Sun
| The Sun | |
| Observation data | |
|---|---|
| Mean distance from Earth | 149.6×106 km (92.95×106 mi) |
| Visual brightness (V) | −26.8m |
| Absolute magnitude | 4.8m |
| Orbital characteristics | |
| Mean distance from Milky Way centre | ~2.5×1017 km (26,000 light-years) |
| Galactic period | ~2.26×108 a |
| Velocity | ~217 km/s |
| Physical characteristics | |
| Diameter | 1.392×106 km (109 Earths) |
| Oblateness | ~9×10-6 |
| Surface area | 6.09 × 1012 km² (11,900 Earths) |
| Volume | 1.41 × 1018 km³ (1,300,000 Earths) |
| Mass | 1.9891 × 1030 kg (332,950 Earths) |
| Density | 1.408 g/cm³ |
| Surface gravity | 273.95 m s-2 (27.9 g) |
| Escape velocity from the surface | 617.54 km/s |
| Surface temperature | 5780 K |
| Temperature of corona | 5 MK |
| Approximate core temperature | 13.6×106 K |
| Luminosity (LS) | 3.827×1026 J s-1 |
| Mean Intensity (IS) | 2.009×107 W m-2 sr-1 |
| Rotation characteristics | |
| Obliquity | 7.25º (to the ecliptic) 67.23º (to the galactic plane) |
| Right ascension of North pole 1 | 286.13º (19 h 4 min 31.2 s) |
| Declination of North pole | 63.87º |
| Rotation period at equator | 25.3800 days (25 d 9 h 7 min 12±8 s) 1 |
| Rotation velocity at equator | 7174.21 km/h |
| Photospheric composition | |
| Hydrogen | 73.46 % |
| 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 % |
Physical and other characteristics
The Sun is a main sequence star, with a spectral class of G2, meaning that it is somewhat more massive and hotter than the average star but far smaller than a blue giant star. A G2 star is on the main sequence, and has a lifetime of about 10 billion years (10 Ga), and the Sun formed about 5 Ga (5 billion years) ago, as determined by nucleocosmochronology. The Sun orbits the Milky Way galaxy at a distance of about 25,000 to 28,000 light-years from the galactic centre, completing one revolution in about 226 Ma (226 million years). The orbital speed is 217 km/s, i.e. 1 light-year in ca. 1400 years, and 1 AU in 8 days. The Sun is a near-perfect sphere, with an oblateness estimated at about 9 millionths (mostly due to the gravitation of Jupiter), which means the polar diameter differs from the equatorial by 10 km at most. This is because the centrifugal effect of the Sun's rather sedate rotation is 18 million times weaker than its surface gravity (at the equator). Extremely high resolution spectrum of the Sun showing thousands of elemental absorption lines ([[fraunhofer lines).]] The Sun does not have definite boundaries as rocky planets do. Instead, the density of gases comprising the Sun drops off following an exponential relationship with distance from the centre of the Sun. The Sun's radius is measured from centre to the edges of the photosphere. At the centre of the Sun, where its density is 1.5×105 kg/m3, thermonuclear reactions (nuclear fusion) convert hydrogen into helium. About 8.9×1037 protons (hydrogen nuclei) are converted to helium nuclei every second. This releases energy at the matter-energy conversion rate of 4.26 million tonnes per second or 383 yottawatts (9.15×1016 tons of TNT per second) which escapes from the surface of the Sun in the form of electromagnetic radiation and neutrinos (and to a smaller extent as the kinetic and thermal energy of solar wind plasma and as the energy in the Sun's magnetic field). A fusion reactor, which some physicists believe may one day provide power for human use, would use a similar process to extract atomic energy. All matter in the Sun is in the form of plasma due to its extreme temperature. This makes it possible for the Sun to rotate faster at its equator (about 25 days) than it does at higher latitudes (28 days near its poles). The differential rotation of the Sun's latitudes causes its magnetic field lines to become twisted together over time, causing magnetic field loops to erupt from the Sun's surface and trigger the formation of the Sun's dramatic sunspots and solar prominences. The solar activity cycle includes old magnetic fields being stripped off the Sun's surface starting from one pole and ending at the other. The corona has a particle density of 1011/m3, and the photosphere a particle density of 1023/m3. SOHO EIT304 instrument in the ultraviolet. (Animation (980kB MPEG)).]] For some time it was thought that the number of neutrinos produced by the nuclear reactions in the Sun was only one third of the number predicted by theory, a result that was termed the solar neutrino problem. Several neutrino observatories were created including the Sudbury Neutrino Observatory to try and measure the amount of neutrinos given off by the Sun. From these observatories and experiments it was recently found that neutrinos had rest mass, and could therefore transform into harder-to-detect varieties of neutrinos while en route from the Sun to Earth; thus measurement and theory were reconciled. To obtain an uninterrupted view of the Sun, the European Space Agency and NASA cooperatively launched the Solar and Heliospheric Observatory (SOHO) on December 2, 1995. Observation of the Sun can reveal such phenomena as:- Sunspots
- Faculae
- Granules
- Solar flares
- Solar prominences
- * Quiescent prominences
- * Eruptive prominences
- * Spicules
- Coronal mass ejection
- Limb darkening
The Death of the Sun
Our Sun is much too light to explode as a supernova. Instead, in 4-5 billion years it will enter its red giant phase, expanding as the hydrogen fuel in the core is consumed and it starts to burn helium and the core temperature rises to some 3×108K. While it is likely that this expansion will reach the current position of Earth's orbit, recent research suggests that mass loss from the Sun earlier in its red giant phase will cause the Earth's orbit to move further out, preventing it from being swallowed. Following the red giant phase, giant thermal pulsations will cause the Sun to throw off its outer layers to form a planetary nebula. The Sun will subsequently become a white dwarf, slowly cooling over many more billions of years.See also
- Astronomical twilight
- Solar radiation
- Solar radius
- Solar energy
- Solar wind
- * Aurora borealis
- * Aurora australis
- Photosphere
- Chromosphere
- Corona
- Airglow
- Eclipse
- Timeline of solar astronomy
- Solar deity
External links
- Current SOHO snapshots
- Far-Side Helioseismic Holography from Stanford
- NASA Eclipse homepage
- Nasa SOHO (Solar & Heliospheric Observatory) satelliteFAQ
- Solar Sounds from Stanford
- Spaceweather.com
- Eric Weisstein's World of Astronomy - Sun
| The Solar System | ||
| Mercury > Venus | Earth (Moon) > Mars | Asteroids |
| Saturn > Uranus | Neptune > Pluto | Kuiper belt > Oort cloud |