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X-ray Bursting Neutron Stars

Published online by Cambridge University Press:  04 August 2017

H. Inoue
H. Inoue*
Affiliation:
Institute of Space and Astronautical Science, Komaba, Meguro-ku, Tokyo 153 Japan

Abstract

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The maximum peak luminosity of the X-ray bursts from a burster is most likely interpreted as the Eddington luminosity of a helium-rich envelope surrounding a neutron star. If this interpretation is true, we can obtain a relation between the mass and the radius of the neutron star in terms of the maximum effective temperature of bursts. On the other hand, the most naive understanding of the origin of the 4.1 keV absorption line often detected in X-ray burst spectra gives us another relation of the neutron star mass with its radius. By solving two simultaneous equations, we can determine the values of the mass and the radius of the neutron star, respectively. However, the result is critical to every neutron star model currently considered.

The persistent emissions from X-ray bursters are also discussed.

Type
II. Accretion Powered Pulsars
Information
Symposium - International Astronomical Union , Volume 125: The Origin and Evolution of Neutron Stars , 1987 , pp. 233 - 243
Copyright
Copyright © Reidel 1987 

References

Alcock, C. 1987, this conference.Google Scholar
Baym, G. and Pethick, C. 1979, Ann. Rev. A. Ap., 17, 415.Google Scholar
Ebisuzaki, T. 1986, submitted to P.A.S. Japan.Google Scholar
Ebisuzaki, T. and Nomoto, K. 1986, Ap. J., in press.Google Scholar
Fujimoto, M.Y. 1985, Ap. J. (Letters), 29, L19.Google Scholar
Fujimoto, M.Y., Sztajno, M., Lewin, W.H.G. and an Paradijs, J. 1986, preprint.Google Scholar
Fujimoto, M.Y. and Taam, R.E. 1986, Ap. J., 305, 246.Google Scholar
Goldmann, I. 1979, A. Ap., 78, L15.Google Scholar
Hanawa, T. 1986, preprint.Google Scholar
Hasinger, G. 1987, this conference.Google Scholar
Hayakawa, S. 1981, Sp. Sci. Rev., 29, 221.CrossRefGoogle Scholar
Hoffman, J.A., Lewin, W.H.G., Primini, F.A. et al., 1979, Ap. J. (Letters), 233, L51.Google Scholar
Hoshi, R. 1984, P.A.S. Japan, 36, 785.Google Scholar
Inoue, H., Waki, I., Koyama, K. et al. 1984, P.A.S. Japan, 36, 831.Google Scholar
Inoue, H. and Hoshi, R. 1986, submitted to Ap. J. (Letters).Google Scholar
Lewin, W.H.G. 1987, this conference.Google Scholar
London, R.A., Taam, R.E. and Howard, W.M. 1984, Ap. J. (Letters), 287, L27.Google Scholar
Mitsuda, K. 1984, , Univ of Tokyo (ISAS RN. 251).Google Scholar
Mitsuda, K., Inoue, H., Koyama, K. et al. 1984, P.A.S. Japan, 36, 741.Google Scholar
Mitsuda, K. and Tanaka, Y. 1986, Proc. NATO Advanced Workshop on the Evolution of Galactic X-Ray Binaries, Tegernsee.Google Scholar
Nakamura, N. 1986, private communication.Google Scholar
Nakamura, N. et al. 1986, in preparation.Google Scholar
Ohashi, T., Inoue, H. Koyama, K. et al. 1982, Ap. J., 258, 254.CrossRefGoogle Scholar
Sugimoto, D., Ebisuzaki, T. and Hanawa, T. 1984, P.A.S. Japan, 36, 839.Google Scholar
Tawara, Y. et al. 1986, in preparation.Google Scholar
van der Klis, M. 198, this conference.Google Scholar
van Paradijs, J. 1982, A. Ap., 107, 51.Google Scholar
Waki, I., Inoue, H., Koyama, K. et al. 1984, P.A.S. Japan, 36, 819.Google Scholar