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Linear Polarization in Close Binaries

Published online by Cambridge University Press:  12 April 2016

S.K. Parman  and
A. Peraiah
S.K. Parman
Affiliation:
Milki H.S. School, Milki, Malda, West Bengal - 73221
A. Peraiah
Affiliation:
Indian Institute of Astrophysics, Bangalore - 560034, India

Abstract

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Theoretical models have been computed for estimating linear polarization from the extended dusty outer layers of the components of close binary stars whose surfaces are distorted by rotation and tidal effects due to the presence of secondary. We have assumed plane-parallel layers of the dusty atmospheres of the components. We have employed a wavelength dependent scattering coefficient, and Rayleigh phase function is used in solving the equation of radiative transfer . It is noticed that polarization increases with decreasing the wavelength and increasing the particle size. Polarization for uniform rotation is larger than that for non-uniform rotation. Polarization for the single stars is always less than that for a binary component.

Subject headings: polarization - radiative transfer - stars: binaries - stars: late-type

Type
Part III Stellar Systems and Galaxies
Information
International Astronomical Union Colloquium , Volume 132: Instability, Chaos and Predictability in Celestial Mechanics and Stellar Dynamics , 1993 , pp. 171 - 181
Copyright
Copyright © Nova Science Publishers 1993

References

[1] Collins, G.W. II, (1970), In Stellar Rotation, ed. Slettebak, A. p.85.Google Scholar
[2] Harrington, J.P. and Collins, G.W. II (1968), Astrophys. J., 151, 1051.CrossRefGoogle Scholar
[3] Hulst, H.C. van de, (1957), Light Scattering by Small Particles, p. 270, John Wiley & Sons, New York.Google Scholar
[4] Ireland, J.G. (1967), Z.Astrophys., 65, 123.Google Scholar
[5] Peraiah, A. (1969), Astron. Astrophys., 3, 163.Google Scholar
[6] Peraiah, A. (1970), Astron. Astrophys., 7, 473.Google Scholar
[7] Peraiah, A. (1976), Astron. Astrophys., 46, 237.Google Scholar
[8] Peraiah, A. (1984), In: Methods in Radiative Transfer, p. 281, ed. Kalkofen, W., Cambridge University Press, Cambridge.Google Scholar
[9] Shah, G.A. (1977), Kodaikanal Obs. Bill. Ser. A, 2, 42.Google Scholar