| 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) | 104.53±0.13[4] km/s |
| Proper motion (μ) | RA: 27.283±0.021[4] mas/yr Dec.: 112.918±0.024[4] mas/yr |
| Parallax (π) | 34.6094 ± 0.0239 mas[4] |
| Distance | 94.24 ± 0.07 ly (28.89 ± 0.02 pc) |
| Absolute magnitude (MV) | 5.25[2] |
| Details[5] | |
| 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[6] dex |
| Rotation | 30.7 d[7] |
| Rotational velocity (v sin i) | 0.421[6] 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.[9] 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[10][7] star with an estimated age of twelve billion years.[5] 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.[6] X-ray emission has not been detected, suggesting a low level of coronal activity.[11][12] The star is radiating 70% of the luminosity of the Sun from its photosphere at an effective temperature of 5,648 K.[5]
Planetary system
[edit]A superjovian planetary companion was detected by the CORALIE team, based on observations beginning in 2003.[7][12] Planets around such metal-poor stars are rare (the only two known similar cases as of 2019 are HD 22781 and HD 181720).[13] An astrometric measurement of the planet's inclination and true mass was published in 2022 as part of Gaia DR3.[14] Later in 2022, these parameters were revised along with the detection of a second substellar companion, likely a brown dwarf.[15]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 7.965+1.128 −0.479 MJ |
2.148+0.088 −0.097 |
3.201+0.002 −0.001 |
0.214+0.005 −0.003 |
93.521+16.622 −18.063° |
— |
| c | 18.063+4.209 −1.612 MJ |
17.250+2.158 −2.151 |
72.478+14.115 −12.341 |
0.558+0.027 −0.028 |
87.902+13.916 −22.591° |
— |
References
[edit]- ^ a b c 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 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 d 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 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. S2CID 119107228. A76.
- ^ 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.
- ^ "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.
- ^ 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, Bibcode:2019Geosc...9..105A, doi:10.3390/geosciences9030105, S2CID 119089419
- ^ Gaia Collaboration; et al. (2023). "Gaia Data Release 3". Astronomy & Astrophysics. 674: A34. arXiv:2206.05595. doi:10.1051/0004-6361/202243782. S2CID 249626026.
- ^ a b 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.
Well, that’s interesting to know that Psilotum nudum are known as whisk ferns. Psilotum nudum is the commoner species of the two. While the P. flaccidum is a rare species and is found in the tropical islands. Both the species are usually epiphytic in habit and grow upon tree ferns. These species may also be terrestrial and grow in humus or in the crevices of the rocks.
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