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Sun

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This article is about Sun (disambiguation). For The Sun (disambiguation), see Sun (disambiguation).

The Sun, also known as Sol, is a star at the center of the solar system. It is a white star that gives off different types of energy such as infrared energy (heat), ultraviolet light, radio waves and light. It also gives off a stream of particles, which reaches Earth as "solar wind". The source of all this energy is nuclear fusion. Nuclear fusion is the reaction in the star which turns hydrogen into helium and makes huge amounts of energy. It is a nearly perfect ball of hot plasma.

Sun ☉
Sun white.jpg
Sun with sunspots and limb darkening as seen in visible light with solar filter.
The Sun by the Atmospheric Imaging Assembly of NASA's Solar Dynamics Observatory - 20100819.jpg
False-color photo of the Sun as seen in ultraviolet light (wavelength of 30.4 nm)
Observation data
Mean distance
from Earth		1 au ≈ 1.496×108 km[1]
8 min 19 s at light speed
Visual brightness (V)−26.74[2]
Absolute magnitude4.83[2]
Spectral classificationG2V[3]
MetallicityZ = 0.0122[4]
Angular size31.6–32.7 minutes of arc[5]
AdjectivesSolar
Orbital characteristics
Mean distance
from Milky Way core		≈ 2.7×1017 km
27,200 light-years
Galactic period(2.25–2.50)×108 yr
Velocity≈ 220 km/s (orbit around the center of the Milky Way)
≈ 20 km/s (relative to average velocity of other stars in stellar neighborhood)
≈ 370 km/s[6] (relative to the cosmic microwave background)
Physical characteristics
Equatorial radius695,700 km,[7]
696,342 km[8]
109 × Earth[9]
Equatorial circumference4.379×106 km[9]
109 × Earth[9]
Flattening9×10−6
Surface area6.09×1012 km2[9]
12,000 × Earth[9]
Volume1.41×1018 km3[9]
1,300,000 × Earth
Mass1.9885×1030 kg[2]
333,000 × Earth[2]
Average density1.408 g/cm3[2][9][10]
0.255 × Earth[2][9]
Center density (modeled)162.2 g/cm3[2]
12.4 × Earth
Equatorial surface gravity274 m/s2[2]
28 × Earth[9]
Moment of inertia factor0.070[2] (estimate)
Escape velocity
(from the surface)		617.7 km/s[9]
55 × Earth[9]
TemperatureCenter (modeled): 1.57×107 K[2]
Photosphere (effective): 5,778 K[2]
Corona: ≈ 5×106 K
Luminosity (Lsol)3.828×1026 W[2]
≈ 3.75×1028 lm
≈ 98 lm/W efficacy
Color (B-V)0.63
Mean radiance (Isol)2.009×107 W·m−2·sr−1
Age≈ 4.6 billion years[11][12]
Rotation characteristics
Obliquity7.25°[2]
(to the ecliptic)
67.23°
(to the galactic plane)
Right ascension
of North pole[13]		286.13°
19 h 4 min 30 s
Declination
of North pole		+63.87°
63° 52' North
Sidereal rotation period
(at equator)		25.05 d[2]
(at 16° latitude)25.38 d[2]
25 d 9 h 7 min 12 s[13]
(at poles)34.4 d[2]
Rotation velocity
(at equator)		7.189×103 km/h[9]
Photospheric composition (by mass)
Hydrogen73.46%[14]
Helium24.85%
Oxygen0.77%
Carbon0.29%
Iron0.16%
Neon0.12%
Nitrogen0.09%
Silicon0.07%
Magnesium0.05%
Sulfur0.04%
Sun

The Sun looks yellow to people on Earth, but it is really white. This happens because the air around the Earth scatters sunlight. The blue and green colors in the sunlight spread out more than the red and yellow colors. Because of this, the light that reaches our eyes is mostly red and yellow, making the Sun appear yellow. If we were in space, where there is no air to scatter the light, we would see that the Sun is actually white.

The Sun is a star like many others in our Milky Way galaxy. The Sun is a type of star called a G-type main-sequence star based on its spectral class.[15]

The Sun is about 4.5 billion years old.

The Sun is about a hundred times as wide as the Earth. It has a mass of 1.9891×1030 kg. This is 333,000 times the mass of the Earth. 1.3 million Earths can fit inside the Sun.[16] The Sun fuses about 600 million tons of hydrogen into helium every second.

