By Y. Ryabov, G. Yankovsky
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Additional info for An Elementary Survey of Celestial Mechanics
10. The limit of detectability of existing measurements is shown, together with the expected improvement due to ever increasing sensitivity and longer observation runs. g. , 2003), the California and Carnegie Planet Search, 1 Detection Methods and Properties of Known Exoplanets 13 Fig. 10. Selection eﬀects of diﬀerent exoplanet detection programmes. Solar System planets are indicated by letter. , 2004). Analysis methods are rapidly becoming more sophisticated and Charbonneau (2006) note that the radial velocity method may soon start turning up terrestial-like planets (Sect.
A coupling of the multi-object DFDI instruments with the SDSS telescope will allow simultaneous monitoring of over 100 stars for planet detection and characterization with a moderate to high RV precision (about 10 m/s Doppler precision for a V∼ 11 solar-type star with a DFDI type instrument in an hour integration at the SDSS telescope). This kind of accuracy is suﬃcient to uncover most of the giant planets with a Jupiter mass and a year period since such a planet produces RV variations with a semi-amplitude of ∼ 30 m/s on a solar-type star.
The ‘habitable zone’ of other stars is likely to be closer to the star and coupled with their lower mass the ‘wobble’ introduced by a terrestrial planet’s mass may now be just about detectable. The analysis of the metallicity of stars which have planetary companions is very revealing (Fig. 9). The [Fe/H] ratio is deﬁned as the abundance of iron in a star to that found in the Sun, expressed on a logarithmic scale. Thus a star with [Fe/H]=1 has 10 times the abundance of iron (and other metals) as the Sun.
An Elementary Survey of Celestial Mechanics by Y. Ryabov, G. Yankovsky