Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.eso.org/~chummel/oyster/manual/node78.html
Дата изменения: Tue Apr 28 19:12:50 2015
Дата индексирования: Sun Apr 10 20:24:16 2016
Кодировка:

Single-lined spectroscopic binary

Select the appropriate orbital elements, and the mass of the secondary. The reason for not choosing the mass of the primary is that with decreasing primary mass, the situation is asymptotically reached where the primary settles on a Keplerian orbit of a planet sized body and its velocity amplitude does not increase anymore. This would prevent proper fitting of velocity curves of larger amplitudes. If, after fitting, the corresponding velocity amplitude $K_1$ is desired, one uses the modelk function, e.g. PRINT, MODELK('A').