The Sun is the main source of energy for the Earth. This energy is made deep inside the Sun in a process called nuclear fusion. Four hydrogen atoms are fused together to make one helium atom. Some of the leftover matter turns into energy. This is the same way energy is released in a hydrogen bomb.

It can take between 10,000 and 170,000 years for the energy in the core of the Sun to escape.

No Sun, no life on Earth

The Sun is the most important source of energy for life on Earth. Without the Sun, there would be no vegetation on Earth: every plant needs light to live and grow. Everything on Earth would freeze over without the Sun. The Sun gives the Earth heat as well as light. Plants make oxygen by photosynthesis. All humans and animals breathe oxygen. The Earth's position in the Solar System is just right for the development of life on Earth.

General characteristics

The Sun is a G-type main-sequence star. It has about 99.86% of the mass of the Solar System. The Sun has an absolute magnitude of +4.83. It is brighter than about 85% of the stars in the Milky Way galaxy.[17][18] The Sun is a Population I star,[19] i.e it a metal-rich fairly young star.

The Sun is the brightest object in the Earth's sky. It has an apparent magnitude of −26.74.[20] It takes 8 minutes and 20 seconds for light to travel from the Sun's surface to Earth's surface.[21]

Physics of the Sun

Origin

Scientists think that the Sun started from a very large cloud of dust and small bits of ice about 4.567 billion years ago.[22]

At the center of that huge cloud, gravity caused the material to build up into a ball. Once this got big enough, the huge pressure inside started a fusion reaction. The energy this released caused that ball to heat and shine. At its very center, hydrogen atoms collide together at great temperature and pressure and fuse to form atoms of helium. This process is called nuclear fusion. It was proposed by Hans Bethe just before World War II.

Orbit

The Sun and everything that orbits it is in the Milky Way galaxy. The Sun orbits around the centre of the Milky Way. It takes along everything in the Solar System. The Sun moves at 820,000 km an hour. At that speed, it still takes 230 million years for a full orbit.

Visible features

Since the Sun is all gas, surface features come and go. If the Sun is viewed through a special solar telescope, dark areas called sunspots can be seen. These areas are caused by the Sun's magnetic field. The sunspots only look dark because the rest of the Sun is very bright.

Some space telescopes, including the ones that orbit the Sun have seen huge arches of the Sun's matter extend suddenly from the Sun. These are called solar prominences. Solar prominences come in many different shapes and sizes. Some of them are so large that the Earth could fit inside of them, and a few are shaped like hands. Solar flares also come and go.

Sunspots, prominences and flares become rare, and then numerous, and then rare again, every 11 years.

Photosphere

This is the surface of the Sun. The light that the Earth receives from the Sun is radiated from this layer. Below this layer, the Sun is opaque, or not transparent to light.

Composition

The Sun is mainly composed of hydrogen and helium. All elements heavier than hydrogen and helium, account for less than 2% of the mass of the Sun.[23][24] The Sun's chemical composition was got from the interstellar medium. The hydrogen and most of the helium in the Sun would have been produced by Big Bang nucleosynthesis in the first 20 minutes of the universe. The heavier elements were produced by stars that died before the Sun was formed. The heavier elements were released into the interstellar medium when stars exploded as supernovae.[23][24]

Atmosphere

Five layers make up the atmosphere of the Sun. The chromosphere, transition region, and corona are much hotter than the outer photosphere surface of the Sun.[25] It is believed that Alfvén waves may pass through to heat the corona.[26]

The minimum temperature zone, the coolest layer of the Sun, is about 500 kilometres (310 miles) above the photosphere. It has a temperature of about 4,100 K (3,830 °C; 6,920 °F).[25] This part of the Sun is cool enough to allow simple molecules such as carbon monoxide and water to form. These molecules can be seen on the Sun with special instruments called spectroscopes.[27]

The chromosphere is the first layer of the Sun which can be seen, especially during a solar eclipse when the moon is covering most of the Sun and blocking the brightest light.

The solar transition region is the part of the Sun's atmosphere, between the chromosphere and outer part called the corona.[28] It can be seen from space using telescopes that can sense ultraviolet light. The transition is between two very different layers. In the bottom part it touches the photosphere and gravity shapes the features. At the top, the transition layer touches the corona.

