearly triple the iron.[102] There also exist chemically peculiar stars that show unusual abundances of certain elements in their spectrum; especially chromium and rare earth elements.[103] Stars with cooler outer atmospheres, including the Sun, can form various diatomic and polyatomic molecules.[104]

text: Diameter

text: Due to their great distance from the Earth, all stars except the Sun appear to the unaided eye as shining points in the night sky that twinkle because of the effect of the Earth's atmosphere. The Sun is also a star, but it is close enough to the Earth to appear as a disk instead, and to provide daylight. Other than the Sun, the star with the largest apparent size is R Doradus, with an angular diameter of only 0.057 arcseconds.[105]

text: The disks of most stars are much too small in angular size to be observed with current ground-based optical telescopes, and so interferometer telescopes are required to produce images of these objects. Another technique for measuring the angular size of stars is through occultation. By precisely measuring the drop in brightness of a star as it is occulted by the Moon (or the rise in brightness when it reappears), the star's angular diameter can be computed.[106]

text: Stars range in size from neutron stars, which vary anywhere from 20 to 40 km (25 mi) in diameter, to supergiants like Betelgeuse in the Orion constellation, which has a diameter 7002887000000000000♠887±203[107] to 950[108] times that of our sun. Betelgeuse, however, has a much lower density than the Sun.[109]

text: Kinematics

text: The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding galaxy. The components of motion of a star consist of the radial velocity toward or away from the Sun, and the traverse angular movement, which is called its proper motion.

text: Radial velocity is measured by the doppler shift of the star's spectral lines, and is given in units of km/s. The proper motion of a star, its parallax, is determined by precise astrometric measurements in units of milli-arc seconds (mas) per year. With knowledge of the star's parallax and its distance, the proper motion velocity can be calculated. Together with the radial velocity, the total velocity can be calculated. Stars with high rates of proper motion are likely to be relatively close to the Sun, making them good candidates for parallax measurements.[111]

text: When both rates of movement are known, the space velocity of the star relative to the Sun or the galaxy can be computed. Among nearby stars, it has been found that younger population I stars have generally lower velocities than older, population II stars. The latter have elliptical orbits that are inclined to the plane of the galaxy.[112] A comparison of the kinematics of nearby stars has allowed astronomers to trace their origin to common points in giant molecular clouds, and are referred to as stellar associations.[113]

text: Magnetic field

text: The magnetic field of a star is generated within regions of the interior where convective circulation occurs. This movement of conductive plasma functions like a dynamo, wherein the movement of electrical charges induce magnetic fields, as does a mechanical dynamo. Those magnetic fields have a great range that extend throughout and beyond the star. The strength of the magnetic field varies with the mass and composition of the star, and the amount of magnetic surface activity depends upon the star's rate of rotation. This surface activity produces starspots, which are regions of strong magnetic fields and lower than normal surface temperatures. Coronal loops are arching magnetic field flux lines that rise from a star's surface into the star's outer atmosphere, its corona. The coronal loops can be seen due to the plasma they conduct along their length. Stellar flares are bursts of high-energy particles that are emitted due to the same magnetic activity.[114]

text:
Young, rapidly rotating stars tend to have high levels of surface activity because of their magnetic field. The magnetic field can act upon a star's stellar wind, functioning as a brake to gradually slow the rate of rotation with time. Thus, older stars such as the Sun have a much slower rate of rotation and a lower level of surface activity. The activity levels of slowly rotating stars tend to vary in a cyclical manner and can shut down altogether for periods of time.[115] During
the Maunder Minimum, for example, the Sun underwent a
70-year period with almost no sunspot activity.

text: Mass

text:
One of the most massive stars known is Eta Carinae,[116] which,
with 100–150 times as much mass as the Sun, will have a lifespan of only several million years. Studies of the most massive open clusters suggests 150 M☉ as an upper limit for stars in the current era of the universe.[117] This
represents an empirical value for the theoretical limit on the mass of forming stars due to increasing radiation pressure on the accreting gas cloud. Several stars in the R136 cluster in the Large Magellanic Cloud have been measured with larger masses,[118] but
it has been determined that they could have been created through the collision and merger of massive stars in close binary systems, sidestepping the 150 M☉ limit on massive star formation.[119]

text:
The first stars to form after the Big Bang may have been larger, up to 300 M☉,[120] due
to the complete absence of elements heavier than lithium in their composition. This generation of supermassive population III stars is likely to have existed in the very early universe (i.e., they are observed to have a high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life. In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60.[121][122]

text:
With a mass only 80 times that of Jupiter (MJ), 2MASS J0523-1403 is the smallest known star undergoing nuclear fusion in its core.[123] For
stars with metallicity similar to the Sun, the theoretical minimum mass the star can have and still undergo fusion at the core, is estimated to be about 75 MJ.[124][125] When the metallicity is very low, however, the minimum star size seems to be about 8.3% of the solar mass, or about 87 MJ.[125][126] Smaller bodies called brown dwarfs, occupy a poorly defined grey area between stars and gas giants.

text: The combination of the radius and the mass of a star determines its surface gravity. Giant stars have a much lower surface gravity than do main sequence stars, while the opposite is the case for degenerate, compact stars such as white dwarfs. The surface gravity can influence the appearance of a star's spectrum, with higher gravity causing a broadening of the absorption lines.[33]

text: Rotation

text: The rotation rate of stars can be determined through spectroscopic measurement, or more exactly determined by tracking their starspots. Young stars can have a rotation greater than 100 km/s at the equator. The B-class star Achernar, for example, has an equatorial velocity of about 225 km/s or greater, causing its equator to bulge outward and giving it an equatorial diameter that is more than 50% greater than between the poles. This rate of rotation is just below the critical velocity of 300 km/s at which speed the star would break apart.[127] By contrast, the Sun rotates once every 25–35 days depending on latitude,[128] with an equatorial velocity of 1.93 km/s.[129] A main sequence star's magnetic field and the stellar wind serve to slow its rotation by a significant amount as it evolves on the main sequence.[130]

text: Degenerate stars have contracted into a compact mass, resulting in a rapid rate of rotation. However they have relatively low rates of rotation compared to what would be expected by conservation of angular momentum—the tendency of a rotating body to compensate for a contraction in size by increasing its rate of spin. A large portion of the star's angular momentum is dissipated as a result of mass loss through the stellar wind.[131] In spite of this, the rate of rotation for a pulsar can be very rapid. The pulsar at the heart of the Crab nebula, for example, rotates 30 times per second.[132] The rotation rate of the pulsar will gradually slow due to the emission of radiation.[133]

text: Temperature

text: The surface temperature of a main sequence star is determined by the rate of energy production of its core and by its radius, and is often estimated from the star's color index.[134] The temperature is normally given in terms of an effective temperature,  which is the temperature of an idealized black body that radiates its energy at the same luminosity per surface area as the star. Note that the effective temperature is only a representative of the surface, as the temperature increases toward the core.[135] The temperature in the core region of a star is several million kelvins.[136]

text: The stellar temperature will determine the rate of ionization of various elements, resulting in characteristic absorption lines in the spectrum. The surface temperature of a star, along with its visual absolute magnitude and absorption features, is used to classify a star (see classification below).[33]

text: Massive main sequence stars can have surface temperatures of 50,000 K. Smaller stars such as the Sun have surface temperatures of a few thousand K. Red giants have relatively low surface temperatures of about 3,600 K; but they also have a high luminosity due to their large exterior surface area.[137]

text: Radiation

text:
The energy produced by stars, a product of nuclear fusion, radiates to space as both electromagnetic radiation and particle radiation. The particle radiation emitted by a star is manifested as the stellar wind,[138] which
streams from the outer layers as electrically charged protons and alpha and beta particles. Although almost massless, there also exists a steady stream of neutrinos emanating from the star's core.

