Misplaced Pages

List of exoplanets detected by microlensing: Difference between revisions

Article snapshot taken from Wikipedia with creative commons attribution-sharealike license. Give it a read and then ask your questions in the chat. We can research this topic together.
Browse history interactively← Previous editNext edit →Content deleted Content addedVisualWikitext
Revision as of 15:29, 2 February 2011 edit92.241.224.66 (talk)No edit summary← Previous edit Revision as of 20:18, 4 February 2011 edit undoMike s (talk | contribs)Extended confirmed users21,550 edits add reference section and referenceNext edit →
Line 13: Line 13:
! Year of discovery ! Year of discovery
|- |-
| ] || 0.01 || 0.62 || 2008 | ] <ref name="Bennett 2008"/> || 0.01 || 0.62 || 2008
|- |-
| ] || 0.88 || 0.83 || 2008 | ] || 0.88 || 0.83 || 2008
Line 35: Line 35:
| ] || 0.27 || 4.54 || 2008 | ] || 0.27 || 4.54 || 2008
|} |}

== References ==
{{reflist|
refs=
<ref name="Bennett 2008"> {{Cite Journal | title=A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192 | url=http://iopscience.iop.org/0004-637X/684/1/663/fulltext | journal=] | volume=684 | issue=1 | pages=663–683 | last=Bennett | first=D. P. | last2=Bond | first2=I. A. | last3=Udalski | first3=A. | last4=''et al.'' | year=2008 | doi=10.1086/589940 }}</ref>
}}


== External links == == External links ==

Revision as of 20:18, 4 February 2011

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

References

  1. Bennett, D. P.; Bond, I. A.; Udalski, A.; et al. (2008). "A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192". The Astrophysical Journal. 684 (1): 663–683. doi:10.1086/589940. {{cite journal}}: Explicit use of et al. in: |last4= (help)

External links


Exoplanets
Main topics
Sizes
and
types
Terrestrial
Gaseous
Other types
Formation
and
evolution
Systems
Host stars
Detection
Habitability
Catalogues
Lists
Other
Categories: