HD 23596
From Wikipedia, the free encyclopedia
| Observation data Epoch J2000.0 |
|
|---|---|
| Constellation (pronunciation) |
Perseus |
| Right ascension | 03h 48m 00.37s |
| Declination | +40° 31′ 50.29″ |
| Apparent magnitude (V) | +7.24 |
| Absolute magnitude (V) | +3.66 |
| Distance | 170 ly (52 pc) |
| Spectral type | F8 |
| Other designations | |
HD 23596 is a star in the constellation Perseus. It is the 7th magnitude star located 170 light years away. The visual luminosity of the star is 1.71 times greater than our Sun. HD 23596 dwarfs the Sun is terms of physical properties; including mass, radius, age, metallicity, and temperature. The spectrum of the star is F8.
The star is unusual as it have one known detected planet.
[edit] HD 23596 b
| Extrasolar planet | List of extrasolar planets | |
|---|---|---|
| Orbital elements | ||
| Semimajor axis | (a) | 2.83 AU |
| Eccentricity | (e) | 0.292±0.023 |
| Orbital period | (P) | 1565±21 d |
| Angular distance | (θ) | 54.423 mas |
| Longitude of periastron |
(ω) | 274.1±3.9° |
| Time of periastron | (T0) | 2,451,604±15 JD |
| Semi-amplitude | (K) | 124.0±3.0 m/s |
| Physical characteristics | ||
| Mass | (m) | >7.80±0.35 MJ |
| Discovery information | ||
| Discovery date | June 2002 | |
| Discoverer(s) | Perrier et al. | |
| Detection method | radial velocity | |
| Discovery status | Published | |
HD 23596 b is an exoplanet orbiting the star HD 23596. The planet is very massive, at least 7.8 times that of Jupiter, classifying as mid-superjovian. Based on its mass, the planet would probably be a gas giant with no solid surface but with gaseous ocean. The planet orbits at the average distance of 2.83 AU, taking 1565 days to complete its orbit with average velocity of 19.7 km/s. The eccentricity of the planet’s orbit is higher than all the planets in our solar system, bringing as close as 2.00 AU to as far as 3.66 AU from the parent star. Combining with very massive planet (7.8 MJ) and wide separation (2.83 AU) will yield high semi-amplitude of 124 m/s.
The planet was discovered by Perrier et al. in 2002 using his radial velocity technique to look for changes in toward (blue-shifting) and away (red-shifting) stellar motion in the sky [radial velocity].
[edit] References
- Perrier, C.; Sivan, J.-P.; Naef, D.; Beuzit, J. L.; Mayor, M.; Queloz, D.; Udry, S. (2003). "The ELODIE survey for northern extra-solar planets. I. Six new extra-solar planet candidates". Astronomy & Astrophysics 410: 1039–1049. doi:.
