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Unpulsed X-rays from Pulsars

Published online by Cambridge University Press:  14 August 2015

David J. Helfand
David J. Helfand*
Affiliation:
Columbia Astrophysics Laboratory, Departments of Astronomy and Physics, Columbia University, New York, New York 10027

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The radio emission from pulsars is energetically insignificant, yet its distinctive character led to their discovery and subsequent identification with rotating magnetized neutron stars. In the intervening thirteen years, a wealth of radio data have been accumulated from which we have learned something of the magnetospheric properties, stellar structure, and evolutionary history of these objects. Yet we still do not know how pulsars pulse, what the neutron star interior is like or, with certainty, how and where pulsars are formed. And, we have not yet ‘seen’ a radio pulsar, in the sense that we see other stars, i.e., by detecting thermal photons from its surface. The Einstein Observatory soft X-ray telescope offers a new opportunity to attempt such an observation. We report herein the preliminary results of several programs aimed at the detection of thermal X-ray emission from isolated neutron stars.

Type
VII. Properties of Neutron Stars
Information
Symposium - International Astronomical Union , Volume 95: Pulsars , 1981 , pp. 343 - 350
Copyright
Copyright © Reidel 1981 

References

Cheng, A. and Ruderman, M.A.: 1977, Astrophys. J. 216, 865.Google Scholar
Cheng, A. and Ruderman, M.A.: 1980, preprint.Google Scholar
Giacconi, R. et al.: 1979, Astrophys. J. 230, 540.Google Scholar
Glen, G. and Sutherland, P.G.: 1980, preprint.Google Scholar
Glen, G. and Sutherland, P.G.: 1979, Bull. Am. Astron. Soc. 11, 779.Google Scholar
Greenstein, G. and McClintock, J.E.: 1974, Science 185, 487.Google Scholar
Greenstein, G., Margon, B., Bowyer, S., Lampton, M., Paresce, F., Stern, R., and Gordon, K.: 1977, Astron. Astrophys. 54, 623.Google Scholar
Harding, D., Guyer, R.A., and Greenstein, G.: 1978, Astrophys. J. 222, 991.Google Scholar
Harnden, F.R.: May 1980, talk presented at Workshop on “Stellar Collapse, Supernovae, and Neutron Star Formation”, Santa Barbara, California.Google Scholar
Harnden, F.R., Buehler, B., Giacconi, R., Grindlay, J., Hertz, P., Schreier, E., Seward, F., Tananbaum, H., and van Speybroeck, L.: 1979, Bull. Am. Astron. Soc. 11, 789.Google Scholar
Helfand, D.: 1981, in Giacconi, R. (ed.), X-Ray Astronomy, Proc. HEAD-AAS, D. Reidel, Dordrecht, p. 39.Google Scholar
Helfand, D.J. and Chanan, G.A.: 1980, in preparation.Google Scholar
Helfand, D.J., Chanan, G.A., and Greenstein, G.: 1980, in preparation.Google Scholar
Helfand, D.J., Chanan, G.A., and Novick, R.: 1980, Nature 283, 337.Google Scholar
Lamb, D.Q. and van Riper, K.A.: 1979, Bull. Am. Astron. Soc. 11, 779.Google Scholar
McCulloch, P.M., Hamilton, P.A., Ables, J.G., and Komesaroff, M.M.: 1976, Mon. Not. R. Astr. Soc. 175, 718.Google Scholar
Novick, R., Chanan, G., and Helfand, D.J.: 1979, Bull. Am. Astron. Soc. 11, 779.Google Scholar
Radhakrishnan, V. and Cooke, D.J.: 1969, Astrophys. J. Letters 3, L225.Google Scholar
Taylor, J.H. and Manchester, R.N.: 1975, Astron. J. 80, 794.Google Scholar
Toor, A. and Seward, F.D.: 1977, Astrophys. J. 216, 560.CrossRefGoogle Scholar
Tsuruta, S.: 1979, Phys. Reports 56, p. 237.Google Scholar
Tuohy, I. and Garmire, G.: 1980, Astrophys. J. Letters, in press.Google Scholar
Wolff, R.S., Kestenbaum, H.L., Ku, W., and Novick, R.: 1975, Astrophys. J. Letters 202, L77.Google Scholar