text: The production of energy at the core is the reason stars shine so brightly: every time two or more atomic nuclei fuse together to form a single atomic nucleus of a new heavier element, gamma ray photons are released from the nuclear fusion product. This energy is converted to other forms of electromagnetic energy of lower frequency, such as visible light, by the time it reaches the star's outer layers.

text:
The color of a star, as determined by the most intense frequency of the visible light, depends on the temperature of the star's outer layers, including its photosphere.[139] Besides
visible light, stars also emit forms of electromagnetic radiation that are invisible to the human eye. In fact, stellar electromagnetic radiation spans the entire electromagnetic spectrum, from the longest wavelengths of radio waves through infrared, visible light, ultraviolet, to the shortest of X-rays, and gamma rays. From the standpoint of total energy emitted by a star, not all components of stellar electromagnetic radiation are significant, but all frequencies provide insight into the star's physics.

text: Using the stellar spectrum, astronomers can also determine the surface temperature, surface gravity, metallicity and rotational velocity of a star. If the distance of the star is found, such as by measuring the parallax, then the luminosity of the star can be derived. The mass, radius, surface gravity, and rotation period can then be estimated based on stellar models. (Mass can be calculated for stars in binary systems by measuring their orbital velocities and distances. Gravitational microlensing has been used to measure the mass of a single star.[140]) With these parameters, astronomers can also estimate the age of the star.[141]

text: Luminosity

text: The luminosity of a star is the amount of light and other forms of radiant energy it radiates per unit of time. It has units of power. The luminosity of a star is determined by its radius and surface temperature. Many stars do not radiate uniformly across their entire surface. The rapidly rotating star Vega, for example, has a higher energy flux (power per unit area) at its poles than along its equator.[142]

text:
Patches of the star's surface with a lower temperature and luminosity than average are known as starspots. Small, dwarf stars such as our Sun generally have essentially featureless disks with only small starspots.  Giant stars have much larger, more obvious starspots,[143] and
they also exhibit strong stellar limb darkening. That is, the brightness decreases towards the edge of the stellar disk.[144] Red
dwarf flare stars such as UV Ceti may also possess prominent starspot features.[145]

text: Magnitude

text: The apparent brightness of a star is expressed in terms of its apparent magnitude. It is a function of the star's luminosity, its distance from Earth, the extinction effect of interstellar dust and gas, and the altering of the star's light as it passes through Earth's atmosphere. Intrinsic or absolute magnitude is directly related to a star's luminosity, and is what the apparent magnitude a star would be if the distance between the Earth and the star were 10 parsecs (32.6 light-years).

text:
Number of stars brighter than magnitude

Apparentmagnitude

Number of stars[146]

0

4

1

15

2

48

3

171

4

513

5

1,602

6

4,800

7

14,000

text: Both the apparent and absolute magnitude scales are logarithmic units: one whole number difference in magnitude is equal to a brightness variation of about 2.5 times[147] (the 5th root of 100 or approximately 2.512). This means that a first magnitude star (+1.00) is about 2.5 times brighter than a second magnitude (+2.00) star, and about 100 times brighter than a sixth magnitude star (+6.00). The faintest stars visible to the naked eye under good seeing conditions are about magnitude +6.

text: On both apparent and absolute magnitude scales, the smaller the magnitude number, the brighter the star; the larger the magnitude number, the fainter the star. The brightest stars, on either scale, have negative magnitude numbers. The variation in brightness (ΔL) between two stars is calculated by subtracting the magnitude number of the brighter star (mb) from the magnitude number of the fainter star (mf), then using the difference as an exponent for the base number 2.512; that is to say:

text: Relative to both luminosity and distance from Earth, a star's absolute magnitude (M) and apparent magnitude (m) are not equivalent;[147] for example, the bright star Sirius has an apparent magnitude of −1.44, but it has an absolute magnitude of +1.41.

text: The Sun has an apparent magnitude of −26.7, but its absolute magnitude is only +4.83. Sirius, the brightest star in the night sky as seen from Earth, is approximately 23 times more luminous than the Sun, while Canopus, the second brightest star in the night sky with an absolute magnitude of −5.53, is approximately 14,000 times more luminous than the Sun. Despite Canopus being vastly more luminous than Sirius, however, Sirius appears brighter than Canopus. This is because Sirius is merely 8.6 light-years from the Earth, while Canopus is much farther away at a distance of 310 light-years.

text: As of 2006, the star with the highest known absolute magnitude is LBV 1806-20, with a magnitude of −14.2. This star is at least 5,000,000 times more luminous than the Sun.[148] The least luminous stars that are currently known are located in the NGC 6397 cluster. The faintest red dwarfs in the cluster were magnitude 26, while a 28th magnitude white dwarf was also discovered. These faint stars are so dim that their light is as bright as a birthday candle on the Moon when viewed from the Earth.[149]

text: Classification

text:
Surface temperature ranges fordifferent stellar classes[150]

Class

Temperature

Sample star

O

33,000 K or more

Zeta Ophiuchi

B

10,500–30,000 K

Rigel

A

7,500–10,000 K

Altair

F

6,000–7,200 K

Procyon A

G

5,500–6,000 K

Sun

K

4,000–5,250 K

Epsilon Indi

M

2,600–3,850 K

Proxima Centauri

text: The current stellar classification system originated in the early 20th century, when stars were classified from A to Q based on the strength of the hydrogen line.[151] It was thought that the hydrogen line strength was a simple linear function of temperature. Instead, it was more complicated: it strengthened with increasing temperature, peaked near 9000 K, and then declined at greater temperatures. The classifications were since reordered by temperature, on which the modern scheme is based.[152]

text: Stars are given a single-letter classification according to their spectra, ranging from type O, which are very hot, to M, which are so cool that molecules may form in their atmospheres. The main classifications in order of decreasing surface temperature are: O, B, A, F, G, K, and M. A variety of rare spectral types are given special classifications. The most common of these are types L and T, which classify the coldest low-mass stars and brown dwarfs. Each letter has 10 sub-divisions, numbered from 0 to 9, in order of decreasing temperature. However, this system breaks down at extreme high temperatures as classes O0 and O1 may not exist.[153]

text: In addition, stars may be classified by the luminosity effects found in their spectral lines, which correspond to their spatial size and is determined by their surface gravity. These range from 0 (hypergiants) through III (giants) to V (main sequence dwarfs); some authors add VII (white dwarfs). Main sequence stars fall along a narrow, diagonal band when graphed according to their absolute magnitude and spectral type.[153] The Sun is a main sequence G2V yellow dwarf of intermediate temperature and ordinary size.

