Sun From Wikipedia, the free encyclopedia This article is about the star. For other uses, see Sun (disambiguation). The Sun Observation data Mean distance from Earth 1.496×108 km 8 min 19 s at light speed Visual brightness (V) −26.74[1] Absolute magnitude 4.83[1] Spectral classification G2V Metallicity Z = 0.0122[2] Angular size 31.6′ – 32.7′[3] Adjectives Solar Orbital characteristics Mean distance from Milky Waycore ~2.7×1017 km 27,200 light-years Galactic period (2.25–2.50)×108 a Velocity ~220 km/s (orbit around the center of the Galaxy) ~20 km/s (relative to average velocity of other stars in stellar neighborhood) ~370 km/s[4] (relative to the cosmic microwave background) Physical characteristics Mean diameter 1.392684×106 km[5] Equatorialradius 6.96342×105 km[5] 109 × Earth[6] Equatorialcircumference 4.379×106 km[6] 109 × Earth[6] Flattening 9×10−6 Surface area 6.0877×1012 km2[6] 11,990 × Earth[6] Volume 1.412×1018 km3[6] 1,300,000 × Earth Mass 1.9891×1030 kg[1] 333,000 × Earth[1] Average density 1.408×103 kg/m3[1][6][7] Density Center (model): 1.622×105 kg/m3[1] Lower photosphere: 2×10−4 kg/m3 Lower chromosphere: 5×10−6 kg/m3 Corona (avg): 1×10−12 kg/m3[8] Equatorialsurface gravity 274.0 m/s2[1] 27.94 g 27,542.29 cgs 28 × Earth[6] Escape velocity (from the surface) 617.7 km/s[6] 55 × Earth[6] Temperature Center (modeled): ~1.57×107 K[1] Photosphere (effective): 5,778 K[1] Corona: ~5×106 K Luminosity(Lsol) 3.846×1026 W[1] ~3.75×1028 lm ~98 lm/W efficacy Meanintensity (Isol) 2.009×107 W•m−2•sr−1 Age 4.57 billion years[9] Rotation characteristics Obliquity 7.25°[1] (to the ecliptic) 67.23° (to the galactic plane) Right ascension of North pole[10] 286.13° 19 h 4 min 30 s Declination of North pole +63.87° 63° 52 North Sidereal rotation period (at equator) 25.05 days[1] (at 16° latitude) 25.38 days[1] 25 d 9 h 7 min 12 s[10] (at poles) 34.4 days[1] Rotation velocity (at equator) 7.189×103 km/h[6] Photospheric composition (by mass) Hydrogen 73.46%[11] Helium 24.85% Oxygen 0.77% Carbon 0.29% Iron 0.16% Neon 0.12% Nitrogen 0.09% Silicon 0.07% Magnesium 0.05% Sulfur 0.04% This box: • view • talk • edit The Sun is the star at the center of the Solar System.[a] It is almost perfectly spherical and consists of hot plasma interwoven with magnetic fields.[12][13] It has a diameter of about 1,392,684 km (865,374 mi),[5] around 109 times that of Earth, and its mass (1.989×1030 kilograms, approximately 330,000 times the mass of Earth) accounts for about 99.86% of the total mass of the Solar System.[14] Chemically, about three quarters of the Suns mass consists of hydrogen, while the rest is mostly helium. The remainder (1.69%, which nonetheless equals 5,600 times the mass of Earth) consists of heavier elements, including oxygen, carbon, neon and iron, among others.[15] The Sun formed about 4.6 billion[b] years ago from the gravitational collapse of a region within a large molecular cloud. Most of the matter gathered in the center, while the rest flattened into an orbiting disk that would become the Solar System. The central mass became increasingly hot and dense, eventually initiating thermonuclear fusion in its core. It is thought that almost all stars form by this process. The Sun is classified as a G-type main-sequence star (G2V) based on spectral class and it is informally designated as a yellow dwarf because its visible radiation is most intense in the yellow-green portion of the spectrum, and although it is actually white in color, from the surface of the Earth it may appear yellow because of atmospheric scattering of blue light.[16] In the spectral class label, G2 indicates its surface temperature, of approximately 5778 K (5505 °C), and V indicates that the Sun, like most stars, is a main-sequence star, and thus generates its energy by nuclear fusion of hydrogen nuclei into helium. In its core, the Sun fuses 620 million metric tons of hydrogen each second. Once regarded by astronomers as a small and relatively insignificant star, the Sun is now thought to be brighter than about 85% of the stars in the Milky Way galaxy, most of which are red dwarfs.[17][18] The absolute magnitude of the Sun is +4.83; however, as the star closest to Earth, the Sun is the brightest object in the sky with an apparent magnitude of −26.74.[19][20] The Suns hot corona continuously expands in space creating the solar wind, a stream of charged particles that extends to the heliopause at roughly 100 astronomical units. The bubble in the interstellar medium formed by the solar wind, the heliosphere, is the largest continuous structure in the Solar System.[21][22] The Sun is currently traveling through the Local Interstellar Cloud (near to the G-cloud) in the Local Bubble zone, within the inner rim of theOrion Arm of the Milky Way galaxy.[23][24] Of the 50 nearest stellar systems within 17 light-years from Earth (the closest being a red dwarf named Proxima Centauri at approximately 4.2 light-years away), the Sun ranks fourth in mass.[25] The Sun orbits the center of the Milky Way at a distance of approximately 24,000–26,000 light-years from the galactic center, completing one clockwise orbit, as viewed from thegalactic north pole, in about 225–250 million years. Since the Milky Way is moving with respect to the cosmic microwave background radiation (CMB) in the direction of the constellation Hydra with a speed of 550 km/s, the Suns resultant velocity with respect to the CMB is about 370 km/s in the direction of Crater or Leo.