HD 202628
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Microscopium |
| Right ascension | 21h 18m 27.26879s[1] |
| Declination | −43° 20′ 04.7450″[1] |
| Apparent magnitude (V) | +6.75 |
| Characteristics | |
| Spectral type | G2V[2] |
| Astrometry | |
| Proper motion (μ) | RA: +240.89[1] mas/yr Dec.: +21.00[1] mas/yr |
| Parallax (π) | 40.95 ± 0.46[1] mas |
| Distance | 79.6 ± 0.9 ly (24.4 ± 0.3 pc) |
| Details | |
| Mass | 1.08[3] M☉ |
| Radius | 1.01[3] R☉ |
| Luminosity | 1.00[3] L☉ |
| Surface gravity (log g) | 4.50±0.02[4] cgs |
| Temperature | 5,833±11[4] K |
| Metallicity [Fe/H] | 0.002±0.009[4] dex |
| Rotational velocity (v sin i) | 2.64±0.11[4] km/s |
| Age | 600±450[4] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia | data |
HD 202628 is a G-type star in the constellation Microscopium with an elliptical (e=0.18) dust disc, inclined at 64°. The inner edge of the ring, which lies at around 158 AU from the star, is sharply defined.[2] This means that there is a likely planet responsible for this defined edge, and it has been calculated as orbiting between 86 and 158 AU from HD 202628.[5]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | > 1 M⊕ | 86-158[5] | — | ~ 0.2 | — | — |
| Disk | 150–220 AU | — | — | |||
References
- 1 2 3 4 5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752 [astro-ph], Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. Cite uses deprecated parameter
|class=(help) - 1 2 Krist, John E.; et al. (2012), "Hubble Space Telescope Observations of the HD 202628 Debris Disk", The Astronomical Journal, 144 (2): 9, arXiv:1206.2078 [astro-ph.SR], Bibcode:2012AJ....144...45K, doi:10.1088/0004-6256/144/2/45, 45. Cite uses deprecated parameter
|class=(help) - 1 2 3 Gáspár, András; Rieke, George H; Ballering, Nicholas (2016). "The Correlation between Metallicity and Debris Disk Mass". The Astrophysical Journal. 826 (2): 171. arXiv:1604.07403. Bibcode:2016ApJ...826..171G. doi:10.3847/0004-637X/826/2/171.
- 1 2 3 4 5 dos Santos, Leonardo A.; et al. (August 2016), "The Solar Twin Planet Search. IV. The Sun as a typical rotator and evidence for a new rotational braking law for Sun-like stars", Astronomy & Astrophysics, 592 (156): 8, arXiv:1606.06214 [astro-ph.SR], Bibcode:2016A&A...592A.156D, doi:10.1051/0004-6361/201628558, A156. Cite uses deprecated parameter
|class=(help) - 1 2 Nesvold, Erika R.; Kuchner, Marc J. (2015). "Gap Clearing by Planets in a Collisional Debris Disk". The Astrophysical Journal. 798 (2): 10. arXiv:1410.7784. Bibcode:2015ApJ...798...83N. doi:10.1088/0004-637X/798/2/83. 83.
This article is issued from
Wikipedia.
The text is licensed under Creative Commons - Attribution - Sharealike.
Additional terms may apply for the media files.