HD 111031 (50 G. Corvi) is a double star in the southern constellation of Corvus. With an apparent visual magnitude of 6.87,[2] it is considered too faint to be readily visible to the naked eye. The distance to this star is 102 light years, but it is drifting closer to the Sun with a radial velocity of −20 km/s.[1] It has an absolute magnitude of 4.42.[2] The star has a relatively large proper motion, traversing the celestial sphere at an angular rate of 0.289 arcsec yr−1.[8]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Corvus |
| Right ascension | 12h 46m 30.84207s[1] |
| Declination | −11° 48′ 44.7902″[1] |
| Apparent magnitude (V) | 6.87[2] |
| Characteristics | |
| Spectral type | G5 V[3] |
| B−V color index | 0.695±0.001[2] |
| Astrometry | |
| Radial velocity (Rv) | −20.24±0.12[1] km/s |
| Proper motion (μ) | RA: −279.627(24) mas/yr[1] Dec.: 46.791(19) mas/yr[1] |
| Parallax (π) | 32.0310 ± 0.0219 mas[1] |
| Distance | 101.83 ± 0.07 ly (31.22 ± 0.02 pc) |
| Absolute magnitude (MV) | 4.42[2] |
| Orbit[4] | |
| Semi-major axis (a) | 21.1±0.6 AU |
| Eccentricity (e) | 0.71±0.01 |
| Inclination (i) | 137+4 −3° |
| Longitude of the node (Ω) | 325+2 −1° |
| Argument of periastron (ω) (secondary) | 42+3 −2° |
| Details[5] | |
| HD 111031 A | |
| Mass | 1.127+0.034 −0.041 M☉ |
| Radius | 1.274+0.024 −0.018 R☉ |
| Luminosity | 1.510+0.004 −0.003[6] L☉ |
| Surface gravity (log g) | 4.459±0.315 cgs |
| Temperature | 5,836±50 K |
| Metallicity [Fe/H] | 0.330±0.105 dex |
| Rotational velocity (v sin i) | 1.728±0.273 km/s |
| Age | 5.036+1.124 −1.092 Gyr |
| HD 111031 B | |
| Mass | 0.129±0.003[4] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
This object is a solar analog with a stellar classification of G5 V;[3] a G-type main-sequence star like the Sun that is generating energy through core hydrogen fusion. It is around five billion years old and is chromospherically inactive,[3] with a projected rotational velocity of 1.7 km/s. The star has 1.13 times the mass and 1.27 times the radius of the Sun. It is radiating 1.5 times the Sun's luminosity from its photosphere at an effective temperature of 5,836 K.[5]
In 2020, a stellar companion was identified using high-contrast imaging. The study authors deem this most likely a K-type main-sequence star with a class of K5V, an angular separation of 1″ along a position angle (PA) of 300° corresponding to a projected separation of 30 AU, and around 11–15% of the mass of the Sun.[9] An independent study published in 2021 identified a companion through speckle imaging. They propose this is a faint red dwarf with a class of M6 or later and a visual magnitude difference of 7.9 or more compared to the primary. It is located at a separation of 1.06″ along a PA of 121°, as of 2021.[10]
A 2022 study claimed the presence of a brown dwarf companion to this star based on radial velocity and astrometry observations,[11] but according to a 2023 follow-up study this was in fact a detection of the previously known stellar companion, poorly characterized due to the baseline of observations being much shorter than the companion's orbital period.[4]
References
edit- ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b c Gray, R. O.; et al. (2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I". The Astronomical Journal. 126 (4): 2048–2059. arXiv:astro-ph/0308182v1. Bibcode:2003AJ....126.2048G. doi:10.1086/378365. S2CID 119417105.
- ^ a b c Philipot, F.; Lagrange, A.-M.; et al. (August 2023). "Multi techniques approach to identify and/or constrain radial velocity sub-stellar companions". Astronomy & Astrophysics. arXiv:2308.05417. doi:10.1051/0004-6361/202346612. S2CID 260775968.
- ^ a b Soto, M. G.; Jenkins, J. S. (2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy and Astrophysics. 615: A76. arXiv:1801.09698. Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533. S2CID 119107228.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ "HD 111031". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-10-01.
- ^ Luyten, W. J. (June 1995), "NLTT Catalogue", VizieR On-line Data Catalog: I/98A. Originally published in: 1979nltt.book.....L, Bibcode:1995yCat.1098....0L
- ^ Gonzales, Erica J.; et al. (April 2020), "The TRENDS High-contrast Imaging Survey. VIII. Compendium of Benchmark Objects", The Astrophysical Journal, 893 (1): 27, arXiv:2010.11866, Bibcode:2020ApJ...893...27G, doi:10.3847/1538-4357/ab71fb, S2CID 216296289, 27
- ^ Dalba, Paul A.; et al. (March 2021). "Speckle Imaging Characterization of Radial Velocity Exoplanet Systems". The Astronomical Journal. 161 (3): 11. arXiv:2012.05253. Bibcode:2021AJ....161..123D. doi:10.3847/1538-3881/abd6ed. S2CID 228083864. 123.
- ^ Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21): 21. arXiv:2208.12720. Bibcode:2022ApJS..262...21F. doi:10.3847/1538-4365/ac7e57. S2CID 251864022.