Planets and stars

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Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998arep...42...99t&link_type=abstract

Astronomy Reports, Volume 42, Issue 1, January 1998, pp.99-104

Astronomy and Astrophysics

Astronomy

2

Scientific paper

The basic conditions for the formation and detection of planetary systems around nearby stars are analyzed. About one-third of main sequence stars with masses below 10 M_solar can have (and probably do have, according to the most recent observations) planetary systems. As expected, all planets discovered so far are located beyond the boundaries of the dust evaporation zones around their central stars, but inside the outer boundaries of the zones in which planets form by accretion over the lifetime of the central star. The central star of a planetary system can be not only a main sequence star, but also a white dwarf, neutron star, or black hole. It is not excluded that the individual components of wide binaries, and also close binary systems, can have planetary systems.

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