51 Ophiuchi
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Ophiuchus |
| Right ascension | 17h 31m 24.95413s[1] |
| Declination | −23° 57′ 45.5136″[1] |
| Apparent magnitude (V) | 4.81[2] |
| Characteristics | |
| Spectral type | B9.5IIIe[3] |
| U−B color index | –0.06[2] |
| B−V color index | +0.00[2] |
| Astrometry | |
| Radial velocity (Rv) | –12[4] km/s |
| Proper motion (μ) | RA: 5.24[1] mas/yr Dec.: -25.72[1] mas/yr |
| Parallax (π) | 8.04 ± 0.24[1] mas |
| Distance | 410 ± 10 ly (124 ± 4 pc) |
| Details | |
| Mass | ~4[5] M☉ |
| Luminosity | 3.12[6] L☉ |
| Temperature | 9,772[6] K |
| Metallicity [Fe/H] | –0.25[6] dex |
| Rotational velocity (v sin i) | 267 ± 5[7] km/s |
| Other designations | |
51 Ophiuchi (51 Oph) is a star located approximately 410 light years 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".[9] There is uncertainty about the stellar classification of this star. It has the nominal classification of B9.5IIIe, a B-type giant star with emission lines. However, it has also been classified as an A0 II-IIIe star and as a Herbig Ae/Be star.[5]
Dust and gas disk
51 Ophiuchi has a disk of dust and gas that appears to be a young debris disk and is probably 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.[9][10]
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.[11] 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.[10] 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.[9]
See also
References
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