05h40m01.7296s, +06° 03′ 38.085″| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Orion |
| Right ascension | 05h40m 01.7283s[1] |
| Declination | +06° 03′ 38.073″[1] |
| Apparent magnitude (V) | 8.67[2] |
| Characteristics | |
| Spectral type | K0 V[3] |
| B−V color index | 0.827±0.005[2] |
| Astrometry | |
| Radial velocity (Rv) | −22.08±0.15[1] km/s |
| Proper motion (μ) | RA: 52.246(26) mas/yr[1] Dec.: −247.136(17) mas/yr[1] |
| Parallax (π) | 21.4364 ± 0.0224 mas[1] |
| Distance | 152.2 ± 0.2 ly (46.65 ± 0.05 pc) |
| Absolute magnitude (MV) | 5.46[2] |
| Details[4] | |
| Mass | 0.98±0.01 M☉ |
| Radius | 0.89±0.01 R☉ |
| Luminosity | 0.602±0.002 L☉ |
| Surface gravity (log g) | 4.52±0.01 cgs |
| Temperature | 5,380±13 K |
| Metallicity [Fe/H] | 0.25±0.04[5] dex |
| Rotation | 57.67[3] days |
| Rotational velocity (v sin i) | 4.5[6] km/s |
| Age | 1.8±1.0 or 7[3] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 37605 is a star in the equatorial constellationofOrion. It is orange in hue but is too faint to be visible to the naked eye, having an apparent visual magnitude of 8.67.[2] Parallax measurements yield a distance estimate of 152 light years from the Sun. It has a high proper motion[3] and is drifting closer with a radial velocity of −22 km/s.[1]
This object is a K-type main-sequence star with a stellar classification of K0 V.[3] It is an inactive, metal-rich star. Age estimates range from 1.8[4] up to 7[3] billion years old, and it is spinning with a projected rotational velocity of 4.5 km/s.[6] The star has 98% of the mass of the Sun and 89% of the Sun's radius. It is radiating 60% of the luminosity of the Sun from its photosphere at an effective temperature of 5,380 K.[4]
There are two giant planets known in orbit. Planet b was discovered in 2004[8] and planet c was discovered eight years later. The planets do not transit relative to Earth; b's maximum inclination is 88.1%.[3][9]
In a simulation, HD 37605 b's orbit "sweeps clean" most test particles within 0.5 AU; leaving only asteroids『in low-eccentricity orbits near the known planet’s apastron distance, near the 1:2 mean-motion resonance』with oscillating eccentricity up to 0.06, and also at 1:3 with oscillating eccentricity up to 0.4. Also, observation has ruled out planets heavier than 0.7 Jupiter mass with a period of one year or less; which still allows for planets at 0.8 AU or more.[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥2.69±0.3 MJ | 0.277±0.015 | 55.01292±0.00062 | 0.6745±0.0019 | — | — |
| c | ≥3.19±0.38 MJ | 3.74±0.21 | 2720±15 | 0.03±0.012 | — | — |
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