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Evolutionary scenario for W UMa-type stars

  • K. Stepień (a1) and K. Gazeas (a2)

Abstract

An alternative to TRO model of a W UMa-type star is presented in which the binary is past mass exchange with mass ratio reversal. The secondary is hydrogen depleted and both components are in thermal equilibrium. Evolution in contact is driven by orbital angular momentum loss and mass transfer from the secondary to primary component, similarly as it is observed in Algols. Temperature equalization of both components results from an assumed energy transfer by a large scale flow encircling the whole system in the common envelope.

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References

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Eggleton, P. P. & Kiseleva-Eggleton, L. 2002, ApJ 575, 461
Gazeas, K. & Stepień, K. 2008, astro-ph0803.0212
Kähler, H. 2004, A&A 414, 317
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Stepień, K. 2004, in: Dupree, A.K. & Benz, A.O. (eds.) Stars as Suns: Activity, Evolution and Planets, IAU Symp. No. 219 (San Francisco: Astr. Soc. of Pacific), p. 967
Stepień, K. 2006, AcA 56, 199
Wood, B. E., Müller, H. R., Zank, G. P., & Linsky, J. L. 2002, ApJ 574, 412
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