Upsilon Andromedae b
|Extrasolar planet||List of extrasolar planets|
|Star||Upsilon Andromedae A|
|Right ascension||(α)||01h 36m 47.8s|
|Declination||(δ)||+41° 24′ 20″|
|Distance||44.0 ± 0.1 ly
(13.49 ± 0.03 pc)
|Radius||(r)||1.480 ± 0.087 R☉|
|Temperature||(T)||6074 ± 13.1 K|
|Semimajor axis||(a)||0.0595 ± 0.0034 AU
|Periastron||(q)||0.0549 ± 0.0046 AU
|Apastron||(Q)||0.0609 ± 0.0046 AU
|Orbital period||(P)||4.62±0.23 d
|Time of periastron||(T0)||2,451,802.64 ± 0.71 JD|
|Semi-amplitude||(K)||69.8 ± 1.5 m/s|
|Minimum mass||(m sin i)||0.62 ± 0.09 MJ|
|Discovery date||June 23, 1996|
|Discoverer(s)||Marcy et al.|
|Discovery method||Radial velocity|
|Other detection methods||Reflection/emission modulations|
|Discovery site||California and Carnegie
Upsilon Andromedae b, occasionally referred to[by whom?] as Upsilon Andromedae Ab (to distinguish it from the red dwarf Upsilon Andromedae B), is an extrasolar planet approximately 44 light-years away from Earth in the constellation of Andromeda (the Chained Maiden). The planet was discovered orbiting the Solar twin star, Upsilon Andromedae, approximately every five days. Discovered in June 1996 by Geoffrey Marcy and R. Paul Butler, it was one of the first hot Jupiters to be discovered. It is also one of the first non-resolved planets to be detected directly. Upsilon Andromedae b is the innermost known planet in its planetary system.
Like the majority of known extrasolar planets, Upsilon Andromedae b was detected by the variations in its star's radial velocity caused by the planet's gravity. The variations were detected by making sensitive measurements of the Doppler shift of Upsilon Andromedae's spectrum. The planet was announced in January 1997, together with 55 Cancri b and the planet orbiting Tau Boötis.
Like 51 Pegasi b, the first extrasolar planet discovered around a normal star, Upsilon Andromedae b orbits very close to its star, closer than Mercury does to our Sun. The planet takes 4.617 days to complete an orbit, with a semimajor axis of 0.0595 AU.
A limitation of the radial velocity method used to detect Upsilon Andromedae b is that only a lower limit on the mass can be found. In the case of Upsilon Andromedae b, this lower limit is 68.7% of the mass of Jupiter, though depending on the inclination of the orbit, the true mass may be much greater. However, astronomers found recently that inclination of the orbital plane is around 25° and the true mass may be about 1.4 MJ. Coplanarity is not to be assumed; the mutual inclination between c and d is 35 degrees.
The Spitzer Space Telescope measured the planet temperature, and found that the difference between the two sides of Upsilon Andromedae b of about 1,400 degrees Celsius, ranging from minus 20 to 230 degrees to about 1,400 to 1,650 degrees Celsius. The temperature difference has led to speculation that Upsilon Andromedae b is tidal locked with the same side always facing Upsilon Andromedae A.
Sudarsky had, on the assumption that the planet is similar to Jupiter in composition and that its environment is close to chemical equilibrium, predicted Upsilon Andromedae b to have reflective clouds of silicates and iron in its upper atmosphere. The cloud deck instead absorbs the sun's radiation; between that and the hot, high pressure gas surrounding the mantle, exists a stratosphere of cooler gas. The outer shell of dark, opaque, hot cloud is assumed to consist of vanadium and titanium oxides ("pM planets"), but other compounds like tholins cannot be ruled out yet.
The planet (with 51 Pegasi b) was deemed a candidate for direct imaging by Planetpol. Preliminary results from polarimetric studies indicate that the planet has predominately blue color, is 1.36 times as large and 0.74 times as massive as Jupiter, meaning that the mean density is 0.36g/cm3. It has a geometric albedo of 0.35 in visible light.
Effect on its sun
Upsilon Andromedae b appears to be responsible for increased chromospheric activity on its parent star. Observations suggest that there is a "hot spot" on the star around 169° away from the sub-planetary point. This may be the result of interactions between the magnetic fields of the planet and the star. The mechanism may be similar to that responsible for the activity of RS Canum Venaticorum variable stars, or the interaction between Jupiter and its moon Io.
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