[26] The mean distance of the Sun from the Earth is approximately 1 astronomical unit (150,000,000 km; 93,000,000 mi), though the distance varies as the Earth moves from perihelion in January to aphelion in July.[27] At this average distance, light travels from the Sun to Earth in about 8 minutes and 19 seconds. The energy of this sunlight supports almost all life[c] on Earth by photosynthesis,[28] and drives Earths climate and weather. The enormous effect of the Sun on the Earth has been recognized since prehistoric times, and the Sun has beenregarded by some cultures as a deity. An accurate scientific understanding of the Sun developed slowly, and as recently as the 19th century prominent scientists had little knowledge of the Suns physical composition and source of energy. This understanding is still developing; there are a number of present day anomalies in the Suns behavior that remain unexplained. Contents [show] Name and etymology The English proper noun Sun developed from Old English sunne (in around 725, attested in Beowulf), and may be related to south. Cognates to English sun appear in other Germanic languages, including Old Frisian sunne, sonne, Old Saxon sunna, Middle Dutch sonne, modernDutch zon, Old High German sunna, modern German Sonne, Old Norse sunna, and Gothic sunnō. All Germanic terms for the Sun stem from Proto-Germanic *sunnōn.[29][30] In relation, the Sun is personified as a goddess in Germanic paganism; Sól/Sunna.[30] Scholars theorize that the Sun, as a Germanic goddess, may represent an extension of an earlier Proto-Indo-European sun deity due to Indo-European linguistic connections between Old Norse Sól, Sanskrit Surya, Gaulish Sulis, Lithuanian Saulė, and Slavic Solntse.[30] The English weekday name Sunday is attested in Old English (Sunnandæg; Suns day, from before 700) and is ultimately a result of aGermanic interpretation of Latin dies solis, itself a translation of the Greek ἡμέρα ἡλίου (hēméra hēlíou).[31] The Latin name for the star, Sol, is widely known but is not common in general English language use; the adjectival form is the related word solar.[32][33] The term sol is also used by planetary astronomers to refer to the duration of a solar day on another planet, such as Mars.[34] A mean Earth solar day is approximately 24 hours, while a mean Martian sol is 24 hours, 39 minutes, and 35.244 seconds.[35] Characteristics This video takes Solar Dynamics Observatory images and applies additional processing to enhance the structures visible. The events in this video represent 24 hours of activity on September 25, 2011. The Sun is a G-type main-sequence star comprising about 99.86% of the total mass of the Solar System. It is a near-perfect sphere, with an oblatenessestimated at about 9 millionths,[36] which means that its polar diameter differs from its equatorial diameter by only 10 kilometres (6.2 mi).[37] Since the Sun consists of a plasma and is not solid, it rotates faster at its equator than at its poles. This behavior is known as differential rotation and is caused by convection in the Sun and the movement of mass, due to steep temperature gradients from the core outwards. This mass carries a portion of the Sun’s counter-clockwise angular momentum (as viewed from the ecliptic north pole), thus redistributing the angular velocity. The period of this actual rotation is approximately 25.6 days at the equator and 33.5 days at the poles. However, due to our constantly changing vantage point from the Earth as it orbits the Sun, the apparent rotation of the star at its equator is about 28 days.[38] The centrifugal effect of this slow rotation is 18 million times weaker than the surface gravity at the Suns equator. The tidal effect of the planets is even weaker and does not significantly affect the shape of the Sun.[39] The Sun is a Population I, or heavy-element-rich,[d] star.[40] The formation of the Sun may have been triggered by shockwaves from one or more nearby supernovae.[41] This is suggested by a high abundance of heavy elements in the Solar System, such as gold and uranium, relative to the abundances of these elements in so-called Population II (heavy-element-poor) stars. These elements could most plausibly have been produced by endothermic nuclear reactions during a supernova, or by transmutation through neutron absorption within a massive second-generation star.[40] The Sun does not have a definite boundary as rocky planets do, and in its outer parts the density of its gases drops exponentially with increasing distance from its center.[42] Nevertheless, it has a well-defined interior structure, described below. The Suns radius is measured from its center to the edge of the photosphere. The photosphere is the last visible layer as those above it are too cool or too thin to radiate sufficient light to be visible to the naked eye[43] in the presence of the brilliant light from the photosphere. During a total solar eclipse, however, when the photosphere is obscured by the Moon, the Suns corona can be easily seen surrounding it. The solar interior is not directly observable, and the Sun itself is opaque to electromagnetic radiation. However, just as seismology uses waves generated by earthquakes to reveal the interior structure of the Earth, the discipline of helioseismology makes use of pressure waves (infrasound) traversing the Suns interior to measure and visualize the stars inner structure.