text: Additional nomenclature, in the form of lower-case letters added to the end of the spectral type to indicate peculiar features of the spectrum. For example, an "e" can indicate the presence of emission lines; "m" represents unusually strong levels of metals, and "var" can mean variations in the spectral type.[153]

text: White dwarf stars have their own class that begins with the letter D. This is further sub-divided into the classes DA, DB, DC, DO, DZ, and DQ, depending on the types of prominent lines found in the spectrum. This is followed by a numerical value that indicates the temperature.[154]

text: Variable stars

text: Variable stars have periodic or random changes in luminosity because of intrinsic or extrinsic properties. Of the intrinsically variable stars, the primary types can be subdivided into three principal groups.

text: During their stellar evolution, some stars pass through phases where they can become pulsating variables. Pulsating variable stars vary in radius and luminosity over time, expanding and contracting with periods ranging from minutes to years, depending on the size of the star. This category includes Cepheid and Cepheid-like stars, and long-period variables such as Mira.[155]

text: Eruptive variables are stars that experience sudden increases in luminosity because of flares or mass ejection events.[155] This group includes protostars, Wolf-Rayet stars, and flare stars, as well as giant and supergiant stars.

text: Cataclysmic or explosive variable stars are those that undergo a dramatic change in their properties. This group includes novae and supernovae. A binary star system that includes a nearby white dwarf can produce certain types of these spectacular stellar explosions, including the nova and a Type 1a supernova.[4] The explosion is created when the white dwarf accretes hydrogen from the companion star, building up mass until the hydrogen undergoes fusion.[156] Some novae are also recurrent, having periodic outbursts of moderate amplitude.[155]

text: Stars can also vary in luminosity because of extrinsic factors, such as eclipsing binaries, as well as rotating stars that produce extreme starspots.[155] A notable example of an eclipsing binary is Algol, which regularly varies in magnitude from 2.1 to 3.4 over a period of 2.87 days.[157]

text: Structure

text: The interior of a stable star is in a state of hydrostatic equilibrium: the forces on any small volume almost exactly counterbalance each other. The balanced forces are inward gravitational force and an outward force due to the pressure gradient within the star. The pressure gradient is established by the temperature gradient of the plasma; the outer part of the star is cooler than the core. The temperature at the core of a main sequence or giant star is at least on the order of 107 K. The resulting temperature and pressure at the hydrogen-burning core of a main sequence star are sufficient for nuclear fusion to occur and for sufficient energy to be produced to prevent further collapse of the star.[158][159]

text: As atomic nuclei are fused in the core, they emit energy in the form of gamma rays. These photons interact with the surrounding plasma, adding to the thermal energy at the core. Stars on the main sequence convert hydrogen into helium, creating a slowly but steadily increasing proportion of helium in the core. Eventually the helium content becomes predominant, and energy production ceases at the core. Instead, for stars of more than 0.4 M☉, fusion occurs in a slowly expanding shell around the degenerate helium core.[160]

text: In addition to hydrostatic equilibrium, the interior of a stable star will also maintain an energy balance of thermal equilibrium. There is a radial temperature gradient throughout the interior that results in a flux of energy flowing toward the exterior. The outgoing flux of energy leaving any layer within the star will exactly match the incoming flux from below.

text: The radiation zone is the region of the stellar interior where the flux of energy outward is dependent on radiative heat transfer, since convective heat transfer is inefficient in that zone. In this region the plasma will not be perturbed, and any mass motions will die out. If this is not the case, however, then the plasma becomes unstable and convection will occur, forming a convection zone. This can occur, for example, in regions where very high energy fluxes occur, such as near the core or in areas with high opacity (making radiatative heat transfer inefficient) as in the outer envelope.[159]

text: The occurrence of convection in the outer envelope of a main sequence star depends on the star's mass. Stars with several times the mass of the Sun have a convection zone deep within the interior and a radiative zone in the outer layers. Smaller stars such as the Sun are just the opposite, with the convective zone located in the outer layers.[161] Red dwarf stars with less than 0.4 M☉ are convective throughout, which prevents the accumulation of a helium core.[2] For most stars the convective zones will also vary over time as the star ages and the constitution of the interior is modified.[159]

text: The photosphere is that portion of a star that is visible to an observer. This is the layer at which the plasma of the star becomes transparent to photons of light. From here, the energy generated at the core becomes free to propagate into space. It is within the photosphere that sun spots, regions of lower than average temperature, appear.

text: Above the level of the photosphere is the stellar atmosphere. In a main sequence star such as the Sun, the lowest level of the atmosphere, just above the photosphere, is the thin chromosphere region, where spicules appear and stellar flares begin. Above this is the transition region, where the temperature rapidly increases within a distance of only 100 km (62 mi). Beyond this is the corona, a volume of super-heated plasma that can extend outward to several million kilometres.[162] The existence of a corona appears to be dependent on a convective zone in the outer layers of the star.[161] Despite its high temperature, and the corona emits very little light, due to its low gas density. The corona region of the Sun is normally only visible during a solar eclipse.

text: From the corona, a stellar wind of plasma particles expands outward from the star, until it interacts with the interstellar medium. For the Sun, the influence of its solar wind extends throughout a bubble-shaped region called the heliosphere.[163]

text: Nuclear fusion reaction pathways

text: A variety of nuclear fusion reactions take place in the cores of stars, that depend upon their mass and composition. When nuclei fuse, the mass of the fused product is less than the mass of the original parts. This lost mass is converted to electromagnetic energy, according to the mass–energy equivalence relationship E = mc2.[1]

text: The hydrogen fusion process is temperature-sensitive, so a moderate increase in the core temperature will result in a significant increase in the fusion rate. As a result, the core temperature of main sequence stars only varies from 4 million kelvin for a small M-class star to 40 million kelvin for a massive O-class star.[136]

text: In the Sun, with a 10-million-kelvin core, hydrogen fuses to form helium in the proton–proton chain reaction:[164]

text: These reactions result in the overall reaction:

text: where e+ is a positron, γ is a gamma ray photon, νe is a neutrino, and H and He are isotopes of hydrogen and helium, respectively. The energy released by this reaction is in millions of electron volts, which is actually only a tiny amount of energy. However enormous numbers of these reactions occur constantly, producing all the energy necessary to sustain the star's radiation output. In comparison, the combustion of two hydrogen gas molecules with one oxygen gas molecule releases only 5.7 eV.

text:
Minimum stellar mass required for fusion

Element

Solarmasses

Hydrogen
0.01

Helium
0.4

Carbon
5[165]

Neon
8

text: In more massive stars, helium is produced in a cycle of reactions catalyzed by carbon called the carbon-nitrogen-oxygen cycle.[164]

text: In evolved stars with cores at 100 million kelvin and masses between 0.5 and 10 M☉, helium can be transformed into carbon in the triple-alpha process that uses the intermediate element beryllium:[164]

text: For an overall reaction of:

text: In massive stars, heavier elements can also be burned in a contracting core through the neon-burning process and oxygen-burning process. The final stage in the stellar nucleosynthesis process is the silicon-burning process that results in the production of the stable isotope iron-56, an endothermic process that consumes energy, and so further energy can only be produced through gravitational collapse.[164]

text: The example below shows the amount of time required for a star of 20 M☉ to consume all of its nuclear fuel. As an O-class main sequence star, it would be 8 times the solar radius and 62,000 times the Sun's luminosity.[166]

text:
Fuelmaterial

Temperature(million kelvins)

