HD 45350 b

Planetbox begin
name=HD 45350 bPlanetbox star
star = HD 45350
constell = Auriga
RA=RA|06|28|45.7103SIMBAD link|HD+45350|HD 45350 -- Star, database entry, SIMBAD, accessed on line September 22, 2008.]
DEC=DEC|+38|57|46.667
dist_ly=160 ± 8
dist_pc=49 ± 2
class=G5 IV [http://exoplanet.eu/star.php?st=HD+45350 Star : HD 45350] , entry, "Extrasolar Planets Encyclopaedia", accessed on line September 22, 2008.] Planetbox orbit
semimajor=1.92 ± 0.067Table 2, combined solution, Determination of the Orbit of the Planetary Companion to the Metal-Rich Star HD 45350, Michael Endl, William D. Cochran, Robert A. Wittenmyer, and Artie P. Hatzes, "Astronomical Journal" 131, #6 (June 2006), pp. 3131–3134, bibcode|2006AJ....131.3131E, doi|10.1086/503746.]
semimajor_gigameter = 287 ± 10
periastron = 0.43
periastron_gigameter = 64
apastron = 3.41
apastron_gigameter = 511
eccentricity=0.778 ± 0.009
period=963.6 ± 3.4
period_year = 2.64 ± 0.01
period_megasecond = 83.3 ± 0.3
speed =
long_peri = 343.4 ± 2.3
t_peri = 2,451,825.3 ± 7.1
semi-amp = 58.0 ± 1.7Planetbox character
mass=>1.79 ± 0.14
mass_earth = >569 ± 44
radius=
density=
gravity=
temperature=
gravity_earth =
insolation =
insolation_earth =
radius_megameter =
mass_wekagram =
radius_earth =Planetbox discovery
discovery_date=January 20, 2005
discovery_method=Radial velocity
discoverers=Marcy, Butler,
Vogt, et al.
discovery_site=Keck Observatory, Hawaii
flag|United States
discovery_status=Published [Five New Extrasolar Planets, Geoffrey W. Marcy, R. Paul Butler, Steven S. Vogt, et al., "Astrophysical Journal" 619, #1 (January 20, 2005), pp. 570–584, bibcode|2005ApJ...619..570M, doi|10.1086/426384.] Planetbox catalog
names = HIP 30860 bPlanetbox reference
star=HD+45350
planet=b

HD 45350 b is an extrasolar planet located approximately 160 light-years away in the constellation of Auriga. It has a minimum mass about 1.79 times that of Jupiter. The mean distance of the planet from the star is more than the distance between Mars and the Sun, but the eccentricity of the orbit is nothing short of remarkable; at periastron the planet is as close to the star as Mercury is from the Sun, but at apastron it is 8 times further. No doubt seasons on the planet would be extreme.

Dynamical simulations covering a period of 10⁷ years show that a second, low-mass, planet could only orbit stably if it were no more than 0.2 AU away from the star; in the simulations, these planets show oscillations in eccentricity up to an eccentricity of 0.25. Radial velocity observations rule out any such planet whose mass is greater than 4 Neptune masses. [Dynamical and Observational Constraints on Additional Planets in Highly Eccentric Planetary Systems, Robert A. Wittenmyer, Michael Endl, William D. Cochran, and Harold F. Levison, "Astronomical Journal" 134, #3 (September 2007), pp. 1276–1284, bibcode|2007AJ....134.1276W, doi|10.1086/520880.]

References

External links

*
*
*
*
* [http://media4.obspm.fr/exoplanets/base/planete.php?etoile=HD+45350&planete=b HD 45350b Simulation]