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Title: A study of K i 7699 Å and related shell lines during the recent eclipse of ϵ Aurigae
Authors: Muthumariappan, C
Parthasarathy, M
Leadbeater, R
Potravnov, I. S
Appakutty, M
Jayakumar, K
Keywords: Stars: AGB and post-AGB;Circumstellar matter;Stars: evolution;Stars: individual : Eclipsing binaries
Issue Date: 11-Dec-2014
Publisher: Oxford University Press on behalf of the Royal Astronomical Society
Citation: Monthly Notices of the Royal Astronomical Society, Vol. 445, No. 3, pp. 2884-2899
Abstract: We report high-resolution (R = 30 000, 45 000 and 75 000) echelle and medium-resolution (R = 22 000 and 10 000) spectroscopic observations of the long-period, eclipsing binary ε Aurigae during the 2009 - 2011 eclipse. Low-excitation shell lines, viz, the K I line at 7699 Å(with 346 data points), A Cr I lines at 5345.807 Å and 5348.326 Å and Fe A A I line at 5110.435 Å which A originated from the disk shaped secondary, Hα and the shell components of the Na D1 and D2 lines show significant variation in their shapes and radial velocities during the eclipse. The equivalent width curve shown by the KI line around the ingress and egress phases indicates that the gas density in the trailing edge is about a factor of two higher than density in the leading edge. Using a geometrical model, in which a homogeneous, cylindrical Keplarian disk eclipses the F0Ia primary star and the shell absorption lines originate from the gaseous atmosphere around an opaque disk, we fit the equivalent width and the radial velocity curves of the KI line covering the full eclipse. A reasonably good fit can be achieved by a low-mass binary model where the mass of the central star of the disk is 5.4 M⊙ and the mass of the primary is 2.5 M⊙ and a disk size of 8.9 AU. The low-mass of the primary, with enhanced s-process elements found by Sadakane et al. (2010), supports that it is a post-AGB F supergiant. For the high-mass binary model, the modelled radial velocity curve deviates significantly from the observations.
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