Rotational velocities of the giants in symbiotic stars: I. D'-type symbiotics

Abstract

We have measured the rotational velocities (v.sini) of the mass donors in a number of D'--type symbiotic stars, using the cross-correlation function method. Four from five D' symbiotic stars with known v.sini, appeared to be very fast rotators compared with the catalogues of v.sini for the corresponding spectral types. At least three of these stars rotate at a substantial fraction (>=0.5) of the critical velocity. This means that at least in D'-type symbiotics the cool components rotate faster than isolated giants. If these binary stars are synchronized, their orbital periods should be relatively short (4-60 days). We also briefly discuss the possible origin of the rapid rotation and its connection with mass loss and dust formation.

arXiv comment6 pages, to be submitted soon

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Cited by in corpus (8)

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• Spectroscopic binaries among Hipparcos M giants III. The eccentricity-period diagram and mass-transfer signatures
• Rotational velocities of the giants in symbiotic stars: III. Evidence of fast rotation in S-type symbiotics
• The spectral energy distribution of D-type symbiotic stars: the role of dust shells
• Gas and dust spectra of the D' type symbiotic star HD330036
• T CrB: overview of the accretion history, Roche-lobe filling, orbital solution, and radiative modeling