Multiplicity Among Massive Stars

Details Multiplicity Among Massive Stars Multiplicity Among Massive Stars

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sfet.confe..57r&link_type=abstract

"Star Formation in the Era of Three Great Observatories, meeting abstracts from the conference held July 13-15, 2005 in Cambridg

Computer Science

Scientific paper

Multiwavelength observations as exemplified by NASA's Great Observatories have provided a far clearer picture of the frequency of multiplicity in star systems. Cepheids (typically 5 Msun) are good representatives of massive stars. It is frequently the case that a third star is not apparent until the second star can be directly observed. As an example, the spectra of hot secondaries in Cepheid systems can be obtained in the satellite ultraviolet. In a number of ways (to be illustrated) this has provided evidence of a third star. In a recent compilation of the best studied ``binary'' Cepheid systems, 44 percent are in fact triple systems.

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