HD 93385
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Vela |
| Right ascension | 10h 46m 15.11587s[1] |
| Declination | –41° 27′ 51.7235″[1] |
| Apparent magnitude (V) | 7.486[2] |
| Characteristics | |
| Spectral type | G2/G3 V[3] |
| B−V color index | 0.595[4] |
| Astrometry | |
| Radial velocity (Rv) | +47.80 ± 0.61[5] km/s |
| Proper motion (μ) | RA: –48.11[1] mas/yr Dec.: –53.86[1] mas/yr |
| Parallax (π) | 23.70 ± 0.69[1] mas |
| Distance | 138 ± 4 ly (42 ± 1 pc) |
| Details | |
| Mass | 1.07[4] M☉ |
| Radius | 1.17[6] R☉ |
| Luminosity | 1.42[6] L☉ |
| Surface gravity (log g) | 4.08 ± 0.11[6] cgs |
| Temperature | 5,823 ± 35[6] K |
| Metallicity [Fe/H] | –0.05 ± 0.03[6] dex |
| Age | 4.13[4] Gyr |
| Other designations | |
HD 93385 is a star in the southern constellation of Vela. At an apparent visual magnitude of 7.5,[2] it is too faint to be seen with the unaided eye. Parallax measurements made using the Hipparcos satellite show an annual shift of 23.70 milli-arcseconds. This is equivalent to a physical separation of around 138[1] light years from the Sun.
This is an ordinary main sequence star with a stellar classification of G2/G3 V.[3] The physical properties of HD 93385 are similar to those of the Sun; it is slightly larger with 107%[4] of the Sun's mass, 117% of the radius, and 142% of the luminosity. The abundance of elements, other than hydrogen and helium, is nearly the same as in the Sun.[6] It is currently at an unusual low level of surface activity and thus is a candidate Maunder minimum analog.[4]
This star hosts two close-orbiting, super-Earth-like planets.[8] The first has 8.3 times the mass of the Earth and an orbital period of 13.186 days. The second is 10.1 times the Earth's mass with a period of 46.025 days.[9] A physical companion star with an apparent visual magnitude of 12.29 is located at an angular separation of 10.32 arcseconds along a position angle of 288°. It is estimated to have 45% of the mass of the Sun.[10]
References
- 1 2 3 4 5 6 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752
, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. - 1 2 Høg, E.; et al. (March 2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy and Astrophysics, 355: L27–L30, Bibcode:2000A&A...355L..27H, doi:10.1888/0333750888/2862.
- 1 2 Houk, Nancy (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, 1, Ann Arbor, Michigan: Department of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
- 1 2 3 4 5 Lubin, Dan; et al. (March 2012), "Frequency of Maunder Minimum Events in Solar-type Stars Inferred from Activity and Metallicity Observations", The Astrophysical Journal Letters, 747 (2): L32, Bibcode:2012ApJ...747L..32L, doi:10.1088/2041-8205/747/2/L32.
- ↑ Valenti, Jeff A.; Fischer, Debra A. (July 2005), "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs", The Astrophysical Journal Supplement Series, 159 (1): 141–166, Bibcode:2005ApJS..159..141V, doi:10.1086/430500.
- 1 2 3 4 5 6 Ghezzi, L.; et al. (September 2010), "Stellar Parameters and Metallicities of Stars Hosting Jovian and Neptunian Mass Planets: A Possible Dependence of Planetary Mass on Metallicity", The Astrophysical Journal, 720 (2): 1290–1302, arXiv:1007.2681, Bibcode:2010ApJ...720.1290G, doi:10.1088/0004-637X/720/2/1290.
- ↑ "HD 93385 -- Star", Strasbourg astronomical Data Center, Centre de Données astronomiques de Strasbourg, retrieved 2013-10-07.
- ↑ González Hernández, J. I.; et al. (April 2013), "Searching for the signatures of terrestrial planets in F-, G-type main-sequence stars", Astronomy & Astrophysics, 552: A6, arXiv:1301.2109, Bibcode:2013A&A...552A...6G, doi:10.1051/0004-6361/201220165.
- ↑ Zolotukhin, Ivan, "Catalog", The Extrasolar Planet Encyclopedia, retrieved 2013-10-07.
- ↑ Tokovinin, Andrei (February 2011), "Low-mass Visual Companions to Nearby G-dwarfs", The Astronomical Journal, 141 (2): 52, arXiv:1011.2051, Bibcode:2011AJ....141...52T, doi:10.1088/0004-6256/141/2/52.