Abstract
Cen X-3 is probably a neutron star, releasing the infall energy of accreted matter. Sufficient material for accretion will be provided by a conventional stellar wind from its more massive companion star. That star is not likely to rotate synchronously; therefore a ‘Roche lobe’ analysis of the eclipses is not valid. A ‘tidal lobe’ analysis allows the neutron star to have a mass of the order of one solar mass. Overflow of the ‘Roche lobe’ is neither necessary as a source of mass nor probable in view of the observed stellar line widths of the two identified X-ray companions.
The mass flow onto the condensed star is very small in all cases. It is limited, for an object of m solar masses by the Eddington Limiting Luminosity to \({\dot M_{ac}} < {10^{ - 7.4}}m\left( {{M_ \odot } y{r^{ - 1}}} \right)\), which limit applies even if the accreting object contacts or traverses its companion star.
The observed 4.84 s rotation period of the Cen X-3 neutron star is very simply explained as the critical value where a centrifugal barrier regulates the rate of infall to the surface. The X-ray spectrum is understood as blackbody radiation coming from a well-defined area near each magnetic pole of the neutron star.
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References
Beals, C. S.: 1951, Publ. Dom. Astrophys. Obs. 9, 1.
Bolton, C.: 1971, Bull. Am. Astron. Soc. 3, No. 4.
Bondi, H. and Hoyle, F.: 1944, Monthly Notices Roy. Astron. Soc. 104, 273.
Carruthers, G. R.: 1968, Astrophys. J. 151, 269.
Eddington, A.: 1926, The Internal Constitution of the Stars, (reprinted by Dover, New York, 1959 ).
Gott, J. R., Gunn, J. E., and Ostriker, J. P.: 1970, Astrophys. J. 160, L91.
Gribben, J.: 1971, Nature 233, 19.
Hiltner, W. A., Werner, J., and Osmer, P.: 1972, Astrophys. J. Letters,(in press).
Jeans, J. H.: 1919, Problems of Cosmogony and Stellar Dynamics, Cambridge Univ. Press.
Jeans, J. H.: 1928, Astronomy and Cosmogony, Cambridge Univ. Press.
Leach, R. and Ruffin, R.: 1972, (preprint).
Lucy, L. B. and Solomon, P. M.: 1970, Astrophys. J. 159, 879.
Morton, D. C.: 1967, Astrophys. J. 147, 1017.
Morton, D. C.: 1969, Astron. Space Sci. 3, 117.
Ostriker, J. P.: 1968, Nature 217, 1227.
Ostriker, J. P., Rees, M., and Silk, J.: 1970, Astrophys. Letters 6, 179.
Ostriker, J. P. and Tassoul, J.-L.: 1968, Nature 219, 577.
Salpeter, E. E.: 1972, this volume, p. 135.
Schreier, E., Levinson, R., Gursky, H., Kellogg, E., Tananbaum, H., and Giacconi, R.: 1972, Astrophys. J. 172, L79.
Tanabaum, H., Gursky, H., Kellogg, E. M., Levinson, R., Schreier, E., and Giacconi, R.: 1972, Astrophys. J. Letters,(in press).
van den Heuvel, E. P. J.: 1970, in A. Slettebak (ed.), Stellar Rotation, D. Reidel Publ. Co., Dordrecht-Holland, p. 178.
van den Heuvel, E. P. J. and Heise, J.: 1972, Nature,(in press).
Webster, B. L. and Murdin, P.: 1972, Nature 235, 37.
Wilson, R. E.: 1972, Astrophys. J. 174, L27.
Zel’dovich, Ya. B. and Novikov, I. D.: 1964, Soy. Phys. Dokl. 9, 246.
Zel’dovich, Ya. B. and Novikov, I. D.: 1971, Relativistic Astrophysics, Vol. 1, Univ. of Chicago Press, Chicago, Chap. 13.
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Ostriker, J.P., Davidson, K. (1973). Models for Compact Pulsing X-ray Sources. In: Bradt, H., Giacconi, R. (eds) X- and Gamma-Ray Astronomy. International Astronomical Union/Union Astronomique Internationale, vol 55. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-2585-0_12
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