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We review the studies of rapid variadility of B[e] star CI Come based on extensive monitoring in two seasons of 2006 and 2008. We found that the variability was caused by pulsations of the B4 III-V component. In the composite frequency spectrum, two pulsations components dominate with the periods 0.416 and 0.266 day. In the high resolution BTA/NES spectra taken simultaneously with the photometry, the absorption components in the emission profiles of weak He I lines temporally appear. This is typical of pulsating stars.