Документ взят из кэша поисковой машины. Адрес
оригинального документа
: http://star.arm.ac.uk/~csj/research/rcb_review/node5.html
Дата изменения: Fri Jan 25 15:33:06 2002 Дата индексирования: Tue Oct 2 09:37:11 2012 Кодировка: Поисковые слова: п п п п п п п п п п п п |
The distribution of galactic RCB stars is controversial. Several
authors have argued that they belong to a thick galactic disk, and are
thus old Population I stars. The evidence is their scale height in the
Galaxy (400pc, [Iben & Tutukov 1985]). However, their distribution and space
velocities suggest they may alternatively belong to the even older
galactic bulge (Population II, [Drilling 1986]). The controversy may
simply be a result of the different ways in which surveys for RCB
stars and related objects have been carried out. In either case, the
populations are sufficiently old that RCB stars must have relatively
low masses (
).
A growing number of RCBs has been discovered in the Large Magellanic
Cloud (LMC), most recently as a result of wide field surveys
([Alcock et al. 1996]). These are the only RCB stars for which a distance is
known and hence for which an absolute magnitude can be deduced. With
to -5, the LMC RCBs are 3000 - 10000 times
more luminous than the Sun ([Feast 1979])