Theoretical Mass Estimates for the Mira-Type Variable R Hydrae

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Abstract

Calculations of stellar evolution at initial abundances of helium 
 and heavier elements 
 were done for stars with masses on the main sequence 
. Evolutionary sequences corresponding to the AGB stage were used for modelling the pulsation period decrease observed for almost two centuries in the Mira-type variable R Hya. Diminution of the period from  @ 495 d in the second half of the eighteenth century to @ d in the 1950s is due to stellar radius decrease accompanying dissipation of the @ diation–diffusion wave generated by the helium flash. For all the history of its @bservations R Hya was the fundamental mode pulsator. The best agreement with @ bservations is obtained for eight evolutionary models with initial mass @ and the mass loss rate parameter of the Blöcker formula @. Theoretical mass estimates of R Hya are in the range @, whereas the mean stellar radius (@) corresponding to the pulsation period @ d agrees well with @easurements of the angular diameter by methods of the optical @nterferometric imaging.

About the authors

Yu. A. Fadeyev

Institute of Astronomy, Russian Academy of Sciences

Author for correspondence.
Email: fadeyev@inasan.ru
119017, Moscow, Russia

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