HD 111031

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HD 111031
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Corvus
Right ascension 12h 46m 30.84223s[1]
Declination −11° 48′ 44.7890″[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)−20.19±0.15[1] km/s
Proper motion (μ) RA: −279.792[1] mas/yr
Dec.: 46.712[1] mas/yr
Parallax (π)32.0167 ± 0.0520[1] mas
Distance101.9 ± 0.2 ly
(31.23 ± 0.05 pc)
Absolute magnitude (MV)4.42[2]
Details[4]
Mass1.127+0.034
−0.041 M☉
Radius1.274+0.024
−0.018 R☉
Luminosity1.510+0.004
−0.003[1] L☉
Surface gravity (log g)4.459±0.315 cgs
Temperature5,836±50 K
Metallicity [Fe/H]0.330±0.105 dex
Rotational velocity (v sin i)1.728±0.273 km/s
Age5.036+1.124
−1.092 Gyr
Other designations
50 G. Corvi, BD−11° 3361, GJ 3746, HD 111031, HIP 62345, SAO 157502, LTT 4887[5]
Database references
SIMBADdata

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.[6]

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.[4]

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.[7] 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.[8]

References[]

  1. ^ a b c d e f g h 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.
  2. ^ 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.
  3. ^ 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.
  4. ^ 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.
  5. ^ "HD 111031". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-10-01.
  6. ^ Luyten, W. J. (June 1995). NLTT Catalogue. VizieR On-line Data Catalog: I/98A. Originally published in: 1979nltt.book.....L. Bibcode:1995yCat.1098....0L.
  7. ^ 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, 27
  8. ^ 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. 123.
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