Astronomy:HD 93385
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Vela[1] |
| Right ascension | 10h 46m 15.116s[2] |
| Declination | −41° 27′ 51.73″[2] |
| Apparent magnitude (V) | 7.486[3] |
| Characteristics | |
| Evolutionary stage | main sequence[2] |
| Spectral type | G2/G3 V[4] |
| B−V color index | 0.595[5] |
| Astrometry | |
| Radial velocity (Rv) | +47.80±0.61[6] km/s |
| Proper motion (μ) | RA: −48.135[2] mas/yr Dec.: −54.551[2] mas/yr |
| Parallax (π) | 23.1489 ± 0.018[2] mas |
| Distance | 140.9 ± 0.1 ly (43.20 ± 0.03 pc) |
| Absolute magnitude (MV) | +4.37[1] |
| Details | |
| Mass | 1.07[5] M☉ |
| Radius | 1.17[7] R☉ |
| Luminosity | 1.42[7] L☉ |
| Surface gravity (log g) | 4.08±0.11[7] cgs |
| Temperature | 5,823±35[7] K |
| Metallicity [Fe/H] | −0.05±0.03[7] dex |
| Age | 4.13[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 93385 is a star in the southern constellation of Vela. At an apparent visual magnitude of 7.5,[3] it is too faint to be seen with the unaided eye. Parallax measurements made using the Gaia spacecraft show an annual shift of 23.15 mas. This is equivalent to a physical separation of around 141[2] light years from the Sun. It is drifting further away with a radial velocity of +47.8 km/s.
This is an ordinary G-type main sequence star with a stellar classification of G2/G3 V.[4] The physical properties of HD 93385 are similar to those of the Sun; it is slightly larger with 107%[5] 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.[7] It is currently at an unusual low level of surface activity and thus is a candidate Maunder minimum analog.[5]
A physical companion star with an apparent visual magnitude of 12.29 is located at an angular separation of 10.32 arcseconds (equivalent to projected separation of 448 AU) along a position angle of 288°. It is estimated to have 45% of the mass of the Sun.[9] A 2015 survey ruled out the existence of any additional stellar companions at projected distances from 12 to 352 astronomical units.[10]
Planetary system
This star hosts two close-orbiting, super-Earth-like planets, suspected since 2011 and confirmed in 2021.[11][12] 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.[13] A third planet on an innermost orbit was discovered in 2017[14] and confirmed in 2021.[12]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥4.2±0.5 M⊕ | 0.0756±0.0013 | 7.3426±0.0012 | <0.295 | — | — |
| c | ≥7.1±0.6 M⊕ | 0.112±0.002 | 13.180±0.003 | <0.20 | — | — |
| d | ≥8.7±0.9 M⊕ | 0.2565±0.0043 | 45.85±0.05 | 0.09+0.15 −0.05 |
— | — |
References
- ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A XHIP record for this object at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 Høg, E. et al. (March 2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy and Astrophysics 355: L27–L30, doi:10.1888/0333750888/2862, Bibcode: 2000A&A...355L..27H.
- ↑ 4.0 4.1 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.
- ↑ 5.0 5.1 5.2 5.3 5.4 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, doi:10.1088/2041-8205/747/2/L32, Bibcode: 2012ApJ...747L..32L.
- ↑ 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, doi:10.1086/430500, Bibcode: 2005ApJS..159..141V.
- ↑ 7.0 7.1 7.2 7.3 7.4 7.5 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, doi:10.1088/0004-637X/720/2/1290, Bibcode: 2010ApJ...720.1290G.
- ↑ "HD 93385". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+93385.
- ↑ Tokovinin, Andrei (February 2011), "Low-mass Visual Companions to Nearby G-dwarfs", The Astronomical Journal 141 (2): 52, doi:10.1088/0004-6256/141/2/52, Bibcode: 2011AJ....141...52T.
- ↑ Mugrauer, M.; Ginski, C. (12 May 2015), "High-contrast imaging search for stellar and substellar companions of exoplanet host stars", Monthly Notices of the Royal Astronomical Society 450 (3): 3127–3136, doi:10.1093/mnras/stv771, Bibcode: 2015MNRAS.450.3127M, https://academic.oup.com/mnras/article/450/3/3127/1063872, retrieved 19 June 2020.
- ↑ 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, doi:10.1051/0004-6361/201220165, Bibcode: 2013A&A...552A...6G.
- ↑ 12.0 12.1 12.2 Unger, N. et al. (October 2021), "The HARPS search for southern extra-solar planets XLVI: 12 super-Earths around the solar type stars HD39194, HD93385, HD96700, HD154088, and HD189567", Astronomy & Astrophysics 654: 19, doi:10.1051/0004-6361/202141351, A104, Bibcode: 2021A&A...654A.104U
- ↑ Zolotukhin, Ivan (1995), Catalog, https://exoplanet.eu/catalog/?f=%27HD%2093385%27+in+name/, retrieved 2013-10-07.
- ↑ Gillon, M. et al. (May 2017), "The Spitzer search for the transits of HARPS low-mass planets - II. Null results for 19 planets", Astronomy & Astrophysics 601: 23, doi:10.1051/0004-6361/201629270, A117, Bibcode: 2017A&A...601A.117G
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