The Full Wiki

More info on 51 Ophiuchi

51 Ophiuchi: Wikis

Advertisements
  
  

Note: Many of our articles have direct quotes from sources you can cite, within the Wikipedia article! This article doesn't yet, but we're working on it! See more info or our list of citable articles.

Did you know ...


More interesting facts on 51 Ophiuchi

Include this on your site/blog:

Encyclopedia

From Wikipedia, the free encyclopedia

51 Ophiuchi
Observation data
Epoch J2000      Equinox J2000
Constellation Ophiuchus
Right ascension 17h 31m 24.94s[1]
Declination −23° 57′ 45″[1]
Apparent magnitude (V) 4.81[1]
Characteristics
Spectral type B9

The star 51 Ophiuchi (also called 51 Oph) is a young B-type star, lying approximately 410 light-years (130 pc) away in the constellation Ophiuchus, northwest of the center of the Milky Way. It is notable for being "a rare, nearby example of a young planetary system just entering the last phase of planet formation".[2]

Dust and gas disk

51 Ophiuchi has a disk of dust and gas that appears to be a young debris disk and is likely a planetary system in the late stages of formation. This system resembles Beta Pictoris, a well known star with a large debris disk, in several ways: spectral type, the presence of an edge-on disk with both gas and dust, and the presence of variable blue-shifted absorption lines suggesting in-falling comets.[2][3]

The distance to 51 Ophiuchi is much greater than the distance to Beta Pictoris, and its debris disk is relatively compact. As a consequence, the disk around 51 Ophiuchi requires an interferometer to resolve, in contrast to that of Beta Pictoris, which has been observed using visual spectrum imaging.[4] Recent observations of 51 Ophiuchi made with the Keck Interferometer Nuller at the W. M. Keck Observatory show that the disk has two components: a central cloud of large particles (exozodiacal dust) surrounded by a much larger cloud of small silicate particles extending to about 1,000 astronomical units.[3] The inner disk has a radius approximately four times the distance between the sun and the Earth, with a density of around 100,000 times that of the dust in our solar system.[2]

See also

References

  1. ^ a b c "* 51 oph—Star". SIMBAD. http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=bet+pic. Retrieved 2009-09-23.  
  2. ^ a b c "Twin Keck telescopes probe dual dust disks". e! Science News. 24 September 2009. http://esciencenews.com/articles/2009/09/24/twin.keck.telescopes.probe.dual.dust.disks. Retrieved 1 October 2009.  
  3. ^ a b Stark, Christopher C.; Kuchner, Marc J.; Traub, Wesley A.; Monnier, John D.; Serabyn, Eugene; Colavita, Mark; Koresko, Chris; Mennesson, Bertrand et al. (2009), "51 Ophiuchus: A Possible Beta Pictoris Analog Measured with the Keck Interferometer Nuller", Astrophysical Journal 703 (2): 1188–1197, doi:10.1088/0004-637X/703/2/1188  
  4. ^ Smith, B. A. and Terrile, R. J. (1984). "A circumstellar disk around Beta Pictoris". Science 226: 1421–1424. doi:10.1126/science.226.4681.1421. http://adsabs.harvard.edu/abs/1984Sci...226.1421S.  
Advertisements

Advertisements






Got something to say? Make a comment.
Your name
Your email address
Message