Density(kg/cm3)

Burn duration(τ in years)

H

37

0.0045

8.1 million

He

188

0.97

1.2 million

C

870

170

976

Ne

1,570

3,100

0.6

O

1,980

5,550

1.25

S/Si

3,340

33,400

0.0315[167]


document_title: Normal (New Girl)

question_text: what episode of new girl do they play true american

root

text: Normal (New Girl)

text: Plot[edit]

text: Jess (Zooey Deschanel) brings her new boyfriend Russell (Dermot Mulroney) home to the loft to meet her roommates. After some reluctance, the men bond when the group plays True American, an active drinking game. The game ends when Cece (Hannah Simone) retreats to Schmidt's bed, prompting Schmidt (Max Greenfield) to join her. Nick (Jake Johnson) then shares his idea for "real apps," a suite of physical "apps" for smartphones with functionality similar to a Swiss Army knife. He accidentally wounds Russell with the prototype, prompting Russell to leave, to Jess's disappointment.

tag: p

text: Winston (Lamorne Morris) begins a new job in "Normal" as an assistant to sports talk show host Joe Napoli (Phil Hendrie). Winston's initial enthusiasm for the job fades when he realizes Napoli is an abrasive and disrespectful boss. Kareem Abdul-Jabbar has a cameo appearance as a guest on Napoli's show.

text: True American[edit]

text: After "Normal" aired, internet sources began to summarize the rules for True American, which the characters described as a mix of a drinking game and Candy Land where the floor is lava; it also involves shouting the names of American presidents.[1][2] The idea of True American came from a New Girl writer who played a similar game in college. As she could not remember the game's exact rules, the writers focused on making the game as funny on the page as possible, but only established chanting "JFK! FDR!" and walking on chairs. As the cast did not understand the game during shooting, the writers created more rules on the spot, advised the actors to "have fun, dig in, jump in" and play it as if "they'd been playing this thing for years and years and years." The high-energy feel of the game and the amounts of coverage made filming True American more challenging for the actors than normal episodes. Producers Dave Finkel, Brett Baer, and writer Luvh Rakhe, came up with most of the obscure American history facts, but much was cut from the finished episode.[1][3] Fox subsequently released a set of official rules for the game, which can be summarized "There are no real rules".[4] The characters also played True American in "Cooler", the 15th episode of the second season, in "Mars Landing", the 20th episode of the third season and in "Wedding Eve" the 21st episode of the fifth season.

text: Reception[edit]

text: The initial broadcast of "Normal" attracted 5.23 million US viewers.[5] The A.V. Club called the episode "the young series at its best," rating it an A- overall.[6] The staff of The Atlantic included it in their list of the best TV episodes of 2012, comparing the actors' performances to "the best sitcom ensembles" of Seinfeld, Will & Grace, and Friends.[7] Alan Sepinwall said the episode "didn't seem quite as effortlessly hilarious as several recent episodes" but was still enjoyable.[8]


document_title: Brain on Fire

question_text: what did the girl have on brain on fire

question_tokens: what did the girl have on brain on fire

text: Brain on Fire

text: Synopsis[edit]

text: The book narrates Cahalan's issues with anti-NMDA receptor encephalitis and the process by which she was diagnosed with this form of encephalitis. She wakes up in a hospital with no memory of the events of the previous month, during which time she would have violent episodes and delusions. Her eventual diagnosis is made more difficult by various physicians misdiagnosing her with several theories such as "partying too much" and schizoaffective disorder.[2] Eventually several physicians, including Dr. Souhel Najjar, began to suspect that Cahalan was suffering from an autoimmune disease.[2] Najjar diagnosed Cahalan using a test that involved her drawing a clock, a test normally given to people suspected of having dementia or Alzheimer's disease.[3] Rather than drawing the clock face normally, the disease caused Cahalan to draw all of the numbers 1 through 12 on the right face of the clock, because the right side of her brain, which regulates the left side of the body, was inflamed. Najjar used this to help diagnose Cahalan and start her road to recovery.[4]

text: The book also covers Cahalan's life after her recovery, including her reactions to watching videotapes of her psychotic episodes while in the hospital. Cahalan also discusses her symptoms prior to her hospitalization, as she had previously been diagnosed by both a psychiatrist and by herself with bipolar disorder.[2] While researching, she learned that the disease had only been discovered three years before she became ill.[5] Her research indicated that in 2009 most people with the disease were either misdiagnosed or undiagnosed. Cahalan was fortunate to be correctly diagnosed because, according to Najjar's estimates, only 10 percent of people with the disease were properly diagnosed at that time.[6] Since then, a better understanding of the disease and its symptoms has resulted in more frequent diagnosis and treatment.

text: Reception[edit]

text: Critical reception for Brain on Fire has been mostly positive. NPR commented that the author was "a naturally talented prose stylist" and that "she perfectly tempers her brutal honesty with compassion and something like vulnerability."[7] The Washington Post praised Cahalan's researching abilities for the book, as they noted that she had to rely on information from others, including family members and medical documents.[8]

text: Film adaptation[edit]

text: In May 2014, it was announced that the book was being adapted into a film of the same name starring Chloë Grace Moretz[9] and produced by Cahalan and Charlize Theron.[10][11] The film was released on Netflix on June 22, 2018.[12]


document_title: List of National Basketball Association career scoring leaders

question_text: who is the all time nba scoring leader

question_tokens: who is the all time nba scoring leader

text: Scoring leaders[edit]

text: The following is a list of National Basketball Association players by total career regular season points scored.

text:
^

Active NBA player

*

Inducted into the Naismith Memorial Basketball Hall of Fame

†

Not yet eligible for Hall of Fame consideration[2]

tag: table

text:
Rank

Player

Position(s)

Team(s) played for (years)[3]

Total points

Games  played

Points  per gameaverage[4]

Field goalsmade

Three-pointfield goalsmade[5]

Free  throws made

1

Kareem Abdul-Jabbar*[6]

C

Milwaukee Bucks (1969–1975)Los Angeles Lakers (1975–1989)

38,387

1,560

24.6

15,837

1

6,712

2

Karl Malone*

PF

Utah Jazz (1985–2003)Los Angeles Lakers (2003–2004)

36,928

1,476

25.0

13,528

85

9,787

3

Kobe Bryant†

SG

Los Angeles Lakers (1996–2016)

33,643

1,346

25.0

11,719

1,827

8,378

4

Michael Jordan*

SG

Chicago Bulls (1984–1993, 1995–1998)Washington Wizards (2001–2003)

32,292

1,072

30.1

12,192

581

7,327

5

Wilt Chamberlain*

C

Philadelphia/San Francisco Warriors (1959–1965)Philadelphia 76ers (1965–1968)Los Angeles Lakers (1968–1973)

31,419

1,045

30.1

12,681

0

6,057

6

Dirk Nowitzki^

PF/C

Dallas Mavericks (1999–present)

31,187

1,471

21.2

11,034

1,918

7,201

7

LeBron James^

SF/PF

Cleveland Cavaliers (2003–2010, 2014–2018)Miami Heat (2010–2014)Los Angeles Lakers (2018–present)

