HD 111232
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Musca |
| Right ascension | 12h 48m 51.75258s[1] |
| Declination | −68° 25′ 30.5471″[1] |
| Apparent magnitude (V) | 7.59[2] |
| Characteristics | |
| Spectral type | G8 V Fe-1.0[3] |
| B−V color index | 0.701±0.003[2] |
| Astrometry | |
| Radial velocity (Rv) | +104.1±0.2[2] km/s |
| Proper motion (μ) | RA: +27.287±0.054[1] mas/yr Dec.: +112.419±0.054[1] mas/yr |
| Parallax (π) | 34.5049 ± 0.0428 mas[1] |
| Distance | 94.5 ± 0.1 ly (28.98 ± 0.04 pc) |
| Absolute magnitude (MV) | 5.25[2] |
| Details[4] | |
| Mass | 0.80±0.02 M☉ |
| Radius | 0.88±0.01 R☉ |
| Luminosity | 0.700±0.003 L☉ |
| Surface gravity (log g) | 4.45±0.02 cgs |
| Temperature | 5,648±30 K |
| Metallicity [Fe/H] | −0.32[5] dex |
| Rotational velocity (v sin i) | 0.421[5] km/s |
| Age | 11.7±1.4 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 111232 is a star in the southern constellation of Musca. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 7.59.[2] The distance to this star is 94.5 light years based on parallax.[1] It is drifting away from the Sun with a radial velocity of +104 km/s,[2] having come to within 14.1 light-years some 264,700 years ago.[7] The absolute magnitude of this star is 5.25,[2] indicating it would have been visible to the naked eye at that time.
This is an ancient, thick disk population II[8][9] star with an estimated age of twelve billion years.[4] It is a G-type main-sequence star with a stellar classification of G8 V Fe-1.0,[3] indicating an anomalous underabundance of iron in the stellar atmosphere. The star has 80% of the mass of the Sun and 88% of the Sun's radius. It is spinning slowly with a projected rotational velocity of 0.4 km/s.[5] X-ray emission has not been detected, suggesting a low level of coronal activity.[10][11] The star is radiating 70% of the luminosity of the Sun from its photosphere at an effective temperature of 5,648 K.[4]
Planetary system
A superjovian planetary companion was detected by the CORALIE team, based on observations beginning in 2003.[9][11] The planets around such metal-poor stars are rare (only three known similar cases are HD 22781, HD 114762, and Sika).[12]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >6.80 MJ | 1.97 | 1,143±14 | 0.20±0.01 | — | — |
References
- ^ a b c d e f 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.
- ^ a b c d e f g 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 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. arXiv:astro-ph/0308182. Bibcode:2003AJ....126.2048G. doi:10.1086/378365. S2CID 119417105.
- ^ a b c Bonfanti, A.; Ortolani, S.; Piotto, G.; Nascimbeni, V. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575: A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID 54555839.
- ^ a b c Soto, M. G.; Jenkins, J. S. (July 2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy & Astrophysics. 615: 28. arXiv:1801.09698. Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533. A76.
- ^ "HD 111232". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-13.
- ^ Bailer-Jones, C.A.L.; Rybizki, J; Andrae, R.; Fouesnea, M. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics. 616: A37. arXiv:1805.07581. Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456. S2CID 56269929.
- ^ Fuhrmann, Klaus; Chini, Rolf (January 2019). "On ancient solar-type stars". Monthly Notices of the Royal Astronomical Society. 482 (1): 471–489. Bibcode:2019MNRAS.482..471F. doi:10.1093/mnras/sty2660.
- ^ a b c Mayor, M.; et al. (2004). "The CORALIE survey for southern extra-solar planets XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE". Astronomy and Astrophysics. 415 (1): 391–402. arXiv:astro-ph/0310316. Bibcode:2004A&A...415..391M. doi:10.1051/0004-6361:20034250. S2CID 5233877.
- ^ Poppenhaeger, K.; et al. (June 2010). "Coronal properties of planet-bearing stars". Astronomy and Astrophysics. 515: 9. arXiv:1003.5802. Bibcode:2010A&A...515A..98P. doi:10.1051/0004-6361/201014245. S2CID 119260432. A98.
- ^ a b Minniti, Dante; et al. (March 2009). "Low-Mass Companions for Five Solar-Type Stars From the Magellan Planet Search Program". The Astrophysical Journal. 693 (2): 1424–1430. arXiv:0810.5348. Bibcode:2009ApJ...693.1424M. doi:10.1088/0004-637X/693/2/1424. S2CID 119224845.
- ^ Adibekyan, Vardan (2019), "HEAVY METAL RULES. I. EXOPLANET INCIDENCE AND METALLICITY", Geosciences, 9 (3): 105, arXiv:1902.04493, doi:10.3390/geosciences9030105, S2CID 119089419
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