The corona is the outer atmosphere of the Sun and is much bigger than the rest of the Sun. The corona continuously expands into space forming the solar wind, which fills all the Solar System.[29] The average temperature of the corona and solar wind is about 1,000,000–2,000,000 K (1,800,000–3,600,000 °F). In the hottest regions it is 8,000,000–20,000,000 K (14,400,000–36,000,000 °F).[30] We do not understand why the corona is so hot.[29][30] It can be seen during a solar eclipse or with an instrument called a coronagraph.

The heliosphere is the thin outer atmosphere of the Sun, filled with the solar wind plasma. It extends out past the orbit of Pluto to the heliopause, where it forms a boundary where it collides with the interstellar medium.[31]

Eclipses

A solar eclipse appears when the moon is between the Earth and Sun. The last total solar eclipse occurred on December 26, 2019, and was visible from Saudi Arabia, India, Sumatra and Borneo, with a partial eclipse visible in Australia and much of Asia.

A lunar eclipse happens when the moon passes through the shadow of the Earth which can only occur during a full moon. The number of lunar eclipses in a single year can range from 0 to 3. Partial eclipses slightly outnumber total eclipses by 7 to 6.[32]

Fate of the Sun

Astrophysicists say our Sun is a G-type main-sequence star in the middle of its life. In about billion years, increased solar energy will boil away the Earth's atmosphere and oceans. In a few more billion years, they think the Sun will get bigger and become a red giant star. The Sun would be up to 250 times its current size, as big as 1.4 AU (210,000,000 kilometres; 130,000,000 miles) and swallow up the Earth.

Earth's fate is still unknown. In the long term, the Earth's future depends on the Sun, and the Sun is going to be fairly stable for the next 5 billion years.[33][34] Calculations suggest that the Earth might move to a wider orbit. This is because about 30% of the Sun's mass will blow away in the solar wind. However, in the very long term the Earth will probably be destroyed as the Sun increases in size. Stars like the Sun become red giants at a later stage.[35] The Sun will expand beyond the orbits of Mercury, Venus, and probably Earth. In any event, the ocean and air would have vanished before the Sun gets to that stage.

After the Sun reaches a point where it can no longer get bigger, it will lose its layers and form a planetary nebula. Eventually, the Sun will shrink into a white dwarf. Then, over several hundred billion or even a trillion years, the Sun would fade into a black dwarf.

Sun Media

  • The Sun photographed on the 8th of May, 2019 in white light (true color). Sunspots AR2740 (to the right) and AR2741 (to the left) visible. Some other interesting features include faculae, white spots near AR2741, limb darkening, and tiny convection cells called granules all across its surface.

  • Astronomical/planetary symbol for the Sun and botanical symbol for annual plants; Daltonian symbol for hydrogen when red. Philatelic symbol for a used stamp.

  • Size comparison of the Sun, all the planets of the Solar System and some larger stars. The Sun is 1.4 million kilometers (4.643 light-seconds) wide, about 109 times wider than Earth, or four times the Lunar distance, and contains 99.86% of all Solar System mass.

  • Illustration of the Sun's structure, in false color for contrast

  • Illustration of a proton-proton reaction chain, from hydrogen forming deuterium, helium-3, and regular helium-4

  • Illustration of different stars' internal structure based on mass. The Sun in the middle has an inner radiating zone and an outer convective zone.

  • Image of the Sun's cell-like surface structures

  • 171879main LimbFlareJan12 lg

  • During a solar eclipse the solar corona can be seen with the naked eye during totality.

