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This is the list of 11 extrasolar planets detected by microlensing, sorted by projected separations. To find planets using that method, the background star is temporarily magnified by a foreground star because of the gravity that bends light. If the foreground star has a planet, the light from background star would be slightly brighter than the star with no planet. Studying the brightness difference of background star between the foreground star with planets and foreground star with no planets, then mass can be estimated. The projected separation can be determined from how much the light bended.
The most massive planet detected by microlensing is OGLE-2005-BLG-071Lb, which masses 3.5 MJ; the least massive is MOA-2007-BLG-192Lb, which masses 0.010 MJ or 3.3 M⊕. The widest separation between a planet and a star is OGLE-2006-BLG-109Lc, which is 4.5 AU; the shortest separation is MOA-2007-BLG-192Lb, which is 0.62 AU.
There are 2 members of the multi-planet systems.
Yellow rows donate the members of the multi-planet system
Planet | Mass (MJ) | Projected separation (AU) | Year of discovery |
---|---|---|---|
MOA-2007-BLG-192Lb | 0.01 | 0.62 | 2008 |
MOA-2007-BLG-400Lb | 0.88 | 0.83 | 2008 |
MOA-2008-BLG-310Lb | 0.23 | 1.24 | 2009 |
MOA-2009-BLG-319Lb | 0.16 | 1.87 | 2010 |
OGLE-2006-BLG-109Lb | 0.73 | 2.31 | 2008 |
OGLE-2005-BLG-169Lb | 0.04 | 2.76 | 2006 |
OGLE-2005-BLG-390Lb | 0.02 | 2.76 | 2006 |
OGLE-2007-BLG-368Lb | 0.07 | 3.14 | 2009 |
OGLE-2005-BLG-071Lb | 3.46 | 3.53 | 2005 |
OGLE-2003-BLG-235Lb | 2.64 | 4.31 | 2004 |
OGLE-2006-BLG-109Lc | 0.27 | 4.54 | 2008 |
External links
- "Candidates detected by microlensing". The Extrasolar Planets Encyclopaedia. Retrieved 2011-01-20.
- "Exoplanets Data Explorer". Retrieved 2011-01-20.