Abstract
A modified Roche potential which incorporates the effects of radiation pressure due to one component of a binary system is mathematically explored. In some cases, the resulting potentials do not exhibit the familiar contact surfaces of the classical Roche potential. The concept of a contact surface, which has been fundamental to the investigations of close binary systems, must be used with discretion for close binaries in which one component is very luminous. A convenient criterion for the existence of a contact surface is given by (1-μ) ≃ 3δc 3/2 \((1 - 2(\tfrac{2}{3})^4 \delta _c )\), (δc≪1) where μ is the mass of the very luminous star in terms of the system mass. For systems of given μ, no contact surface exists if δ is greater than δc where δ is the ratio of radiation pressure force to gravitational attraction. Furthermore, energy considerations of the modified Roche potential indicate that binary systems with δ < δc should have a greater tendency to form rings than those with δ < δc.
Similar content being viewed by others
References
Allen, C. W.: 1963,Astrophysical Quantities, Athlone Press, London, 2nd. ed, p. 203.
Biermann, P.: 1971,Astron. Astrophys. 10, 205.
Bisnovatyi-Kogan, G. S.: 1967,Priklad. Mat. Mekh. SSSR 31, 762.
Bisnovatyi-Kogan, G. S. and Zel'dovich, Ya. B.: 1968,Soviet Astron. J. 12, 192.
Faulkner, D. J.: 1970,Astrophys. J. 162, 513.
Finzi, A. and Wolf, R. A.: 1970,Astrophys. Letters 5, 63.
Finzi, A. and Wolf, R. A.: 1971,Astron. Astrophys. 11, 418.
Kuiper, G. P.: 1941,Astrophys. J. 93, 133.
Kutter, G. S., Savedoff, M. P., and Schuerman, D. W.: 1969,Astrophys. Space Sci. 3, 192.
Lucy, L. B.: 1971,Astrophys. J. 163, 95.
Lucy, L. B. and Solomon, P. M.: 1970,Astrophys. J. 159, 879.
Marlborough, J. M. and Roy-Rene, J.: 1970,Astrophys. J. 160, 221.
Prendergast, K. H.: 1960,Astrophys. J. 132, 162.
Schuerman, D. W. and Savedoff, M. P.: 1973, to be published
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Schuerman, D.W. Roche potentials including radiation effects. Astrophys Space Sci 19, 351–358 (1972). https://doi.org/10.1007/BF00645718
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00645718