HD 136118
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| Observation data Epoch J2000.0 |
|
|---|---|
| Constellation (pronunciation) |
Serpens |
| Right ascension | 15h 18m 55.5s |
| Declination | -1º 35' 32.6 |
| Apparent magnitude (V) | +6.94 |
| Distance | 171 ly (52.3 pc) |
| Spectral type | F9V |
| Other designations | |
|
BD-01° 3045, GC 20583, HIP 74948, SAO 140452.
|
|
HD 136118 is a star located in the constellation Serpens Cauda. It is an F-type dwarf and magnitude 7. The distance from Earth is 52.3 parsecs.
The astronomer Debra Fischer discovers a very massive planet, which was announced to other astronomers on February 7, 2002.
[edit] HD 136118 b
| Extrasolar planet | List of extrasolar planets | |
|---|---|---|
| Orbital elements | ||
| Semimajor axis | (a) | 2.3 AU |
| Eccentricity | (e) | 0.37 ± 0.025 |
| Orbital period | (P) | 1209 ± 24 d |
| Angular distance | (θ) | 44 mas |
| Longitude of periastron |
(ω) | 315 ± 4.5° |
| Time of periastron | (T0) | 2451800.6 ± 36.6 JD |
| Semi-amplitude | (K) | 212.8 ± 5.8 m/s |
| Physical characteristics | ||
| Mass | (m) | >11.9 MJ |
| Discovery information | ||
| Discovery date | February 7, 2002 | |
| Discoverer(s) | Fischer et al. | |
| Detection method | Doppler Spectroscopy | |
| Discovery status | Published | |
HD 136118 b is a massive extrasolar planet, having mass of 11.9 times that of Jupiter. The lower limit on its mass is only slightly less than the deuterium-burning threshold that some astronomers use to distinguish between planets and brown dwarfs. Depending on the inclination of its orbit, the true mass could be above this limit.
The orbit of the planet is located at the average distance of 2.3 astronomical units from the parent star, taking 40 months to complete one eccentric orbit.
Due to its high mass the planet is likely to be very hot and possibly glowing faintly.
[edit] References
- Fischer et al. (2002). "Planetary Companions to HD 136118, HD 50554, and HD 106252". Publications of the Astronomical Society of the Pacific 114: 529 – 535. doi:.
- Butler et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal 646 (1): 505 – 522. doi:. (web Preprint)

