Barnard's Star, also known as Barnard's Runaway Star, is a very low-mass red dwarf star approximately six light-years away from Earth in the constellation of Ophiuchus (the Snake-holder). It is very old, and moving relatively fast.
In 1916, the American astronomer E. E. Barnard measured its proper motion as 10.3 arcseconds per year. This is the largest-known proper motion of any star relative to the Sun. At a distance of about 1.8 parsecs from the Solar System, or just under six light-years, Barnard's Star is the nearest known star in the constellation Ophiuchus, and the fourth-closest known individual star to the Sun, after the three components of the Alpha Centauri system. Despite its proximity, Barnard's Star, at a dim apparent magnitude of about nine, is not visible with the unaided eye; however, it is much brighter in infrared light than it is in visible light.
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Barnard's Star has been the subject of much study, and it has probably received more attention from astronomers than any other class M dwarf star due to its proximity and favorable location for observation near the celestial equator. Barnard's Star is also notable as the target for Project Daedalus, a study on the possibility of fast, unmanned travel to nearby star systems.
At seven to 12 billion years of age, Barnard's Star is considerably older than the Sun, and it might be among the oldest stars in the Milky Way galaxy. Barnard's Star rotates just once every 130 days (compared with just over 25 days for the Sun). In 1998 astronomers saw an intense flare, showing that Barnard's Star is a 'flare star'. Barnard's Star has the variable star designation V2500 Ophiuchi.
The proper motion of Barnard's Star is 'sideways' relative to our line of sight to the Sun of 90 kilometers per second (km/s). The 10.3 seconds of arc it travels annually amount to a quarter of a degree in a human lifetime, roughly half the angular diameter of the full Moon.
The radial velocity of Barnard's Star towards the Sun can be measured by its blue shift. These measurements, combined with proper motion, suggest a true velocity relative to the Sun of about 140 km/s.
Barnard's Star will make its closest approach to the Sun around AD 11,700, when it approaches to within about 3.8 light-years. However, at that time, it will not be the nearest star, since Proxima Centauri will have moved even closer to the Sun. Barnard's Star will still be too dim to be seen with the naked eye at the time of its closest approach, since its apparent magnitude will be about 8.5 then. After that it will gradually recede from the Sun.
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- "Parallax of Barnard's "Runaway" Star". Nature 99 (2484): 293–293. 1917. .
- Barnard, E.E. (1916). "A small star with large proper motion". Astronomical Journal 29 (695): 181. .
- Dawson P.C. & De Robertis M.M. (2004). "Barnard's Star and the M Dwarf temperature scale". Astronomical Journal 127 (5): 2909. .
- Riedel et al, A.R. (2005). "Barnard's Star as a proxy for old disk dM Stars: magnetic activity, light variations, XUV irradiances, and planetary habitable zones". Bulletin of the American Astronomical Society 37: 442.
- Croswell, Ken (2005). "A Flare for Barnard's Star". Astronomy Magazine. http://www.astronomy.com/asy/default.aspx?c=a&id=3658. Retrieved 2006-08-10.
- Kaler, James B. (2005). "Barnard's Star (V2500 Ophiuchi)". Stars. James B. Kaler. http://www.astro.uiuc.edu/~kaler/sow/barnard.html. Retrieved September 7, 2006.
- García-Sánchez, J. (2001). "Stellar encounters with the solar system". Astronomy & Astrophysics 379: 642. .
- Matthews R.A.J. et al. (1994). "The close approach of stars in the solar neighborhood". Quarterly Journal of the Royal Astronomical Society 35: 1–9.