31,038

1,143

27.2

11,280

1,616

6,862

8

Shaquille O'Neal*

C

Orlando Magic (1992–1996)Los Angeles Lakers (1996–2004)Miami Heat (2004–2008)Phoenix Suns (2008–2009)Cleveland Cavaliers (2009–2010)Boston Celtics (2010–2011)

28,596

1,207

23.7

11,330

1

5,935

9

Moses Malone*

C

Buffalo Braves (1976)Houston Rockets (1976–1982)Philadelphia 76ers (1982–1986, 1993–1994)Washington Bullets (1986–1988)Atlanta Hawks (1988–1991)Milwaukee Bucks (1991–1993)San Antonio Spurs (1994–1995)

27,409

1,329

20.6

9,435

8

8,531

10

Elvin Hayes*

PF/C

San Diego/Houston Rockets (1968–1972, 1981–1984)Baltimore/Capital/Washington Bullets (1972–1981)

27,313

1,303

21.0

10,976

5

5,356

11

Hakeem Olajuwon*[7]

C

Houston Rockets (1984–2001)Toronto Raptors (2001–2002)

26,946

1,238

21.8

10,749

25

5,423

12

Oscar Robertson*

PG

Cincinnati Royals (1960–1970)Milwaukee Bucks (1970–1974)

26,710

1,040

25.7

9,508

0

7,694

13

Dominique Wilkins*

SF

Atlanta Hawks (1982–1994)Los Angeles Clippers (1994)Boston Celtics (1994–1995)San Antonio Spurs (1996–1997)Orlando Magic (1999)

26,668

1,074

24.8

9,963

711

6,031

14

Tim Duncan†

PF/C

San Antonio Spurs (1997–2016)

26,496

1,392

19.0

10,285

30

5,896

15

Paul Pierce†

SF/SG

Boston Celtics (1999–2013)Brooklyn Nets (2013–2014)Washington Wizards (2014–2015)Los Angeles Clippers (2015–2017)

26,397

1,343

19.7

8,668

2,143

6,918

16

John Havlicek*

SF/SG

Boston Celtics (1962–1978)

26,395

1,270

20.8

10,513

0

5,369

17

Kevin Garnett†

PF/C

Minnesota Timberwolves (1995–2007, 2015–2016)Boston Celtics (2007–2013)Brooklyn Nets (2013–2015)

26,071

1,462

17.8

10,505

174

4,887

18

Alex English*

SF

Milwaukee Bucks (1976–1978)Indiana Pacers (1978–1980)Denver Nuggets (1980–1990)Dallas Mavericks (1990–1991)

25,613

1,193

21.5

10,659

18

4,277

19

Carmelo Anthony^

SF

Denver Nuggets (2003–2011)New York Knicks (2011–2017)Oklahoma City Thunder (2017–2018)Houston Rockets (2018–present)

25,417

1,054

24.1

9,088

1,341

5,900

20

Reggie Miller*

SG

Indiana Pacers (1987–2005)

25,279

1,389

18.2

8,241

2,560

6,237

21

Jerry West*

PG/SG

Los Angeles Lakers (1960–1974)

25,192

932

27.0

9,016

0

7,160

22

Vince Carter^

SG/SF

Toronto Raptors (1999–2004)New Jersey Nets (2004–2009)Orlando Magic (2009–2010)Phoenix Suns (2010–2011)Dallas Mavericks (2011–2014)Memphis Grizzlies (2014–2017)Sacramento Kings (2017–2018)Atlanta Hawks (2018–present)

24,868

1,405

17.7

8,990

2,106

4,782

23

Patrick Ewing*

C

New York Knicks (1985–2000)Seattle SuperSonics (2000–2001)Orlando Magic (2001–2002)

24,815

1,183

21.0

9,702

19

5,392

24

Ray Allen*

SG

Milwaukee Bucks (1996–2003)Seattle SuperSonics (2003–2007)Boston Celtics (2007–2012)Miami Heat (2012–2014)

24,505

1,300

18.9

8,567

2,973

4,398

25

Allen Iverson*

SG/PG

Philadelphia 76ers (1996–2006, 2009–2010)Denver Nuggets (2006–2008)Detroit Pistons (2008–2009)Memphis Grizzlies (2009)

24,368

914

26.7

8,467

1,059

6,375

26

Charles Barkley*

PF

Philadelphia 76ers (1984–1992)Phoenix Suns (1992–1996)Houston Rockets (1996–2000)

23,757

1,073

22.1

8,435

538

6,349

27

Robert Parish*

C

Golden State Warriors (1976–1980)Boston Celtics (1980–1994)Charlotte Hornets (1994–1996)Chicago Bulls (1996–1997)

23,334

1,611

14.5

9,614

0

4,106

28

Adrian Dantley*

SF

Buffalo Braves (1976–1977)Indiana Pacers (1977)Los Angeles Lakers (1977–1979)Utah Jazz (1979–1986)Detroit Pistons (1986–1989)Dallas Mavericks (1989–1990)Milwaukee Bucks (1991)

23,177

955

24.3

8,169

7

6,832

29

Elgin Baylor*

SF

Minneapolis/Los Angeles Lakers (1958–1971)

23,149

846

27.4

8,693

0

5,763

30

Clyde Drexler*

SG

Portland Trail Blazers (1983–1995)Houston Rockets (1995–1998)

22,195

1,086

20.4

8,335

827

4,698

31

Dwyane Wade^

SG

Miami Heat (2003–2016, 2018–present)Chicago Bulls (2016–2017) Cleveland Cavaliers (2017–2018)

22,082

982

22.5

8,038

463

5,543

32

Gary Payton*

PG

Seattle SuperSonics (1990–2003)Milwaukee Bucks (2003)Los Angeles Lakers (2003–2004)Boston Celtics (2004–2005)Miami Heat (2005–2007)

21,813

1,335

16.3

8,708

1,132

3,265

33

Larry Bird*

SF/PF

Boston Celtics (1979–1992)

21,791

897

24.3

8,591

649

3,960

34

Hal Greer*

SG/PG

Syracuse Nationals/Philadelphia 76ers (1958–1973)

21,586

1,122

19.2

8,504

0

4,578

35

Walt Bellamy*

C

Chicago Packers/Zephyrs/Baltimore Bullets (1961–1965)New York Knicks (1965–1968)Detroit Pistons (1968–1970)Atlanta Hawks (1970–1974)New Orleans Jazz (1974)

20,941

1,043

20.1

7,914

0

5,113

36

Kevin Durant^

SF

Seattle SuperSonics/Oklahoma City Thunder (2007–2016)Golden State Warriors (2016–present)

20,913

771

27.1

7,093

1,433

5,294

37

Bob Pettit*

PF/C

Milwaukee/St. Louis Hawks (1954–1965)

20,880

792

26.4

7,349

0

6,182

38

David Robinson*

C

San Antonio Spurs (1989–2003)

20,790

987

21.1

7,365

25

6,035

39

Pau Gasol^

C/PF

Memphis Grizzlies (2001–2008)Los Angeles Lakers (2008–2014)Chicago Bulls (2014–2016)San Antonio Spurs (2016–present)