[44] Computer modeling of the Sun is also used as a theoretical tool to investigate its deeper layers. Core Main article: Solar core The structure of the Sun The core of the Sun is considered to extend from the center to about 20–25% of the solar radius.[45] It has a density of up to150 g/cm3[46][47] (about 150 times the density of water) and a temperature of close to 15.7 million kelvin (K).[47] By contrast, the Suns surface temperature is approximately 5,800 K. Recent analysis of SOHO mission data favors a faster rotation rate in the core than in the rest of the radiative zone.[45] Through most of the Suns life, energy is produced by nuclear fusion through a series of steps called the p–p (proton–proton) chain; this process converts hydrogen into helium.[48] Only 0.8% of the energy generated in the Sun comes from the CNO cycle.[49] The core is the only region in the Sun that produces an appreciable amount of thermal energy through fusion; 99% of the power is generated within 24% of the Suns radius, and by 30% of the radius, fusion has stopped nearly entirely. The rest of the star is heated by energy that is transferred outward by radiation from the core to the convective layers just outside. The energy produced by fusion in the core must then travel through many successive layers to the solar photosphere before it escapes into space as sunlight or the kinetic energy of particles.[50][51] The proton–proton chain occurs around 9.2×1037 times each second in the core. Since this reaction uses four free protons (hydrogen nuclei), it converts about 3.7×1038 protons to alpha particles (helium nuclei) every second (out of a total of ~8.9×1056 free protons in the Sun), or about 6.2×1011 kg per second.[51] Since fusing hydrogen into helium releases around 0.7% of the fused mass as energy,[52] the Sun releases energy at the mass–energy conversion rate of 4.26 million metric tons per second, 384.6 yotta watts(3.846×1026 W),[1] or 9.192×1010 megatons of TNT per second. The power production by fusion in the core varies with distance from the solar center. At the center of the Sun, theoretical models estimate it to be approximately 276.5 watts/m3,[53] a power production density that more nearly approximates reptile metabolism than a thermonuclear bomb.[e] Peak power production in the Sun has been compared to the volumetric heats generated in an active compost heap. The tremendous power output of the Sun is not due to its high power per volume, but instead due to its large size. The fusion rate in the core is in a self-correcting equilibrium: a slightly higher rate of fusion would cause the core to heat up more and expand slightly against the weight of the outer layers, reducing the fusion rate and correcting the perturbation; and a slightly lower rate would cause the core to cool and shrink slightly, increasing the fusion rate and again reverting it to its present level.[54][55] The gamma rays (high-energy photons) released in fusion reactions are absorbed in only a few millimeters of solar plasma and then re-emitted again in a random direction and at slightly lower energy. Therefore it takes a long time for radiation to reach the Suns surface. Estimates of the photon travel time range between 10,000 and 170,000 years.[56] In contrast, it takes only 2.3 seconds for the neutrinos, which account for about 2% of the total energy production of the Sun, to reach the surface. Since energy transport in the Sun is a process which involves photons in thermodynamic equilibrium with matter, the time scale of energy transport in the Sun is longer, on the order of 30,000,000 years. This is the time it would take the Sun to return to a stable state if the rate of energy generation in its core were suddenly to be changed.[57] During the final part of the photons trip out of the sun, in the convective outer layer, collisions are fewer and far between, and they have less energy. The photosphere is the transparent surface of the Sun where the photons escape as visible light. Each gamma ray in the Suns core is converted into several million photons of visible light before escaping into space. Neutrinos are also released by the fusion reactions in the core, but unlike photons they rarely interact with matter, so almost all are able to escape the Sun immediately. For many years measurements of the number of neutrinos produced in the Sun were lower than theories predicted by a factor of 3. This discrepancy was resolved in 2001 through the discovery of the effects of neutrino oscillation: the Sun emits the number of neutrinos predicted by the theory, but neutrino detectors were missing 2⁄3 of them because the neutrinos had changed flavor by the time they were detected.[58] Cross-section of a solar-type star (NASA) Radiative zone Main article: Radiation zone Below about 0.7 solar radii, solar material is hot and dense enough that thermal radiation is the primary means of energy transfer from the core.[59] This zone is not regulated by thermal convection; however the temperature drops from approximately 7 to 2 million kelvin with increasing distance from the core.