M Dwarfs as Desirable Targets for Planet Search Surveys

Details M Dwarfs as Desirable Targets for Planet Search Surveys M Dwarfs as Desirable Targets for Planet Search Surveys

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.1003t&link_type=abstract

American Astronomical Society, DPS meeting #38, #10.03; Bulletin of the American Astronomical Society, Vol. 38, p.494

Astronomy and Astrophysics

Astronomy

Scientific paper

Here I will illustrate the advantages and disadvantages of focusing different types of planet searches on M dwarfs with the goal of illustrating that these stars may represent the best targets for detecting super-Earth mass (10Me) planets from the ground. These stars have been desirable targets for both radial velocity (RV) and astrometry targets since their reduced mass results in larger signals. However, M dwarfs were not the focus of the original long term RV programs since their faintness counters the advantage gained by a large velocity amplitude. There was also a desire to understand the population of planets around FGK type stars that resemble our Sun. There are now both radial velocity and astrometric programs devoted to searching to planets with three new planetary systems discovered to date - GL876, GL 581, and GL 436. The planets around these stars have some of the lowest masses discovered to date ( 20MJ sini). Ironically, the fact that M dwarfs are faint makes them ideal targets for both transit and direct imaging programs due to a reduction in the contrast level between the star and planet. Larger telescopes and improvements in imaging capabilities are making M dwarfs more viable targets for direct imaging and transit surveys. It is believed that a dedicated transit M dwarf survey could result in the detection of superEarths. In addition to the observational arguments, I will address the theoretical expectations for the population of planets around M dwarfs given current planet formation models. The observed frequency of planets around M dwarfs can distinguish core accretion or disk instability as the dominant planet formation mechanism around low mass stars. Finally, I will discuss the potential for detecting terrestrial mass planets around the nearest M dwarfs with SIM PlanetQuest.

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