References

  1. ↑ Pitjeva, E. V.; Standish, E. M. (2009). "Proposals for the masses of the three largest asteroids, the Moon-Earth mass ratio and the Astronomical Unit". Celestial Mechanics and Dynamical Astronomy. 103 (4): 365–372. Bibcode:2009CeMDA.103..365P. doi:10.1007/s10569-009-9203-8. ISSN 1572-9478. S2CID 121374703.
  2. ↑ 2.00 2.01 2.02 2.03 2.04 2.05 2.06 2.07 2.08 2.09 2.10 2.11 2.12 2.13 2.14 2.15 Williams, D.R. (1 July 2013). "Sun Fact Sheet". NASA Goddard Space Flight Center. Archived from the original on 15 July 2010. Retrieved 12 August 2013.
  3. ↑ Zombeck, Martin V. (1990). Handbook of Space Astronomy and Astrophysics 2nd edition. Cambridge University Press.
  4. ↑ Asplund, M.; Grevesse, N.; Sauval, A.J. (2006). "The new solar abundances – Part I: the observations". Communications in Asteroseismology. 147: 76–79. Bibcode:2006CoAst.147...76A. doi:10.1553/cia147s76. ISSN 1021-2043.
  5. ↑ "Eclipse 99: Frequently Asked Questions". NASA. Archived from the original on 27 May 2010. Retrieved 24 October 2010.
  6. ↑ Hinshaw, G.; et al. (2009). "Five-year Wilkinson Microwave Anisotropy Probe observations: data processing, sky maps, and basic results". The Astrophysical Journal Supplement Series. 180 (2): 225–245. arXiv:0803.0732. Bibcode:2009ApJS..180..225H. doi:10.1088/0067-0049/180/2/225. S2CID 3629998.
  7. ↑ Mamajek, E.E.; Prsa, A.; Torres, G.; et, al. (2015). "IAU 2015 Resolution B3 on Recommended Nominal Conversion Constants for Selected Solar and Planetary Properties". arXiv:1510.07674 [astro-ph.SR]. 
  8. ↑ Emilio, Marcelo; Kuhn, Jeff R.; Bush, Rock I.; Scholl, Isabelle F. (2012), "Measuring the Solar Radius from Space during the 2003 and 2006 Mercury Transits", The Astrophysical Journal, 750 (2): 135, arXiv:1203.4898, Bibcode:2012ApJ...750..135E, doi:10.1088/0004-637X/750/2/135, S2CID 119255559
  9. ↑ 9.00 9.01 9.02 9.03 9.04 9.05 9.06 9.07 9.08 9.09 9.10 9.11 "Solar System Exploration: Planets: Sun: Facts & Figures". NASA. Archived from the original on 2 January 2008.
  10. ↑ Ko, M. (1999). Elert, G. (ed.). "Density of the Sun". The Physics Factbook.
  11. ↑ Bonanno, A.; Schlattl, H.; Paternò, L. (2002). "The age of the Sun and the relativistic corrections in the EOS". Astronomy and Astrophysics. 390 (3): 1115–1118. arXiv:astro-ph/0204331. Bibcode:2002A&A...390.1115B. doi:10.1051/0004-6361:20020749. S2CID 119436299.
  12. ↑ Connelly, JN; Bizzarro, M; Krot, AN; Nordlund, Å; Wielandt, D; Ivanova, MA (2 November 2012). "The Absolute Chronology and Thermal Processing of Solids in the Solar Protoplanetary Disk". Science. 338 (6107): 651–655. Bibcode:2012Sci...338..651C. doi:10.1126/science.1226919. PMID 23118187. S2CID 21965292. Retrieved 17 March 2014.(registration required)
  13. ↑ 13.0 13.1 Seidelmann, P.K.; et al. (2000). "Report Of The IAU/IAG Working Group On Cartographic Coordinates And Rotational Elements Of The Planets And Satellites: 2000". Archived from the original on 12 May 2020. Retrieved 22 March 2006.
  14. ↑ "The Sun's Vital Statistics". Stanford Solar Center. Retrieved 29 July 2008. Citing Eddy, J. (1979). A New Sun: The Solar Results From Skylab. NASA. p. 37. NASA SP-402.
  15. ↑ Connelly, J. N.; Bizzarro, M.; Krot, A. N.; Nordlund, A.; Wielandt, D.; Ivanova, M. A. (2012-11-02). "The absolute chronology and thermal processing of solids in the Solar protoplanetary Dpdisk". Science. 338 (6107): 651–655. Bibcode:2012Sci...338..651C. doi:10.1126/science.1226919. ISSN 0036-8075. PMID 23118187. S2CID 21965292.
  16. ↑ Bonanno, A.; Schlattl, H.; Paternò, L. (2002). "The age of the Sun and the relativistic corrections in the EOS". Astronomy & Astrophysics. 390 (3): 1115–1118. arXiv:astro-ph/0204331. Bibcode:2002A&A...390.1115B. doi:10.1051/0004-6361:20020749. ISSN 0004-6361. S2CID 119436299.