[47] This temperature gradient is less than the value of the adiabatic lapse rate and hence cannot drive convection.[47] Energy is transferred by radiation—ions of hydrogen and helium emit photons, which travel only a brief distance before being reabsorbed by other ions.[59] The density drops a hundredfold (from 20 g/cm3 to only 0.2 g/cm3) from 0.25 solar radii to the top of the radiative zone.[59] The radiative zone and the convective zone are separated by a transition layer, the tachocline. This is a region where the sharp regime change between the uniform rotation of the radiative zone and the differential rotation of the convection zone results in a large shear—a condition where successive horizontal layers slide past one another.[60] The fluid motions found in the convection zone above, slowly disappear from the top of this layer to its bottom, matching the calm characteristics of the radiative zone on the bottom. Presently, it is hypothesized (see Solar dynamo), that a magnetic dynamo within this layer generates the Suns magnetic field.[47] Convective zone Main article: Convection zone In the Suns outer layer, from its surface to approximately 200,000 km below (70% of the solar radius away from the center), the temperature is lower than in the radiative zone and heavier atoms are not fully ionized. As a result, radiative heat transport is less effective. The density of the gases are low enough to allow convective currents to develop. Material heated at the tachocline picks up heat and expands, thereby reducing its density and allowing it to rise. As a result, thermal convection develops as thermal cells carry the majority of the heat outward to the Suns photosphere. Once the material cools off at the photosphere, its density increases, and it sinks to the base of the convection zone, where it picks up more heat from the top of the radiative zone and the cycle continues. At the photosphere, the temperature has dropped to 5,700 K and the density to only 0.2 g/m3 (about 1/6,000th the density of air at sea level).[47] The thermal columns in the convection zone form an imprint on the surface of the Sun as the solar granulation and supergranulation. The turbulent convection of this outer part of the solar interior causes small-scale dynamos that produces magnetic north and south poles all over the surface of the Sun.[47] The Suns thermal columns are Bénard cells and take the shape of hexagonal prisms.[61] Photosphere The effective temperature, or black bodytemperature, of the Sun (5777 K) is the temperature a black body of the same size must have to yield the same total emissive power. Main article: Photosphere The visible surface of the Sun, the photosphere, is the layer below which the Sun becomes opaque to visible light.[62] Above the photosphere visible sunlight is free to propagate into space, and its energy escapes the Sun entirely. The change in opacity is due to the decreasing amount of H− ions, which absorb visible light easily.[62] Conversely, the visible light we see is produced as electrons react with hydrogen atoms to produce H− ions.[63][64]The photosphere is tens to hundreds of kilometers thick, being slightly less opaque than air on Earth. Because the upper part of the photosphere is cooler than the lower part, an image of the Sun appears brighter in the center than on the edge or limb of the solar disk, in a phenomenon known aslimb darkening.[62] The spectrum of sunlight has approximately the spectrum of a black-body radiating at about 6,000 K, interspersed with atomicabsorption lines from the tenuous layers above the photosphere. The photosphere has a particle density of ~1023 m−3 (about 0.37% of the particle number per volume of the Earths atmosphere at sea level). The photosphere is not fully ionized—the extent of ionization is about 3%, leaving almost all of the hydrogen in atomic form.[65] During early studies of the optical spectrum of the photosphere, some absorption lines were found that did not correspond to any chemical elementsthen known on Earth. In 1868, Norman Lockyer hypothesized that these absorption lines were caused by a new element which he dubbed helium, after the Greek Sun god Helios. Twenty-five years later, helium was isolated on Earth.[66] Atmosphere See also: Corona and Coronal loop During a total solar eclipse, the solarcorona can be seen with the naked eye, during the brief period of totality. The parts of the Sun above the photosphere are referred to collectively as the solar atmosphere.[62] They can be viewed with telescopes operating across the electromagnetic spectrum, from radio through visible light to gamma rays, and comprise five principal zones: the temperature minimum, thechromosphere, the transition region, the corona, and the heliosphere.[62] The heliosphere, which may be considered the tenuous outer atmosphere of the Sun, extends outward past the orbit of Pluto to the heliopause, which forms the boundary with the interstellar medium. The chromosphere, transition region, and corona are much hotter than the surface of the Sun.[62] The reason has not been conclusively proven; evidence suggests that Alfvén wavesmay have enough energy to heat the corona.[67] The coolest layer of the Sun is a temperature minimum region about 500 km above the photosphere, with a temperature of about 4,100 K.