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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 Gaia spacecraft show an annual shift of 23.15 mas. This is equivalent to a physical separation of around 141[1] light years from the Sun. It is drifting further away with a radial velocity of +47.8 km/s.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Vela |
| Right ascension | 10h 46m 15.116s[1] |
| Declination | –41° 27′ 51.73″[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: −48.135 mas/yr[1] Dec.: −54.551 mas/yr[1] |
| Parallax (π) | 23.1489 ± 0.018 mas[1] |
| Distance | 140.9 ± 0.1 ly (43.20 ± 0.03 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 | |
| Database references | |
| SIMBAD | data |
This is an ordinary G-type 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]
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.[8] A 2015 survey ruled out the existence of any additional stellar companions at projected distances from 12 to 352 astronomical units.[9]
This star hosts two close-orbiting, super-Earth-like planets, suspected since 2011 and confirmed in 2021.[10][11] 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.[12] A third planet on an innermost orbit was discovered in 2017[13] and confirmed in 2021.[11]
| 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 |
— | — |
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