Difference between revisions of "Wolf 359"
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| − | Wolf 359 is the fourth closest star at only 7.7 light years; only [[Proxima Centauri]], [[Alpha Centauri]] and [[Barnard's Star]] | + | {{Night Sky |
| + | | image =Leo constellation map.JPG | ||
| + | | designation =Wolf 359<br/>CN Leonis | ||
| + | | rightascension =10<sup>h</sup> 56<sup>m</sup> 28.865<sup>s</sup><ref name=simbad>[http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Wolf+359&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Wolf 359] from the [http://simbad.u-strasbg.fr/simbad SIMBAD Astronomical Database]</ref> | ||
| + | | declination =+07° 00′ 52.77″<ref name=simbad/> | ||
| + | | distance =7.78 ly<ref name=solstation>[http://www.solstation.com/stars/wolf359.htm Wolf 359] from solstation.com</ref> | ||
| + | | constellation =Leo | ||
| + | | type =Star | ||
| + | | dimensions = | ||
| + | | magnitude =Apparent Mag: 13.54<ref>Landolt, A. (1992). UBVRI photometric standard stars in the magnitude range 11.5-16.0 around the celestial equator. ''The Astronomical Journal'', 104, p.340. [https://ui.adsabs.harvard.edu/#abs/1992AJ....104..340L Astrophysics Data System]</ref><br/>Absolute Mag: 16.64<ref>From definition of absolute magnitude, using apparent magnitude (+13.54) and distance (7.78 ly) given here.</ref> | ||
| + | | redshift = | ||
| + | | radvelocity =19±1 km/s<ref name=simbad/> | ||
| + | | propmotion =RA: -3842 mas/yr<ref name=simbad/><br/>Dec.: -2725 mas/yr<ref name=simbad/> | ||
| + | | parallax =419.1 ± 2.10 mas<ref name=simbad/> | ||
| + | }} | ||
| + | '''Wolf 359''' is the fourth closest star at only 7.7 light years; only [[Proxima Centauri]], [[Alpha Centauri]] and [[Barnard's Star]] are closer. The star can be found in the [[constellation]] of [[Leo]]. One of the faintest known stars, it cannot be seen by the unaided eye and has a visual magnitude of only 13.54. | ||
| − | Discovered in 1918 by German astronomer Max Wolf, whom the star is named after, Wolf 359 is a dim [[red dwarf]] with a [[spectral class]] of | + | Discovered in 1918 by German astronomer Max Wolf, whom the star is named after, Wolf 359 is a dim [[red dwarf]] with a [[Star#Spectral Type|spectral class]] of M5.8Ve. The star's mass is between 9 and 13 percent of Sol's, and has a diameter of approximately 16 to 19 of Sol's. The luminosity is a mere 0.002% of our own star, so dim if Wolf 359 replaced our sun, it would appear only 10 times brighter then the moon from our world. Like many [[red dwarf]]s, Wolf 359 is a [[flare star]], and can violently [[solar flare|flare]] and brighten on occasion. However these flares are not as intense and are less frequent then on well known flare stars such as [[Luyten 726-8|UV Ceti]] or [[Proxima Centauri]].<ref>Gershberg, R. and Shakhovskaya, N. (1983). Characteristics of activity energetics of the UV cet-type flare stars. ''Astrophysics and Space Science'', 95(2), pp.235-253. [https://ui.adsabs.harvard.edu/#abs/1983Ap%26SS..95..235G Astrophysics Data System]</ref><ref name=solstation/> |
| − | At present there are no known companion bodies orbiting Wolf 359<ref> | + | At present there are no known companion bodies orbiting Wolf 359.<ref>Schroeder, D. et al. (2000). A Search for Faint Companions to Nearby Stars Using the Wide Field Planetary Camera 2. The Astronomical Journal, 119(2), pp.906-922. [https://ui.adsabs.harvard.edu/#abs/2000AJ....119..906S Astrophysics Data System]</ref> For an Earth-like world to have liquid water on its surface (within the [[habitable zone]]), it would have to be only 0.0042 AU from its parent star. Such a world would be tidally locked to Wolf 359, and be repeatedly exposed to intense radiation from the occasional flares. |
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==References== | ==References== | ||
{{reflist}} | {{reflist}} | ||
| + | |||
| + | {{Stars}} | ||
| + | |||
| + | [[Category:Astronomy]] | ||
| + | [[Category:Stars]] | ||
Latest revision as of 17:39, June 25, 2018
| Wolf 359 | |
|---|---|
| |
| Observational Data | |
| Designation | Wolf 359 CN Leonis |
| Right ascension | 10h 56m 28.865s[1] |
| Declination | +07° 00′ 52.77″[1] |
| Constellation | Leo |
| Type of object | Star |
| Magnitude | Apparent Mag: 13.54[2] Absolute Mag: 16.64[3] |
| Astrometry | |
| Distance from Earth | 7.78 ly[4] |
| Radial velocity | 19±1 km/s[1] |
| Proper motion | RA: -3842 mas/yr[1] Dec.: -2725 mas/yr[1] |
| Parallax | 419.1 ± 2.10 mas[1] |
Wolf 359 is the fourth closest star at only 7.7 light years; only Proxima Centauri, Alpha Centauri and Barnard's Star are closer. The star can be found in the constellation of Leo. One of the faintest known stars, it cannot be seen by the unaided eye and has a visual magnitude of only 13.54.
Discovered in 1918 by German astronomer Max Wolf, whom the star is named after, Wolf 359 is a dim red dwarf with a spectral class of M5.8Ve. The star's mass is between 9 and 13 percent of Sol's, and has a diameter of approximately 16 to 19 of Sol's. The luminosity is a mere 0.002% of our own star, so dim if Wolf 359 replaced our sun, it would appear only 10 times brighter then the moon from our world. Like many red dwarfs, Wolf 359 is a flare star, and can violently flare and brighten on occasion. However these flares are not as intense and are less frequent then on well known flare stars such as UV Ceti or Proxima Centauri.[5][4]
At present there are no known companion bodies orbiting Wolf 359.[6] For an Earth-like world to have liquid water on its surface (within the habitable zone), it would have to be only 0.0042 AU from its parent star. Such a world would be tidally locked to Wolf 359, and be repeatedly exposed to intense radiation from the occasional flares.
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Wolf 359 from the SIMBAD Astronomical Database
- ↑ Landolt, A. (1992). UBVRI photometric standard stars in the magnitude range 11.5-16.0 around the celestial equator. The Astronomical Journal, 104, p.340. Astrophysics Data System
- ↑ From definition of absolute magnitude, using apparent magnitude (+13.54) and distance (7.78 ly) given here.
- ↑ 4.0 4.1 Wolf 359 from solstation.com
- ↑ Gershberg, R. and Shakhovskaya, N. (1983). Characteristics of activity energetics of the UV cet-type flare stars. Astrophysics and Space Science, 95(2), pp.235-253. Astrophysics Data System
- ↑ Schroeder, D. et al. (2000). A Search for Faint Companions to Nearby Stars Using the Wide Field Planetary Camera 2. The Astronomical Journal, 119(2), pp.906-922. Astrophysics Data System