[62] This part of the Sun is cool enough to allow simple molecules such as carbon monoxide and water, which can be detected by their absorption spectra.[68] Above the temperature minimum layer is a layer about 2,000 km thick, dominated by a spectrum of emission and absorption lines.[62] It is called thechromosphere from the Greek root chroma, meaning color, because the chromosphere is visible as a colored flash at the beginning and end of total eclipses of the Sun.[59] The temperature in the chromosphere increases gradually with altitude, ranging up to around 20,000 K near the top.[62] In the upper part of chromosphere helium becomes partially ionized.[69] Taken by Hinodes Solar Optical Telescope on January 12, 2007, this image of the Sun reveals the filamentary nature of the plasma connecting regions of different magnetic polarity. Above the chromosphere, in a thin (about 200 km) transition region, the temperature rises rapidly from around 20,000 K in the upper chromosphere to coronal temperatures closer to 1,000,000 K.[70] The temperature increase is facilitated by the full ionization of helium in the transition region, which significantly reduces radiative cooling of the plasma.[69] The transition region does not occur at a well-defined altitude. Rather, it forms a kind of nimbus around chromospheric features such as spicules and filaments, and is in constant, chaotic motion.[59] The transition region is not easily visible from Earths surface, but is readily observable from space by instruments sensitive to the extreme ultraviolet portion of the spectrum.[71] The corona is the extended outer atmosphere of the Sun, which is much larger in volume than the Sun itself. The corona continuously expands into space becoming the solar wind, which fills all the Solar System.[72] The low corona, near the surface of the Sun, has a particle density around 1015–1016 m−3.[69][f] The average temperature of the corona and solar wind is about 1,000,000–2,000,000 K; however, in the hottest regions it is 8,000,000–20,000,000 K.[70] While no complete theory yet exists to account for the temperature of the corona, at least some of its heat is known to be from magnetic reconnection.[70][72] The heliosphere, which is the volume around the Sun filled with the solar wind plasma, begins from approximately 20 solar radii (0.1 AU) and extends to the outer fringes of the Solar System. Its inner boundary is defined as the layer in which the flow of thesolar wind becomes superalfvénic—that is, where the flow becomes faster than the speed of Alfvén waves.[73] Turbulence and dynamic forces in the heliosphere cannot affect the shape of the solar corona within, because the information can only travel at the speed of Alfvén waves. The solar wind travels outward continuously through the heliosphere, forming the solar magnetic field into a spiral shape,[72] until it impacts the heliopause more than 50 AU from the Sun. In December 2004, the Voyager 1 probe passed through a shock front that is thought to be part of the heliopause. Both of the Voyager probes have recorded higher levels of energetic particles as they approach the boundary.[74] Magnetic field See also: Stellar magnetic field In this false-color ultraviolet image, the Sun shows a C3-class solar flare (white area on upper left), a solar tsunami (wave-like structure, upper right) and multiple filaments of plasma following a magnetic field, rising from the stellar surface. The heliospheric current sheet extends to the outer reaches of the Solar System, and results from the influence of the Suns rotating magnetic field on the plasma in theinterplanetary medium.[75] The Sun is a magnetically active star. It supports a strong, changing magnetic field that varies year-to-year and reverses direction about every eleven years around solar maximum.[76] The Suns magnetic field leads to many effects that are collectively called solar activity, including sunspots on the surface of the Sun, solar flares, and variations in solar wind that carry material through the Solar System.[77] The effects of solar activity on Earth include auroras at moderate to high latitudes and the disruption of radio communications and electric power. Solar activity is thought to have played a large role in the formation and evolution of the Solar System. Solar activity changes the structure of Earths outer atmosphere.[78] All matter in the Sun is in the form of gas and at high temperatures, plasma. This makes it possible for the Sun to rotate faster at its equator (about 25 days) than it does at higher latitudes (about 35 days near its poles). The differential rotation of the Suns latitudes causes its magnetic field lines to become twisted together over time, producing magnetic field loops to erupt from the Suns surface and trigger the formation of the Suns dramaticsunspots and solar prominences (see Magnetic reconnection). This twisting action creates the solar dynamo and an 11-year solar cycle of magnetic activity as the Suns magnetic field reverses itself about every 11 years.[79][80] The solar magnetic field extends well beyond the Sun itself. The magnetized solar wind plasma carries the Suns magnetic field into space forming what is called the interplanetary magnetic field.