| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Musca |
| Right ascension | 12h 57m 31.95991s[1] |
| Declination | −65° 38′ 47.2594″[1] |
| Apparent magnitude (V) | 6.86[2] |
| Characteristics | |
| Evolutionary stage | red giant branch |
| Spectral type | G8III[3] |
| B−V color index | 1.018±0.008[2] |
| Astrometry | |
| Radial velocity (Rv) | 72.82±0.15[1] km/s |
| Proper motion (μ) | RA: −65.486±0.043[1] mas/yr Dec.: +31.269±0.038[1] mas/yr |
| Parallax (π) | 6.3628 ± 0.0284 mas[1] |
| Distance | 513 ± 2 ly (157.2 ± 0.7 pc) |
| Absolute magnitude (MV) | 1.22[2] |
| Details[4] | |
| Mass | 1.21±0.25[4] 1.54±0.05[5] 2.32±0.23[6] M☉ |
| Radius | 10.28+0.11 −0.17[1] R☉ |
| Luminosity | 50.5±0.4[1] L☉ |
| Surface gravity (log g) | 2.49±0.06 cgs |
| Temperature | 4,793±22 K |
| Metallicity [Fe/H] | −0.28±0.05 dex |
| Rotational velocity (v sin i) | 3.29±0.47 km/s |
| Age | 4.17±2.34 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 112410 is a star in the southern constellation of Musca. It has a yellow hue and is too dim to be readily visible to the average sight, having an apparent visual magnitude of 6.86.[2] The distance to this star is 513 light years based on parallax, and it is drifting further away from the Sun with a radial velocity of 73 km/s.[1] It has an absolute magnitude of 1.22.[2]
This is an aging giant star with a stellar classification of G8III.[3] It is cooling and expanding along the red giant branch,[5] having evolved off the main sequence after exhausting its core supply of hydrogen fuel. At present it has 10[1] times the Sun's radius. Mass estimates range from 1.21[4] up to 2.32[6] times the mass of the Sun. The star has a lower metallicity the Sun – what astronomers term the abundance of elements with more mass than helium – and it is spinning with a projected rotational velocity of 3.3 km/s.[4] It is radiating 50.5[1] times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,793 K.[4]
Planetary system
[edit]HD 112410 has a substellar companion calculated to have a mass at least 9.2 times that of Jupiter and an orbital period of 124.6 days at a typical separation of approximately 0.57 astronomical units (AU). As of 2013, this is the nearest exoplanet orbiting around any ascending red giant branch star, and second-closest planet to a giant star after the companion of HIP 13044.[5]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| HD 112410 b | >9.18 MJ | 0.565 | 124.6 | 0.23 | — | — |
References
[edit]- ^ a b c d e f g h i j k 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 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 Houk, Nancy (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 1. Ann Arbor, Michigan: Department of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
- ^ a b c d e Jofré, E.; et al. (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy & Astrophysics. 574: A50. arXiv:1410.6422. Bibcode:2015A&A...574A..50J. doi:10.1051/0004-6361/201424474. S2CID 53666931.
- ^ a b c Jones, M. I.; et al. (2013). "Study of the Impact of the Post-MS evolution of the Host Star on the Orbits of Close-in Planets. II. A Giant Planet in a Close-in Orbit around the RGB Star HIP 63242". Astronomy & Astrophysics. 556 (A78): 5. arXiv:1306.3939. Bibcode:2013A&A...556A..78J. doi:10.1051/0004-6361/201321660. S2CID 118618692.
- ^ a b Sousa, S. G.; et al. (November 2018). "SWEET-Cat updated. New homogenous spectroscopic parameters". Astronomy & Astrophysics. 620: 13. arXiv:1810.08108. Bibcode:2018A&A...620A..58S. doi:10.1051/0004-6361/201833350. S2CID 119374557. A58.
- ^ "HD 112410". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-08-04.
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.
View the detailed Guide of Psilotum nudum: Detailed Study Of Psilotum Nudum (Whisk Fern), Classification, Anatomy, Reproduction