HD 50499
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Puppis |
| Right ascension | 06h 52m 02.024s[1] |
| Declination | −33° 54′ 56.01″[1] |
| Apparent magnitude (V) | 7.221 |
| Characteristics | |
| Spectral type | G1V |
| Astrometry | |
| Proper motion (μ) | RA: −68.95 ± 0.41[1] mas/yr Dec.: 68.96 ± 0.47[1] mas/yr |
| Parallax (π) | 21.68 ± 0.49 mas[1] |
| Distance | 150 ± 3 ly (46 ± 1 pc) |
| Details | |
| Mass | 1.25 ± 0.01[2] M☉ |
| Radius | 1.35 ± 0.03[2] R☉ |
| Luminosity | 2.25 ± 0.02[2] L☉ |
| Surface gravity (log g) | 4.27 ± 0.03[2] cgs |
| Temperature | 6102 ± 54[2] K |
| Age | 2.7 ± 0.6[2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 50499 is a yellow dwarf star approximately 154 light-years away in the constellation of constellation of Puppis. It is suspected that the star is hotter, larger, and more massive than the Sun. The magnitude is 7, this star is too faint to be in naked eye visibility. As of 2005, at least one extrasolar planet has been confirmed to be orbiting the star.
Planetary system
The first planet discovered, HD 50499 b, is a gas giant with mass of 1.7 times Jupiter. It is a long period, taking 351 weeks to orbit the star. The planet’s eccentric orbit passes through the average distance of 574 Gm or 18.6 μpc.
The planet was discovered by four team members including Steven Vogt in 2005 using their radial velocity method, which used to measure changes in red- and blue-shifting of the star that indicate the presence of planets caused by gravitational tug.[3] There is also a linear trend in the radial velocities, which may indicate an additional outer planet. The best two-planet model gives a different period and mass for the inner planet (9.8 years and 3.4 Jupiter masses), with an outer planet of 2.1 Jupiter masses in a 37-year orbit. However the two-planet model does not represent a significant improvement over the model with one planet and a linear trend, so more observations are needed to constrain the parameters of the outer planet.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >1.72 ± 0.03 MJ | 3.84 ± 0.04 | 2458 ± 38 | 0.25 ± 0.20 | — | — |
| c (unconfirmed) | >2 MJ | >4 | >3100 | — | — | — |
See also
References
- ^ a b c d e van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
- ^ a b c d e f Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951.
- ^ Vogt, Steven S.; et al. (2005). "Five New Multicomponent Planetary Systems". The Astrophysical Journal. 632 (1): 638–658. Bibcode:2005ApJ...632..638V. doi:10.1086/432901.
External links
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