[72] Since the plasma can only move along the magnetic field lines, the interplanetary magnetic field is initially stretched radially away from the Sun. Because the fields above and below the solar equator have different polarities pointing towards and away from the Sun, there exists a thin current layer in the solar equatorial plane, which is called the heliospheric current sheet.[72] At great distances, the rotation of the Sun twists the magnetic field and the current sheet into the Archimedean spiral like structure called the Parker spiral.[72] The interplanetary magnetic field is much stronger than the dipole component of the solar magnetic field. The Suns dipole magnetic field of 50–400 μT (at the photosphere) reduces with the cube of the distance to about 0.1 nT at the distance of the Earth. However, according to spacecraft observations the interplanetary field at the Earths location is around 5 nT, about a hundred times greater.[81] The difference is due to magnetic fields generated by electrical currents in the plasma surrounding the Sun. Chemical composition Image taken by NASA STEREO probes launched in 2006; utilizing two spacecraft to image the Sun at the extreme UVwavelength (171 Å). The Sun is composed primarily of the chemical elements hydrogen and helium; they account for 74.9% and 23.8% of the mass of the Sun in the photosphere, respectively.[82] All heavier elements, called metals in astronomy, account for less than 2% of the mass. The most abundant metals are oxygen (roughly 1% of the Suns mass), carbon (0.3%), neon (0.2%), and iron (0.2%).[83] The Sun inherited its chemical composition from the interstellar medium out of which it formed. The hydrogen and helium in the Sun were produced byBig Bang nucleosynthesis, and the metals were produced by stellar nucleosynthesis in generations of stars which completed their stellar evolution and returned their material to the interstellar medium before the formation of the Sun.[84] The chemical composition of the photosphere is normally considered representative of the composition of the primordial Solar System.[85] However, since the Sun formed, some of the helium and heavy elements have gravitationally settled from the photosphere. Therefore, in todays photosphere the helium fraction is reduced and the metallicity is only 84% of that in the protostellar phase (before nuclear fusion in the core started). The protostellar Suns composition was reconstructed as 71.1% hydrogen, 27.4% helium, and 1.5% metals.[82] In the inner portions of the Sun, nuclear fusion has modified the composition by converting hydrogen into helium, so the innermost portion of the Sun is now roughly 60% helium, with the metal abundance unchanged. Because the interior of the Sun is radiative, not convective (see Radiative zone above), none of the fusion products from the core have risen to the photosphere.[86] The reactive core zone of Hydrogen Burning, where hydrogen is converted into helium, is starting to surround the core of Helium ash. This development will continue and will eventually cause the sun to leave the Main Sequence, to become a Red Giant[87] The solar heavy-element abundances described above are typically measured both using spectroscopy of the Suns photosphere and by measuring abundances in meteorites that have never been heated to melting temperatures. These meteorites are thought to retain the composition of the protostellar Sun and thus not affected by settling of heavy elements. The two methods generally agree well.[15] Singly ionized iron group elements In the 1970s, much research focused on the abundances of iron group elements in the Sun.[88][89] Although significant research was done, the abundance determination of some iron group elements (e.g., cobalt and manganese) was still difficult at least as far as 1978 because of their hyperfine structures.[88] The first largely complete set of oscillator strengths of singly ionized iron group elements were made available first in the 1960s,[90] and improved oscillator strengths were computed in 1976.[91] In 1978 the abundances of singly Ionized elements of the iron group were derived.[88] Solar and planetary mass fractionation relationship Various authors have considered the existence of a mass fractionation relationship between the isotopic compositions of solar and planetary noble gases,[92] for example correlations between isotopic compositions of planetary and solar neon and xenon.[93] Nevertheless, the belief that the whole Sun has the same composition as the solar atmosphere was still widespread, at least until 1983.[94] In 1983, it was claimed that it was the fractionation in the Sun itself that caused the fractionation relationship between the isotopic compositions of planetary and solar wind implanted noble gases.[94] Solar cycles Main articles: Sunspots and List of solar cycles Sunspots and the sunspot cycle Measurements of solar cycle variation during the last 30 years When observing the Sun with appropriate filtration, the most immediately visible features are usually its sunspots, which are well-defined surface areas that appear darker than their surroundings because of lower temperatures. Sunspots are regions of intense magnetic activity where convection is inhibited by strong magnetic fields, reducing energy transport from the hot interior to the surface. The magnetic field causes strong heating in the corona, forming active regions that are the source of intense solar flares and coronal mass ejections. The largest sunspots can be tens of thousands of kilometers across.