Mu Arae b: Difference between revisions
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| t_peri = 2452365.6 ± 12.6<ref name="pepe07" /> |
| t_peri = 2452365.6 ± 12.6<ref name="pepe07" /> |
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| semi-amp = 37.78 ± 0.40 |
| semi-amp = 37.78 ± 0.40 |
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| semimajor = |
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| semimajor_gigameter = |
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| periastron = |
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| periastron_gigameter = |
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| apastron = |
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| apastron_gigameter = |
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| period_year = 1.76 |
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| period_megasecond = |
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}} |
}} |
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{{Planetbox character |
{{Planetbox character |
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| mass = >1.676<ref name="pepe07" /> |
| mass = >1.676<ref name="pepe07" /> |
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| radius=1 |
| radius=1.045 |
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| density= |
| density= |
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| gravity=38 |
| gravity=38.0 |
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| temperature=240 |
| temperature=240 |
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| mass_earth =532.6328 |
| mass_earth =532.6328 |
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| gravity_earth =3 |
| gravity_earth =3.8834 |
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| insolation = |
| insolation = |
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| insolation_earth = |
| insolation_earth = |
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| radius_megameter = |
| radius_megameter = |
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| mass_wekagram = |
| mass_wekagram = |
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| radius_earth =11.6984948 |
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}} |
}} |
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{{Planetbox discovery |
{{Planetbox discovery |
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| names=HD 160691 b |
| names=HD 160691 b |
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}} |
}} |
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{{Planetbox reference |
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|- style="background-color: #A0B0FF;" colspan="3" |
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| star=HD+160691 |
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| '''Database references''' |
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| planet=b |
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|- bgcolor="#FFFAFA" |
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}} |
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| '''Exoplanet''' || [http://exoplanet.eu/planet.php?p1=HD+160691&p2=b data] |
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{{Planetbox end}} |
{{Planetbox end}} |
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Revision as of 23:26, 2 October 2008
Template:Planetbox begin Template:Planetbox star Template:Planetbox orbit Template:Planetbox character Template:Planetbox discovery Template:Planetbox catalog Template:Planetbox reference Template:Planetbox end
Mu Arae b (also referred to as HD 160691 b) is an extrasolar planet orbiting the star Mu Arae. At least one and a half times the mass of Jupiter. Its orbital period is 643.25 days. This planet's discovery was announced on December 12, 2002 and was originally thought to be on a highly eccentric orbit.[1] The latest models of the system which incorporate four planets give a lower eccentricity orbit.[2] While the planet itself is likely to be a gas giant with no solid surface, the orbital distance of 1.497 astronomical units from the star puts it within the liquid water habitable zone of the system. As a result, large satellites of the planet, if they exist, could potentially support life. However it may not receive enough ultraviolet light for abiogenesis to proceed.[3] Furthermore it is not clear that Earth-size moons can actually form in the environment around a gas giant planet.[4]
References
- ^ Butler, R. Paul; Tinney, C. G.; Marcy, Geoffrey W.; Jones, Hugh R. A.; Penny, Alan J.; Apps, Kevin (2001). "Two New Planets from the Anglo-Australian Planet Search". The Astrophysical Journal. 555 (1): 410–417. doi:10.1086/321467.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ^ Cite error: The named reference
pepe07was invoked but never defined (see the help page). - ^ Buccino, Andrea P.; Lemarchand, Guillermo A.; Mauas, Pablo J. D. (2006). "Ultraviolet Radiation Constraints around the Circumstellar Habitable Zones". Icarus. 183 (2): 491–503. doi:10.1016/j.icarus.2006.03.007.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ^ Canup, R., Ward, W. (2006). "A common mass scaling for satellite systems of gaseous planets". Nature. 441: 834–839.
{{cite journal}}: CS1 maint: multiple names: authors list (link)
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