HD 108874
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Observation data Epoch 2000 |
|
---|---|
Constellation | Coma Berenices |
Right ascension | 12h 30m 26.8829s |
Declination | +22° 52' 47.383" |
Apparent magnitude (V) | 8.76 |
Distance | 223.4 ly (68.5 pc) |
Spectral type | G5 V |
Other designations | |
BD+23°2466,HIP 61028
|
HD 108874 is a yellow dwarf star (spectral type G5 V) in the constellation of Coma Berenices. It is 223 light years from Earth and has two extrasolar planets that are possibly in a 4:1 orbital resonance.
Contents |
[edit] Planets
[edit] HD 108874 b
Orbital elements | ||
---|---|---|
Semi-major axis | (a) | 1.051 ± 0.02 AU |
Eccentricity | (e) | 0.07 ± 0.04 |
Orbital period | (P) | 395.4 ± 2.5 d |
Inclination | (i) | ?° |
Longitude of periastron |
(ω) | 248.4 ± 36° |
Time of periastron | (τ) | 2,450,131.5 ± 60 JD |
Physical characteristics | ||
Mass | >1.36 ± 0.13 MJ | |
Radius | ? RJ | |
Density | ? kg/m³ | |
Temperature | ? K | |
Discovery | ||
Discovery date | 2003 | |
Detection method(s) | ||
Discoverer(s) | Butler, Marcy, Vogt, Fischer et al. |
HD 108874 b is a gas giant discovered in 2003 that orbits in the star's habitable zone. This means that its moons may have the potential to bear life provided their atmospheric conditions are right.
[edit] HD 108874 c
Orbital elements | ||
---|---|---|
Semi-major axis | (a) | 2.68 ± 0.25 AU |
Eccentricity | (e) | 0.25 ± 0.07 |
Orbital period | (P) | 1605.8 ± 88 d |
Inclination | (i) | ?° |
Longitude of periastron |
(ω) | 17.3 ± 23° |
Time of periastron | (τ) | 2,449,584.8 ± 180 JD |
Physical characteristics | ||
Mass | >1.018 ± 0.3 MJ | |
Radius | ? RJ | |
Density | ? kg/m³ | |
Temperature | ? K | |
Discovery | ||
Discovery date | 2005 | |
Detection method(s) | ||
Discoverer(s) | Vogt, Butler Marcy, Fischer et al. |
HD 108874 c is a gas giant discovered in 2005 which orbits beyond the star's habitable zone.
[edit] References
- Butler et al. (2003). "Seven New Keck Planets Orbiting G and K Dwarfs". The Astrophysical Journal 582: 455-466.
- Vogt et al. (2005). "Five New Multicomponent Planetary Systems". The Astrophysical Journal 632: 638 – 658.