[95] The number of sunspots visible on the Sun is not constant, but varies over an 11-year cycle known as the solar cycle. At a typical solar minimum, few sunspots are visible, and occasionally none at all can be seen. Those that do appear are at high solar latitudes. As the sunspot cycle progresses, the number of sunspots increases and they move closer to the equator of the Sun, a phenomenon described by Spörers law. Sunspots usually exist as pairs with opposite magnetic polarity. The magnetic polarity of the leading sunspot alternates every solar cycle, so that it will be a north magnetic pole in one solar cycle and a south magnetic pole in the next.[96] History of the number of observed sunspots during the last 250 years, which shows the ~11-year solar cycle The solar cycle has a great influence on space weather, and a significant influence on the Earths climate since the Suns luminosity has a direct relationship with magnetic activity.[97] Solar activity minima tend to be correlated with colder temperatures, and longer than average solar cycles tend to be correlated with hotter temperatures. In the 17th century, the solar cycle appeared to have stopped entirely for several decades; few sunspots were observed during this period. During this era, known as the Maunder minimum or Little Ice Age, Europe experienced unusually cold temperatures.[98]Earlier extended minima have been discovered through analysis of tree rings and appear to have coincided with lower-than-average global temperatures.[99] Possible long-term cycle A recent theory claims that there are magnetic instabilities in the core of the Sun that cause fluctuations with periods of either 41,000 or 100,000 years. These could provide a better explanation of the ice ages than the Milankovitch cycles.[100][101] Life phases Main articles: Formation and evolution of the Solar System and Stellar evolution The Sun today is roughly halfway through the most stable part of its life. It has not changed dramatically for several billion[b] years, and will remain fairly unchanged for several billion more. However after hydrogen fusion in its core has stopped, the Sun will undergo severe changes, both internally and externally. Formation The Sun was formed about 4.57 billion years ago from the collapse of part of a giant molecular cloud that consisted mostly of hydrogen and helium and which probably gave birth to many other stars.[102] This age is estimated using computer models of stellar evolution and through nucleocosmochronology.[9] The result is consistent with the radiometric date of the oldest Solar System material, at 4.567 billion years ago.[103][104] Studies of ancient meteorites reveal traces of stable daughter nuclei of short-lived isotopes, such as iron-60, that form only in exploding, short-lived stars. This indicates that one or more supernovae must have occurred near the location where the Sun formed. A shock wave from a nearby supernova would have triggered the formation of the Sun by compressing the gases within the molecular cloud and causing certain regions to collapse under their own gravity.[105] As one fragment of the cloud collapsed it also began to rotate due toconservation of angular momentum and heat up with the increasing pressure. Much of the mass became concentrated in the center, while the rest flattened out into a disk which would become the planets and other solar system bodies. Gravity and pressure within the core of the cloud generated a lot of heat as it accreted more gas from the surrounding disk, eventually triggering nuclear fusion. Thus, the Sun was born. Main sequence Evolution of the Suns luminosity, radius and effective temperature compared to the present Sun. After Ribas (2010)[106] The Sun is about halfway through its main-sequence stage, during which nuclear fusion reactions in its core fuse hydrogen into helium. Each second, more than four million tonnes of matter are converted into energy within the Suns core, producing neutrinos and solar radiation. At this rate, the Sun has so far converted around 100 Earth-masses of matter into energy. The Sun will spend a total of approximately 10 billion years as a main-sequence star.[107] After core hydrogen exhaustion The size of the current Sun (now in the main sequence) compared to its estimated size during its red giant phase in the future The Sun does not have enough mass to explode as a supernova. Instead it will exit the main sequence in approximately 5.4 billion years and start to turn into a red giant. It is calculated that the Sun will become sufficiently large to engulf the current orbits of the solar systems inner planets, possibly including Earth.[108][109] Even before it becomes a red giant, the luminosity of the Sun will have nearly doubled, and the Earth will be hotter than Venus is today. Once the core hydrogen is exhausted in 5.4 billion years, the Sun will expand into asubgiant phase and slowly double in size over about half a billion years. It will then expand more rapidly over about half a billion years until it is over two hundred times larger than today and a couple of thousand times more luminous. This then starts the red giant branch (RGB) phase where the Sun will spend around a billion years and lose around a third of its mass.