  17. ↑ January 2006, Ker Than 30 (30 January 2006). "Astronomers Had it Wrong: Most Stars are Single". Space.com. Retrieved 2020-09-15.
  18. ↑ Lada, Charles J. (2006-03-20). "Stellar multiplicity and the initial mass function: most stars are single". The Astrophysical Journal. 640 (1): L63–L66. arXiv:astro-ph/0601375. Bibcode:2006ApJ...640L..63L. doi:10.1086/503158. ISSN 0004-637X. S2CID 8400400.
  19. ↑ Zeilik, Michael. (1998). Introductory astronomy & astrophysics. Gregory, Stephen A. (4th ed.). Belmont Drive, CA: Brooks/Cole, Cengage Learning. ISBN 0-03-006228-4. OCLC 38157539.
  20. ↑ "Stellar parameters". Space Science Reviews. 43 (3–4). 1986. doi:10.1007/BF00190626. ISSN 0038-6308. S2CID 189796439.
  21. ↑ Simon, Anne Elizabeth, 1956- (2001). The real science behind the X-files : microbes, meteorites, and mutants (1st Touchstone ed.). New York: Simon & Schuster. ISBN 0-684-85618-2. OCLC 48151793.{{cite book}}: CS1 maint: multiple names: authors list (link)
  22. ↑ Connelly, James N.; et al. (2012). "The absolute chronology and thermal processing of solids in the solar protoplanetary disk". Science. 338 (6107): 651–655. Bibcode:2012Sci...338..651C. doi:10.1126/science.1226919. PMID 23118187. S2CID 21965292.
  23. ↑ 23.0 23.1 Lodders, Katharina (2003-07-10). "Solar System Abundances and Condensation Temperatures of the Elements". The Astrophysical Journal. 591 (2): 1220–1247. Bibcode:2003ApJ...591.1220L. doi:10.1086/375492. ISSN 0004-637X. S2CID 42498829.
  24. ↑ 24.0 24.1 Hansen, Carl J. (2004). Stellar interiors : physical principles, structure, and evolution. Kawaler, Steven D., Trimble, Virginia. (2nd ed.). New York: Springer. ISBN 0-387-20089-4. OCLC 53083938.
  25. ↑ 25.0 25.1 Abhyankar K.D. (1977). "A survey of the solar atmospheric models". Bull. Astr. Soc. India. 5: 40–44. Bibcode:1977BASI....5...40A.
  26. ↑ De Pontieu B.; et al. (2007). "Chromospheric Alfvénic waves strong enough to power the solar wind". Science. 318 (5856): 1574–77. Bibcode:2007Sci...318.1574D. doi:10.1126/science.1151747. PMID 18063784. S2CID 33655095.
  27. ↑ Solanki S.K; Livingston W. & Ayres T (1994). "New light on the heart of darkness of the solar chromosphere". Science. 263 (5143): 64–66. Bibcode:1994Sci...263...64S. doi:10.1126/science.263.5143.64. PMID 17748350. S2CID 27696504.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  28. ↑ "The Transition Region". Solar Physics, NASA Marshall Space Flight Center. NASA. Archived from the original on 2017-01-08. Retrieved 2012-12-12.
  29. ↑ 29.0 29.1 Russell, C.T. (2001). "Solar wind and interplanetary magnetic filed: A tutorial". In Song, Paul; Singer, Howard J. and Siscoe, George L. (ed.). Space weather (Geophysical Monograph) (PDF). American Geophysical Union. pp. 73–88. ISBN 978-0-87590-984-4. Archived from the original (PDF) on 2018-10-01. Retrieved 2012-12-12.{{cite book}}: CS1 maint: multiple names: editors list (link)
  30. ↑ 30.0 30.1 Erdèlyi R. & Ballai I. 2007. Heating of the solar and stellar coronae: a review. Astron. Nachr. 328 (8): 726–733
  31. ↑ European Space Agency (2005). "The distortion of the Heliosphere: our interstellar magnetic compass". Press release. http://www.spaceref.com/news/viewpr.html?pid=16394. Retrieved 2006-03-22. 
  32. ↑ "Lunar Eclipses for Beginners".
  33. ↑ The Sun's evolution
  34. ↑ Goldsmith D. & Owen T. 2001. The search for life in the universe. University Science Books, p. 96. ISBN 978-1-891389-16-0
  35. ↑ Schröder K.-P. & Smith R.C. 2008. Distant future of the Sun and Earth revisited. Monthly Notices of the Royal Astronomical Society 386 (1): 155–163. [1]

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