HD 28185 b
|Extrasolar planet||List of extrasolar planets|
|Right ascension||(α)||04h 26m 26.323s|
|Declination||(δ)||–10° 33′ 02.93″|
|Distance||138 ± 5 ly
(42 ± 2 pc)
|Mass||(m)||0.99 ± 0.07 M☉|
|Semimajor axis||(a)||1.031 ± 0.060 AU
|Eccentricity||(e)||0.070 ± 0.040|
|Orbital period||(P)||383.0 ± 2.0 d
|Orbital speed||(υ)||29.37 km/s|
|(ω)||351 ± 25°|
|Time of periastron||(T0)||2,451,863 ± 26 JD|
|Semi-amplitude||(K)||161 ± 11 m/s|
|Minimum mass||(m sin i)||5.72 ± 0.93 MJ|
|Discovery date||April 4, 2001|
|Discoverer(s)||Santos et al.|
|Discovery method||Radial velocity (CORALIE)|
|Discovery site||Chile La Silla Observatory|
HD 28185 b is an extrasolar planet approximately 138 light-years away from Earth in the constellation of Eridanus. The planet was discovered orbiting the Sun-like star HD 28185 in April 2001 as a part of the CORALIE survey for southern extrasolar planets, and its existence was independently confirmed by the Magellan Planet Search Survey in 2008. HD 28185 b orbits its sun in a circular orbit that is at the inner edge of its star's habitable zone.
Like the majority of known extrasolar planets, HD 28185 b was discovered by detecting small periodic variations in the radial velocity of its parent star caused by the gravitational attraction of the planet. This was achieved by measuring the Doppler shift of the star's spectrum. In 2001 it was announced that HD 28185 exhibited a wobble along the line-of-sight with a period of 383 days, with an amplitude indicating a minimum mass 5.72 times that of Jupiter.
Orbit and mass
HD 28185 b takes 1.04 years to orbit its parent star. Unlike most known long-period planets, the orbit of HD 28185 b has a low eccentricity, comparable to that of Mars in our solar system. The orbit lies entirely within its star's habitable zone.
The amplitude of the radial velocity oscillations means that the planet has a mass at least 5.7 times that of Jupiter in our solar system. However, the radial velocity method only yields a minimum value on the planet's mass, depending on the orbital inclination to our line-of-sight. Therefore, the true mass of the planet may be much greater than this lower limit.
Given the planet's high mass, it is most likely to be a gas giant with no solid surface. Since the planet has only been detected indirectly through observations of the star, properties such as its radius, composition, and temperature are unknown.
Since HD 28185 b orbits in its star's habitable zone, some have speculated on the possibility of life on worlds in the HD 28185 system. While it is unknown whether gas giants can support life, simulations of tidal interactions suggest that HD 28185 b could harbor Earth-mass satellites in orbit around it for many billions of years. Such moons, if they exist, may be able to provide a habitable environment, though it is unclear whether such satellites would form in the first place. Additionally, a small planet in one of the gas giant's Trojan points could survive in a habitable orbit for long periods. The high mass of HD 28185 b, of over six Jupiter masses, actually makes either of these scenarios more likely than if the planet was about Jupiter's mass or less.
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