20,776

1,196

17.4

7,938

173

4,727

40

George Gervin*

SG/SF

San Antonio Spurs (1976–1985)Chicago Bulls (1985–1986)

20,708

791

26.2

8,045

77

4,541

41

Mitch Richmond*

SG

Golden State Warriors (1988–1991)Sacramento Kings (1991–1998)Washington Wizards (1999–2001)Los Angeles Lakers (2001–2002)

20,497

976

21.0

7,305

1,326

4,561

42

Joe Johnson^

SG/SF

Boston Celtics (2001–2002)Phoenix Suns (2002–2005)Atlanta Hawks (2005–2012)Brooklyn Nets (2012–2016)Miami Heat (2016)Utah Jazz (2016–2018)Houston Rockets (2018–present)

20,405

1,276

16.0

7,822

1,978

2,783

43

Tom Chambers

PF

San Diego Clippers (1981–1983)Seattle SuperSonics (1983–1988)Phoenix Suns (1988–1993)Utah Jazz (1993–1995)Charlotte Hornets (1997)Philadelphia 76ers (1997)

20,049

1,107

18.1

7,378

227

5,066

44

Antawn Jamison

PF/SF

Golden State Warriors (1999–2003)Dallas Mavericks (2003–2004)Washington Wizards (2004–2010)Cleveland Cavaliers (2010–2012)Los Angeles Lakers (2012–2013)Los Angeles Clippers (2013–2014)

20,042

1,083

18.5

7,679

1,163

3,521

45

John Stockton*

PG

Utah Jazz (1984–2003)

19,711

1,504

13.1

7,039

845

4,788

46

Bernard King*

SF

New Jersey Nets (1977–1979, 1993)Utah Jazz (1979)Golden State Warriors (1980–1982)New York Knicks (1982–1985, 1987)Washington Bullets (1987–1991)

19,655

874

22.5

7,830

23

3,972

47

Clifford Robinson

PF/SF

Portland Trail Blazers (1989–1997)Phoenix Suns (1997–2001)Detroit Pistons (2001–2003)Golden State Warriors (2003–2005)New Jersey Nets (2005–2007)

19,591

1,380

14.2

7,389

1,253

3,560

48

Walter Davis

SG/SF

Phoenix Suns (1977–1988)Denver Nuggets (1988–1991, 1991–1992)Portland Trail Blazers (1991)

19,521

1,033

18.9

8,118

157

3,128

49

Terry Cummings

PF

San Diego Clippers (1982–1984)Milwaukee Bucks (1984–1989, 1995–1996)San Antonio Spurs (1989–1995)Seattle SuperSonics (1996–1997)Philadelphia 76ers (1997–1998)New York Knicks (1998)Golden State Warriors (1999–2000)

19,460

1,183

16.4

8,045

44

3,326

50

Bob Lanier*

C

Detroit Pistons (1970–1980)Milwaukee Bucks (1980–1984)

19,248

959

20.1

7,761

2

3,724

text: Progressive list of scoring leaders[edit]

text: This is a progressive list of scoring leaders showing how the record increased through the years.[1]

text:
Team abbreviations

Team(s) listed is the one player was on when he established the record.

ATL
Atlanta Hawks
DET
Detroit Pistons
MIL
Milwaukee Bucks
PHX
Phoenix Suns

BOS
Boston Celtics
FTW
Fort Wayne Pistons
MIN
Minnesota Timberwolves
PHW
Philadelphia Warriors

BUF
Buffalo Braves
GSW
Golden State Warriors
MNL
Minneapolis Lakers
SAS
San Antonio Spurs

CHI
Chicago Bulls
HOU
Houston Rockets
NOJ
New Orleans Jazz
SDR
San Diego Rockets

CHS
Chicago Stags
IND
Indiana Pacers
NOP
New Orleans Pelicans
SFW
San Francisco Warriors

CLE
Cleveland Cavaliers
KCO
Kansas City-Omaha Kings
OKC
Oklahoma City Thunder
STL
St. Louis Hawks

DAL
Dallas Mavericks
LAL
Los Angeles Lakers
ORL
Orlando Magic
SYR
Syracuse Nationals

DEN
Denver Nuggets
MIA
Miami Heat
PHI
Philadelphia 76ers
UTA
Utah Jazz

text:
Scoring leader at the end of every season

Season
Year-by-year leader
Points
Active player leader
Total points
Career record
Total points
Single-season record
Points
Season

1946–47
Joe Fulks*000PHW
1,389
Joe Fulks*000PHW
1,389
Joe Fulks*000PHW
1,389
Joe Fulks*000PHW
1,389
1946–47

1947–48
Max Zaslofsky000CHS
1,007
2,338
2,338
1947–48

1948–49
George Mikan*000MNL
1,698
3,898
3,898
George Mikan*000MNL
1,698
1948–49

1949–50
1,865
4,863
4,863
1,865
1949–50

1950–51
1,932
6,099
6,099
1,932
1950–51

1951–52
Paul Arizin*000PHW
1,674
7,021
7,021
1951–52

1952–53
Neil Johnston*000PHW
1,564
George Mikan*000MNL
8,460
George Mikan*000MNL
8,460
1952–53

1953–54
1,759
9,766
9,766
1953–54

1954–55
1,631
Max Zaslofsky000FTW
7,902
1954–55

1955–56
Bob Pettit*000STL
1,849
George Mikan*000MNL
10,156
10,156
1955–56

1956–57
Paul Arizin*000PHW
1,817
Ed Macauley*000STL
10,150
1956–57

1957–58
George Yardley*000DET
2,001
Dolph Schayes*000SYR
11,764
Dolph Schayes*000SYR
11,764
George Yardley*000DET
2,001
1957–58

1958–59
Bob Pettit*000STL
2,105
13,298
13,298
Bob Pettit*000STL
2,105
1958–59

1959–60
Wilt Chamberlain*000PHW 1959–62000SFW 1962–65000PHI 1965–66
2,707
14,987
14,987
Wilt Chamberlain*000PHW
2,707
1959–60

1960–61
3,033
16,855
16,855
3,033
1960–61

1961–62
4,029
17,677
17,677
4,029
1961–62

1962–63
3,586
18,304
18,304
1962–63

1963–64
2,948
Bob Pettit*000STL
19,756
Bob Pettit*000STL
19,756
1963–64

1964–65
2,534
20,880
20,880
1964–65

1965–66
2,649
Wilt Chamberlain*000PHI 1965–68000LAL 1968–73
21,486
Wilt Chamberlain*000PHI 1965–68000LAL 1968–73
21,486
1965–66