[109] Evolution of a sun-like star. The track of a one solar mass star on the Hertzsprung–Russell diagram is shown from the main sequence to the post-AGB stage. After RGB the Sun now has only about 120 million years of active life left, but they are highly eventful. First the core ignites violently in the helium flash, and the Sun shrinks back to around 10 times its current size with 50 times the luminosity, with a temperature a little lower than today. It has now reached thered clump or horizontal branch (HB), but a star of the Suns mass does not evolve blueward along the HB. Instead it just becomes mildly larger and more luminous over about 100 million years as it continues to burn helium in the core.[109] When the helium is exhausted, the Sun will repeat the expansion it followed when the hydrogen in the core was exhausted, except that this time it all happens faster, and the Sun becomes larger and more luminous. This is the asymptotic giant branch (AGB) phase, and the Sun is alternately burning hydrogen in a shell or helium in a deeper shell. After about 20 million years on the early AGB, the Sun becomes increasingly unstable, with rapid mass loss and thermal pulses that increase the size and luminosity for a few hundred years every 100,000 years or so. The thermal pulses become larger each time, with the later pulses pushing the luminosity to as much as 5,000 times the current level and the radius to over 1 AU.[110] Models vary depending on the rate and timing of mass loss. Models that have higher mass loss on the RGB produce smaller, less luminous stars at the tip of the AGB, perhaps only 2,000 times the luminosity and less than 200 times the radius.[109] For the Sun, four thermal pulses are predicted before it completely loses its outer envelope and starts to make a planetary nebula. By the end of that phase - lasting approximately 500,000 years - the Sun will only have about half of its current mass. The post AGB evolution is even faster. The luminosity stays approximately constant while the temperature increases, with the ejected half of the Suns mass becoming ionised into a planetary nebula as the exposed core reaches 30,000K. The final naked core temperature will be over 100,000K, after which the remnant will cool towards a white dwarf. The planetary nebula will disperse in about 10,000 years, but the white dwarf will survive for trillions of years before fading to black.[111][112] Earths fate Main article: Future of the Earth An artists depiction of the Sun entering its red giant phase viewed from Earth. All life on Earth is extinct at this phase. At its largest, the Sun will have a maximum radius beyond the Earths current orbit, 1 AU (1.5×1011 m), 250 times the present radius of the Sun.[113] When the Sun is an asymptotic giant branch star, it will have lost roughly 30% of its present mass due to a stellar wind, so the orbits of the planets will move outward. Also,tidal acceleration will help boost the Earth to a higher orbit (similar to what the Earth does to the moon). If it were only for this, Earth would probably remain outside the Sun. However, new research suggests that after the Sun becomes a red giant, Earth will be pulled in owing to tidal deceleration.[113] If Earth should escape incineration in the Sun, its water will be boiled away and most of its atmosphere will escape into space. During its life in the main sequence, the Sun is becoming more luminous (about 10% every 1 billion years) and its surface temperature is slowly rising. The Sun used to be fainter in its early past. The increase in solar temperatures is such that in about another billion years the surface of the Earth will probably become too hot for liquid water to exist, rendering it inhospitable to all known terrestrial life.[113][114] Sunlight Main article: Sunlight Comparison of the Suns apparent size, as seen from the vicinity of Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune and Pluto Sunlight is Earths primary source of energy. The only other source of energy the Earth has are the fissionable materials generated by the cataclysmic death of another star. These fissionable materials trapped in the Earths crust is what gives rise to geothermal energy, which drives the volcanism on Earth while also making it possible for mankind to fuel nuclear reactors. The solar constant is the amount of power that the Sun deposits per unit area that is directly exposed to sunlight. The solar constant is equal to approximately 1,368 W/m2 (watts per square meter) at a distance of one astronomical unit (AU) from the Sun (that is, on or near Earth).[115] Sunlight at the top of Earths atmosphere is composed (by total energy) of about 50% infrared light, 40% visible light, and 10% ultraviolet light.[116] Sunlight on the surface of Earth is attenuated by the Earths atmosphere so that less power arrives at the surface—closer to1,000 W/m2 in clear conditions when the Sun is near the zenith.[117] The atmosphere in particular filters out over 70% of solar ultraviolet, especially at the shorter wavelengths.[118]
Posted on: Fri, 24 Jan 2014 08:16:54 +0000
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