| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Vela |
| Right ascension | 10 46 15.116 |
| Declination | –41° 27′ 51.73″ |
| Apparent magnitude (V) | 7.486 |
| Characteristics | |
| Spectral type | G2/G3 V |
| B−V color index | 0.595 |
| Astrometry | |
| Radial velocity (Rv) | +47.80±0.61 km/s |
| Proper motion (μ) | RA: −48.135 mas/yr Dec.: −54.551 mas/yr |
| Parallax (π) | 23.1489 ± 0.018 mas |
| Distance | 140.9 ± 0.1 ly (43.20 ± 0.03 pc) |
| Details | |
| Mass | 1.07 M☉ |
| Radius | 1.17 R☉ |
| Luminosity | 1.42 L☉ |
| Surface gravity (log g) | 4.08±0.11 cgs |
| Temperature | 5,823±35 K |
| Metallicity | –0.05±0.03 dex |
| Age | 4.13 Gyr |
| Other designations | |
| CD–40 6283, HD 93385, HIP 52676, SAO 222310 | |
| Database references | |
| SIMBAD | data |
HD 93385 is a star in the southern constellation of Vela. At an apparent visual magnitude of 7.5, 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 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. The physical properties of HD 93385 are similar to those of the Sun; it is slightly larger with 107% 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. It is currently at an unusual low level of surface activity and thus is a candidate Maunder minimum analog.
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. A 2015 survey ruled out the existence of any additional stellar companions at projected distances from 12 to 352 astronomical units.
Planetary system
This star hosts two close-orbiting, super-Earth-like planets, suspected since 2011 and confirmed in 2021. 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. A third planet on an innermost orbit was discovered in 2017 and confirmed in 2021.
| 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
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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, S2CID 118565025.
- "HD 93385". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2013-10-07.
{{cite web}}: CS1 maint: postscript (link) - 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, S2CID 43663915.
- 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, Bibcode:2015MNRAS.450.3127M, doi:10.1093/mnras/stv771, hdl:1887/49340, 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, arXiv:1301.2109, Bibcode:2013A&A...552A...6G, doi:10.1051/0004-6361/201220165, S2CID 118410500.
- ^ 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, arXiv:2108.10198, Bibcode:2021A&A...654A.104U, doi:10.1051/0004-6361/202141351, A104
- Zolotukhin, Ivan (1995), "Catalog", Extrasolar Planets Encyclopaedia, 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, arXiv:1701.01303, Bibcode:2017A&A...601A.117G, doi:10.1051/0004-6361/201629270, A117
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