HD 23596b and HD 23596 b: Difference between pages
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| names = HIP 17747 b, SAO 39910 b |
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'''HD |
'''HD 23596 b''' is an [[exoplanet]] approximately 170 [[light year]]s away in the [[constellation]] [[Perseus (constellation)|Perseus]]. The planet is very massive, at least 7.8 times that of [[Jupiter]], classifying as mid-[[Planetary mass type#Type I – Superjovian|superjovian]]. Based on its mass, the planet would probably be a [[gas giant]] with no solid surface but with gaseous ocean. The planet orbits at the average distance of 2.83 AU, taking 1565 days to complete its orbit with average velocity of 19.7 km/s. The eccentricity of the planet’s orbit is higher than all the planets in our [[solar system]], bringing as close as 2.00 AU to as far as 3.66 AU from the parent star. Combining with very massive planet (7.8 M<sub>J</sub>) and wide separation (2.83 AU) will yield high semi-[[amplitude]] of 124 m/s. |
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The planet was discovered by Perrier et al. in 2002 using his [[Methods of detecting extrasolar planets#Radial velocity|radial velocity technique]] to look for changes in toward (blue-shifting) and away (red-shifting) stellar motion in the sky <nowiki>[</nowiki>[[radial velocity]]<nowiki>]</nowiki>. |
The planet was discovered by Perrier et al. in 2002 using his [[Methods of detecting extrasolar planets#Radial velocity|radial velocity technique]] to look for changes in toward (blue-shifting) and away (red-shifting) stellar motion in the sky <nowiki>[</nowiki>[[radial velocity]]<nowiki>]</nowiki>. |
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Revision as of 19:07, 12 July 2008
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HD 23596 b is an exoplanet approximately 170 light years away in the constellation Perseus. The planet is very massive, at least 7.8 times that of Jupiter, classifying as mid-superjovian. Based on its mass, the planet would probably be a gas giant with no solid surface but with gaseous ocean. The planet orbits at the average distance of 2.83 AU, taking 1565 days to complete its orbit with average velocity of 19.7 km/s. The eccentricity of the planet’s orbit is higher than all the planets in our solar system, bringing as close as 2.00 AU to as far as 3.66 AU from the parent star. Combining with very massive planet (7.8 MJ) and wide separation (2.83 AU) will yield high semi-amplitude of 124 m/s.
The planet was discovered by Perrier et al. in 2002 using his radial velocity technique to look for changes in toward (blue-shifting) and away (red-shifting) stellar motion in the sky [radial velocity].
References
- Perrier, C.; Sivan, J.-P.; Naef, D.; Beuzit, J. L.; Mayor, M.; Queloz, D.; Udry, S. (2003). "The ELODIE survey for northern extra-solar planets. I. Six new extra-solar planet candidates". Astronomy & Astrophysics. 410: 1039–1049. doi:10.1051/0004-6361:20031340. Retrieved 2007-09-22.
{{cite journal}}: CS1 maint: multiple names: authors list (link)
External links
- "Notes for planet HD 23596b". The Extrasolar Planet Encyclopaedia.
- "HD 23596 B – Water Cloud Jovian, Eccentric". Extrasolar Visions.
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