10h10m07.68s, +18° 11′ 12.74″| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Leo |
| Right ascension | 10h10m 07.676s[1] |
| Declination | +18° 11′ 12.73″[1] |
| Apparent magnitude (V) | 8.01[2] |
| Characteristics | |
| Spectral type | G8V[3] |
| B−V color index | 0.810±0.015[2] |
| Astrometry | |
| Radial velocity (Rv) | −3.62±0.14[4] km/s |
| Proper motion (μ) | RA: −11.135 mas/yr[1] Dec.: −264.912 mas/yr[1] |
| Parallax (π) | 13.5882 ± 0.0249 mas[1] |
| Distance | 240.0 ± 0.4 ly (73.6 ± 0.1 pc) |
| Absolute magnitude (MV) | 3.50[5] |
| Details | |
| Mass | 1.23±0.16[6] M☉ |
| Radius | 2.01±0.04[6] R☉ |
| Luminosity | 3.14±0.02[4] L☉ |
| Surface gravity (log g) | 3.82[5] cgs |
| Temperature | 5,414±97[4] K |
| Metallicity [Fe/H] | 0.26[5] dex |
| Rotational velocity (v sin i) | 4.9[5] km/s |
| Age | 5.08[5] Gyr |
| Other designations | |
BD+18 2326, HD 88133, HIP 49813, SAO 98978, LTT 12725, NLTT 23562, TYC 1422-1130-1, 2MASS J10100767+1811132[7] | |
| Database references | |
| SIMBAD | data |
HD 88133 is a yellow star with an orbiting exoplanet in the equatorial constellationofLeo. It has an apparent visual magnitude of 8.01,[2] which is too faint to be visible to the naked eye. With a small telescope it should be easily visible. The distance to this system, as measured through parallax, is 240 light years, but it is slowly drifting closer with a radial velocity of −3.6 km/s.[4]
This is classified as an ordinary G-type main-sequence star with a stellar classification of G8V.[3] However, D. A. Fischer and associates in 2005 listed a class of G5 IV, suggesting it is instead a subgiant star that is evolving away from the main sequence having exhausted the hydrogen at its core.[8] It is about 5 billion years old and is spinning with a projected rotational velocity of 4.9 km/s.[5] The star has 23% more mass than the Sun and has double the Sun's girth.[6] It is radiating over three times the luminosity of the Sun from its photosphere at an effective temperature of 5,414 km/s.[4]
In 2004 a close orbiting exoplanet was found using Doppler spectroscopy.[8] In 2016 the direct detection of the planetary thermal emission spectrum was claimed,[9] but the detection was brought into questioned in 2021.[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥0.282±0.046 MJ | 0.0479±0.0032 | 3.414887±0.000045 | 0 (fixed) | — | — |
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