1966–67
Rick Barry*000SFW
2,775
23,442
23,442
1966–67

1967–68
Dave Bing*000DET
2,142
25,434
25,434
1967–68

1968–69
Elvin Hayes*000SDR
2,327
27,098
27,098
1968–69

1969–70
Kareem Abdul-Jabbar*000MIL
2,361
27,426
27,426
1969–70

1970–71
2,596
29,122
29,122
1970–71

1971–72
2,822
30,335
30,335
1971–72

1972–73
Tiny Archibald*000KCO
2,719
31,419
31,419
1972–73

1973–74
Bob McAdoo*000BUF
2,261
Oscar Robertson*000MIL
26,710
1973–74

1974–75
2,831
John Havlicek*000BOS
22,389
1974–75

1975–76
2,427
23,678
1975–76

1976–77
Pete Maravich*000NOJ
2,273
25,073
1976–77

1977–78
George Gervin*000SAS
2,232
26,395
1977–78

1978–79
2,365
Kareem Abdul-Jabbar*000LAL
22,141
1978–79

1979–80
2,585
24,175
1979–80

1980–81
Adrian Dantley*000UTA
2,452
26,270
1980–81

1981–82
George Gervin*000SAS
2,551
28,088
1981–82

1982–83
Alex English*000DEN
2,326
29,810
1982–83

1983–84
Adrian Dantley*000UTA
2,418
31,527
Kareem Abdul-Jabbar*000LAL
31,527
1983–84

1984–85
Michael Jordan*000CHI
2,313
33,262
33,262
1984–85

1985–86
Alex English*000DEN
2,414
35,108
35,108
1985–86

1986–87
Michael Jordan*000CHI
3,041
36,474
36,474
1986–87

1987–88
2,868
37,639
37,639
1987–88

1988–89
2,633
38,387
38,387
1988–89

1989–90
2,753
Moses Malone*000ATL 1989–91000MIL 1991–93000PHI 1993–94000SAS 1994–95
24,868
1989–90

1990–91
2,580
25,737
1990–91

1991–92
2,404
27,016
1991–92

1992–93
2,541
27,066
1992–93

1993–94
David Robinson*000SAS
2,383
27,360
1993–94

1994–95
Shaquille O'Neal*000ORL
2,315
27,409
1994–95

1995–96
Michael Jordan*000CHI
2,491
Michael Jordan*000CHI
24,489
1995–96

1996–97
2,431
26,920
1996–97

1997–98
2,357
29,277
1997–98

1998–99
Shaquille O'Neal*000LAL
1,289
Karl Malone*000UTA 1998–2003000LAL 2003–04
28,946
1998–99

1999–00
2,344
31,041
1999–00

2000–01
Jerry Stackhouse00DET
2,380
32,919
2000–01

2001–02
Paul Pierce†000BOS
2,144
34,707
2001–02

2002–03
Kobe Bryant†000LAL
2,461
36,374
2002–03

2003–04
Kevin Garnett†000MIN
1,987
36,928
2003–04

2004–05
Allen Iverson*000PHI
2,302
Reggie Miller*000IND
25,279
2004–05

2005–06
Kobe Bryant†000LAL
2,832
Shaquille O'Neal*000MIA 2005–08000PHO 2008–09000CLE 2009–10000BOS 2010–11
24,764
2005–06

2006–07
2,430
25,454
2006–07

2007–08
2,323
26,286
2007–08

2008–09
Dwyane Wade^000MIA
2,386
27,619
2008–09

2009–10
Kevin Durant^000OKC
2,472
28,255
2009–10

2010–11
2,161
28,596
2010–11

2011–12
1,850
Kobe Bryant†000LAL
29,484
2011–12

2012–13
2,280
31,617
2012–13

2013–14
2,593
31,700
2013–14

2014–15
James Harden^000HOU
2,217
32,482
2014–15

2015–16
2,376
33,643
2015–16

2016–17
Russell Westbrook^000OKC
2,558
Dirk Nowitzki^000DAL
30,260
2016–17

2017–18
LeBron James^000CLE
2,251
31,187
Abdul-Jabbar*0 35 yrs
38,387
Chamberlain*059 yrs
4,029
2017–18

Season
Year-by-year leader
Points
Active player leader
Total points
Career record
Total points
Single-season record
Points
Season


document_title: Coraline

question_text: where does the other mother keep coraline’s parents

question_tokens: where does the other mother keep coraline 's parents

text: Coraline

text: Plot

text: Coraline Jones and her parents move into an old house that has been divided into flats. The other tenants include Miss Spink and Miss Forcible, two elderly women retired from the stage, and Mr. Bobo, initially referred to as "the crazy old man upstairs", who claims to be training a mouse circus. The flat beside Coraline's is unoccupied, and a small door that links them is revealed to be bricked up when opened.

text: Coraline goes to visit her new neighbours. Mr. Bobo relays to her a message from his mice: "Don't go through the door." Coraline also has tea with Miss Spink and Miss Forcible, and Miss Spink spies danger in Coraline’s future after reading her tea leaves. She then gives her a lucky stone with a hole in the middle, which is supposed to be "good for bad things."

text: Despite these warnings, Coraline decides to unlock the door when she is home by herself. This time, she finds the brick wall behind the door is gone. In its place is a long hallway that leads to a flat identical to her own, except inhabited by the "Other Mother" and "Other Father," who have black buttons for eyes. The Other Mother is notably taller and thinner than her real mother. Her black hair seems to move by itself, her skin is paper-white, and her nails are long and red. Coraline finds the "Other World" more interesting than her own; the Other Mother cooks food that she actually enjoys, both of her Other Parents pay more attention to her, her toy box is filled with animate toys that can move and fly, the Other Miss Spink and Miss Forcible perform a never-ending act in their flat, and the Other Mr. Bobo performs a mice circus. She even finds that the feral black cat that wanders around the house in the real world can talk. The cat identifies itself as the same cat that lives in the real world, and possesses the ability to travel through the gaps between the two worlds. Although intentionally rude and unhelpful for the greater part of the conversation, it briefly praises her for bringing "protection", then vanishes.

text: After Coraline returns to the copy of her flat, the Other Mother offers Coraline the opportunity to stay in the Other World forever, but in order to do so, Coraline must allow buttons to be sewn into her eyes. Coraline is horrified and returns through the door to her home. Upon return to her apartment, Coraline finds that her real parents are missing. They do not return the next day, and the black cat wakes her and takes her to a mirror in her hallway, through which she can see her trapped parents. They signal to her by writing "Help Us" on the glass, from which Coraline deduces the Other Mother has kidnapped them. Though frightened of returning, Coraline goes back to the Other World to confront the Other Mother and rescue her parents. In the garden, Coraline is prompted by the cat to challenge the Other Mother, as "her kind of thing loves games and challenges." The Other Mother tries to convince Coraline to stay, but Coraline refuses, and is locked within a small space behind a mirror as punishment.

text: In the small dark closet space, she meets three ghost children. Each had in the past let the Other Mother, who they archaically refer to as the "beldam," sew buttons over their eyes. They tell Coraline how the Other Mother eventually grew bored with them, leaving them to die and cast them aside, but they are trapped there because she has kept their souls. If their souls can be rescued from the Other Mother, then the ghosts can pass on. The ghost children implore Coraline to escape and avoid their fate.

text: After the Other Mother releases Coraline from the mirror, Coraline proposes a game: if she can find the ghost children's souls and her parents, then she, her parents, and the ghost children may go free. If she loses, then Coraline will let the Other Mother sew the buttons into her eyes and become a loving daughter to her. The Other Mother agrees and they both swear on their right hands.

