| Extrasolar planet | List of extrasolar planets | |
|---|---|---|
| Parent star | ||
| Star | HD 50499 | |
| Constellation | Puppis | |
| Right ascension | (α) | 06h 52m 02s |
| Declination | (δ) | -33° 54′ 56″ |
| Apparent magnitude | (mV) | 7.221 |
| Distance | 154.14 ly (47.26 pc) |
|
| Spectral type | G1V | |
| Orbital elements | ||
| Semimajor axis | (a) | 3.84 ± 0.04 AU |
| Eccentricity | (e) | 0.25 ± 0.20 |
| Orbital period | (P) | 2458 ± 38 d |
| Argument of periastron |
(ω) | 259 ± 36° |
| Time of periastron | (T0) | 2451220 ± 77 JD |
| Semi-amplitude | (K) | 23.0 ± 1.1 m/s |
| Physical characteristics | ||
| Minimum mass | (m sin i) | 1.72 ± 0.03 MJ |
| Discovery information | ||
| Discovery date | 5 June 2005 | |
| Discoverer(s) | Vogt, Butler, Marcy, and Fischer et al. |
|
| Detection method | Radial velocity | |
| Discovery site | United States | |
| Discovery status | Confirmed | |
| Database references | ||
| Extrasolar Planets Encyclopaedia |
data | |
| SIMBAD | data | |
HD 50499 b is an extrasolar planet approximately 154 light-years away in the constellation of Puppis. The planet is suspected to be 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.
The planet was discovered by four team members including Steve 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.[1] He also indicated the existence of two additional outer planets.