| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Leo |
| Right ascension | 10h 10m 07.676s[1] |
| Declination | +18° 11′ 12.73″[1] |
| Apparent magnitude (V) | 8.01[2] |
| Characteristics | |
| Spectral type | G8V[3] |
| B−Vcolor index | 0.810±0.015[2] |
| Astrometry | |
| Radial velocity (Rv) | −3.62±0.14[4] km/s |
| Proper motion (μ) | RA: −11.135mas/yr[1] Dec.: −264.912mas/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 yellowstar with an orbitingexoplanet in theequatorialconstellation ofLeo. It has anapparent visual magnitude of 8.01,[2] which is too faint to be visible to the naked eye. With a smalltelescope it should be easily visible. The distance to this system, as measured throughparallax, is 240 light years, but it is slowly drifting closer with aradial velocity of −3.6 km/s.[4]
This is classified as an ordinaryG-type main-sequence star with astellar classification of G8V.[3] However, D. A. Fischer and associates in 2005 listed a class of G5 IV, suggesting it is instead asubgiant star that isevolving away from themain sequence having exhausted the hydrogen at itscore.[8] It is about 5 billion years old and is spinning with aprojected 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 itsphotosphere at aneffective temperature of 5,414 K.[4]
In 2004 a close orbiting exoplanet was found usingDoppler spectroscopy.[8] In 2016 the direct detection of the planetarythermal 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) | — | — |
