Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Cetus |
Right ascension | 01h 52m 50.534416s [1] |
Declination | −19° 30′ 25.108238″ [1] |
Apparent magnitude (V) | 7.51 [2] |
Characteristics | |
Spectral type | G0V [3] |
B−V color index | 0.607±0.015 [2] |
Astrometry | |
Radial velocity (Rv) | −7.53±0.13 [1] km/s |
Proper motion (μ) |
RA: 22.039±0.022
[1]
mas/
yr Dec.: −97.904±0.016 [1] mas/ yr |
Parallax (π) | 19.5342 ± 0.0221 mas [1] |
Distance | 167.0 ± 0.2
ly (51.19 ± 0.06 pc) |
Absolute magnitude (MV) | 3.94 [2] |
Details [4] | |
Mass | 1.12±0.02 M☉ |
Radius | 1.06±0.01 R☉ |
Luminosity | 1.17±0.01 L☉ |
Surface gravity (log g) | 4.43±0.02 cgs |
Temperature | 5,833±28 K |
Metallicity [Fe/H] | 0.29±0.03 [5] dex |
Rotational velocity (v sin i) | 5.01 [6] km/s |
Age | 1.6±0.9 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
HD 11506 is a star in the equatorial constellation of Cetus. It has a yellow hue and can be viewed with a small telescope but is too faint to be visible to the naked eye, having an apparent visual magnitude of 7.51. [2] The distance to this object is 167 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −7.5 km/s. [1] It has an absolute magnitude of 3.94. [2]
This object is an ordinary G-type main-sequence star with a stellar classification of G0V, [3] which indicates it is generating energy via hydrogen fusion at its core. It is around 1.6 [4] billion years old and is spinning with a projected rotational velocity of 5 km/s. [6] The star has 112% of the mass of the Sun and 106% of the Sun's radius. The spectrum shows a higher than solar abundance of elements other than hydrogen and helium – what astronomers term the metallicity. [5] The star is radiating 117% of the Sun's luminosity from its photosphere at an effective temperature of 5,833 K. [4]
The superjovian planet HD 11506 b was discovered orbiting the star by the N2K Consortium in 2007 using the doppler spectroscopy method. [3] In 2009, a second planet discovery was claimed based on Bayesian analysis of the original data. [8] However, in 2015 additional radial velocity measurements showed that the planetary parameters were significantly different than those determined by Bayesian analysis. An additional linear trend in the radial velocities indicates a stellar or planetary companion on a long term orbit. [5] In 2022, the presence of a third planet with an orbital period of 40 years was confirmed, and the mass and inclination of both planet b and the new planet d were measured via astrometry. [9]
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
c | ≥0.408±0.057 MJ | 0.774±0.038 | 223.41±0.32 | 0.193±0.038 | — | — |
b | 4.880+1.986 −0.333 MJ |
2.800+0.123 −0.136 |
1,613.7+4.3 −4.5 |
0.391±0.010 | 112.598+23.304 −52.700 ° |
— |
d | 7.383+2.015 −1.085 MJ |
12.235+1.571 −1.762 |
14,723.6+2,801.3 −2,735.0 |
0.061+0.028 −0.022 |
82.004+25.098 −21.421 ° |
— |