text: Coraline searches through the Other World and overcomes the Other Mother's obstacles by using her wits and Miss Spink's lucky stone to find the marble-like souls of the ghost children. She also deduces that her parents are imprisoned in a snow globe on the mantelpiece. The ghost children warn her that even if Coraline wins, the Other Mother will not let them go, so Coraline tricks the Other Mother by announcing that she knows where her parents are hidden: in the passageway between the worlds. The Other Mother cannot resist gloating by opening the door to show Coraline that her parents are not there. When the Other Mother opens the door Coraline throws the cat at the Other Mother, grabs the snow globe, and escapes to the real world with the key, and the Cat quickly follows. While escaping, Coraline forces the door shut on the Other Mother's hand. Back in her home, Coraline falls asleep on a chair. She is awoken by her parents who have no memory of the events.

text: That night, Coraline has a dream in which she meets the three children at a picnic. The children are dressed in clothes from different periods and one seems to have wings. They warn her that her task is still not done: the Other Mother will attempt to get her back and will try to get the key to open the door between the worlds. Coraline goes to the old well in the woods to dispose of the key. She pretends to have a picnic, with the picnic blanket laid over the entrance to the well. The Other Mother's severed hand attempts to seize the key, but steps on the blanket and falls into the well. Coraline returns to the house, greeting her neighbours (who finally get her name right), and getting ready for school tomorrow.

text: Characters

text:
Coraline Jones – The young explorer. She is curious, intelligent, resourceful, and courageous. Coraline is often irritated by rain, crazy grown-ups (as they all seem to be), and not being taken seriously because of her young age. She's described as being "small for her age", but Coraline is not afraid to face anyone; she is the most adventurous person in the book.
Mrs. Jones – Coraline's mother. She is very busy most of the time, and sometimes a little inattentive, but she loves and cares about Coraline. She is nice, and helpful, though Coraline considers her to be rather boring. Coraline also gets annoyed with her real mother because she doesn't seem to want to let Coraline "fit in". In the film, her first name is Mel.
Mr. Jones – Coraline's father. He works at his house on the computer. He cares about Coraline very much and is kind, brave, and helpful. He makes interesting food creations that Coraline strongly dislikes. He, too, is usually too busy to spend time with Coraline. In the film, his first name is Charlie.
The Cat – A black cat from Coraline's world. The cat acts as a mentor to Coraline and guides her through her journey. It claims to have no name, explaining that cats do not need names to tell each other apart. Unlike many of the characters in the novel, it does not have an "Other World" counterpart, saying that unlike other creatures in the world, cats can "keep themselves together". It moves freely from one world to the other, although it seems to be only able to talk in the Other World. It is very sarcastic, though helpful to Coraline. It's defiant of the Other Mother, but seems to tremble at the thought of being stuck in the Other Mother's world. It befriends Coraline and helps her escape from the Other Mother, though Coraline also uses it as a weapon without its permission.
The Other Mother – The creature that created much of the Other World and the main villain of the novel. She looks similar to Coraline's real mother but taller and thinner, with long black hair that seems to move by itself, black button eyes, paper-white skin, and extremely long, twitchy fingers with long dark red nails. During the course of the novel, she grows taller, thinner, and paler, looking less and less like Coraline's mother. She cannot create, but only copy, twist and change things from the real world when constructing her version of it. She collects children, whom she loves possessively to the point of eventual destruction. She mainly wants someone to mother. It's implied that she killed her own mother because when Coraline asked her if she had a grave she replied "Oh yes, I put her there myself." In the film her true form is a spidery, skeletal creature. She is referred to several times as "the beldam", a Middle English word meaning "grandmother", "ugly old woman", "hag", or "witch", and also used to refer to creatures of fairy.
The Other Father – A creation of the Other Mother, the Other Father is used to help trick Coraline into staying in the Other Mother's world. Like her real father, he has a study and sits there during the day and will not talk to Coraline for long. He does not work, however; he merely occupies the study, as he is not permitted to talk to Coraline by himself. He is much more fun than Coraline's real father and always tries to be cheerful and fun in front of Coraline. In reality, the Other Father is sad and nervous. The Other Mother ends up punishing him for revealing too much to Coraline—she transforms him into a grub-like creature, and orders the Other Father to trap Coraline so she cannot win her challenge, but Coraline escapes.
Miss Spink and Miss Forcible – A pair of retired actresses who live in the flat under Coraline's. They own many ageing Scotties, such as Hamish, Angus, and Jock, and talk in theater jargon, often referencing their time as actresses. They recognize the danger Coraline is in after reading her fortune through tea leaves and give her a stone with a hole in it to help protect her. In the Other World they are young, pretty, and perform continuously in front of many different dogs, who, in the Other World, are anthropomorphic.
Mr. Bobo – A retired circus performer living in the flat above Coraline's; he is commonly referred to as the Crazy Old Man Upstairs. Over the course of the book he claims to be training mice to perform in a mouse circus, and often brings Coraline messages from them, though at first Coraline doubts he even has mice to train, and doesn't listen to what he says to be messages from the mice. His counterpart in the Other World trains rats, and is in fact made of rats. (In the film adaptation, this character is named Mr. Bobinsky.)
The three ghost children – A trio of children who were previous victims of the Other Mother: two girls and one boy. The boy is described as having a dirty face and red trousers. One of the girls has brown hair, a pink blouse and a pink skirt. The other has a brown bonnet and brown dress. They were trapped by the other mother at different times before Coraline, and reside in the dark space behind the mirror. After having their souls restored, they go to the afterlife, but not before meeting Coraline for a last time, in a dream where she picnics with them. Here, she sees their true appearances and they thank her for freeing them from the Other Mother.

tag: ul

text: In other media

text: Television

text: Coraline inspired the "Coralisa" segment of The Simpsons episode "Treehouse of Horror XXVIII", which aired on 22 October 2017 . Neil Gaiman provided the voice to the Simpsons' cat, Snowball V.[5]

text: Film

text: With the help of the animation studio Laika, director Henry Selick released a stop motion film adaptation in 2009 that received critical acclaim. At the 82nd Academy Awards, the film was nominated for Best Animated Feature but lost to Pixar's Up. In the film, Coraline is depicted as having short blue hair and freckles. Henry Selick added a new character, Wyborn "Wybie" Lovat, who is an annoyance at first to Coraline in the real world but she grows to like him. In the Other world he cannot speak, but is an ally to Coraline. At the end of the film, Coraline reaches out to help Wybie tell his grandmother what is behind the little door.

text: Comic books

text: A comic book adaptation, published in 2008, was illustrated by P. Craig Russell and lettered by Todd Klein.[6]

text: Musical

text: A theatrical adaptation, with music and lyrics by Stephin Merritt and book by David Greenspan, premiered on 6 May 2009, produced by MCC Theater and True Love Productions Off-Broadway at The Lucille Lortel Theatre.[7] Nine-year-old Coraline was played by an adult, Jayne Houdyshell, and the Other Mother was played by David Greenspan.[7]

text: Video games

text: A video game adaptation, based on the film, was published and developed by D3 Publisher of America. The game was released on 27 January 2009 for the PlayStation 2, Nintendo DS and Wii platforms and contains features such as playing as Coraline, interacting with other characters, and playing minigames. The game received mostly negative reviews.[8][9]

text: Opera

text: An opera by Mark-Anthony Turnage, based on the novella, made its world premiere at the Barbican Centre in London on 27 March 2018.