Talk:Methods of detecting exoplanets

Planet-star interactions

Although initial test were not successful, it may prove possible to detect star-planet interaction due to tidal effects or magnetic interactions from close-in (giant) planets.

Ref: S. H. Saar, M. Cuntz (2001). "A Search for Ca II Emission Enhancement in Stars resulting from Nearby Giant Planets". Monthly Notices of the Royal Astronomical Society. 325 (1): 55–59.

Fair use rationale for Image:GQLupi b.jpg

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BetacommandBot (talk) 17:29, 2 January 2008 (UTC)

"The phase function of the giant planet may be constrained, which will lead to constraints on the actual particle size distribution of its atmospheric particles."

I have only the vaguest idea of what this sentence means. Can anyone rephrase it in more generally comprehensible terms?24.69.167.26 (talk) 04:18, 5 September 2009 (UTC)

I rewrote most of that paragraph. Let me know if it makes sense as it is now. James McBride (talk) 02:07, 26 November 2009 (UTC)

Solar System Barycenter diagram

While reviewing this article, I noticed that the diagram "Motion of Barycenter of solar system relative to the Sun" was a relatively poor quality gif file, the source URL was to a PhotoBucket account that is now disabled, and it was for the years 1945-1996. Therefore I created two new diagrams and uploaded them to Wikimedia for you: 1) File:Solar System Barycenter 1944-1997.png is a complete recreation of the diagram in the article with the same years and path to verify validity of my algorithms, and 2) File:Solar System Barycenter 2000-2050.png which is a more "current" diagram for the years 2000-2050. Feel free to use one or both of these public domain png files if you want to replace the older diagram. Larry McNish, Calgary Centre of the Royal Astronomical Society of Canada. http://commons.wikimedia.org/wiki/File:Solar_System_Barycenter_2000-2050.png http://commons.wikimedia.org/wiki/File:Solar_System_Barycenter_1944-1997.png 68.144.133.105 (talk) 12:52, 8 January 2010 (UTC)