Hostname: page-component-7479d7b7d-q6k6v Total loading time: 0 Render date: 2024-07-12T04:29:38.507Z Has data issue: false hasContentIssue false
  • English
  • Français

Two Types of Pulsars

Published online by Cambridge University Press:  04 August 2017

J.H. Huang
J.H. Huang*
Affiliation:
Astrophysics Institute, Nanking University, Nanking, China

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

To sort out the whole sample of pulsars with measured P and P into two types has much something to do with the origin and evolution of neutron stars. Under the configuration of two types of pulsars with different spindown mechanism, we have discussed a variety of their properties, including their radio emission mechanism, space velocities, interior structures and evolutionary modes. The fact that different type of pulsars does have quite different properties indicates that the processes to create neutron stars may have two distinct types, say, Type II supernova explosion and the collapse of accreting white dwarfs. The evolutionary mode for our Type I pulsars provides such a key link between binary pulsars and X-ray binary pulsars that we may propose a self-consistent scenario for binary pulsars, X-ray binary pulsars, fast pulsars as well as Type I pulsars.

Type
V. Neutron Star Physics
Information
Symposium - International Astronomical Union , Volume 125: The Origin and Evolution of Neutron Stars , 1987 , pp. 425 - 437
Copyright
Copyright © Reidel 1987 

References

Alpar, M.A., Cheng, A.F., Ruderman, M.A., and Shaham, J.: 1982, Nature, 300, 728.Google Scholar
Arnaud, M., and Rothenflug, R.: 1981, Astron. Astrophys., 103, 263.Google Scholar
Deng, Z.G., Huang, J.H., and Xia, X.Y.: 1987, this volume.Google Scholar
Gunn, J.H., and Ostriker, J.P.: 1970, Astrophys. J., 160, 979.Google Scholar
Helfand, D.J., and Tademaru, E.: 1977, Astrophys. J., 216, 842.CrossRefGoogle Scholar
Huang, J.H., Lingenfelter, R.E., Peng, Q.H., and Huang, K.L.: 1982, Astron. Astrophys., 113, 9.Google Scholar
Huang, J.H., Huang, K.L., and Peng, Q.H.: 1983, Astron. Astrophys, 117, 205.Google Scholar
Huang, J.H., Huang, K.L., and Peng, Q.H.: 1985, Astron. Astrophys., 148, 391.Google Scholar
Huang, J.H., Deng, Z.G., and Xia, X.Y.: 1987a, this volume, ‘Radio Emission Mechanism for Two Types of Pulsars’.Google Scholar
Huang, J.H., Deng, Z.G., and Xia, X.Y.: 1987b, this volume, ‘Kinematic Properties for Two Types of Pulsars’.Google Scholar
Huang, J.H., Deng, Z.G., and Xia, X.Y.: 1987c, this volume, ‘Interior Structures for Two Types of Pulsars’.CrossRefGoogle Scholar
Krishnamohan, S.: 1987, this volume.Google Scholar
Lyne, A.G., Manchester, R.N., and Taylor, J.H.: 1985, Mon. Not. R. Astron. Soc., 213, 613.CrossRefGoogle Scholar
Malov, I.F.: 1985, Sov. Astron., 29, 144.Google Scholar
Manchester, R.N., and Lyne, A.G.: 1977, Mon. Not. R. Astron. Soc., 181, 761.Google Scholar
Peng, Q.H., Huang, K.L., and Huang, J.H.: 1982, Astron. Astrophys., 107, 258.Google Scholar
Pineault, S.: 1987, this volume.Google Scholar
Prószyński, M.: 1979, Astron. Astrophys., 79, 8.Google Scholar
Prószyńaki, M., and Przybycien, D.: 1984, STScI preprint, No.22.Google Scholar
Radhakrishnan, V.: 1981, in Pulsars, ed. Sieber, W., Wielebinski, R., Reidel, Dordrecht, p.449.Google Scholar
Radhakrishnan, V.: 1984, in Birth and Evolution of Netron Stars: issues raised by millisecond pulsars, ed. Reynolds, S.P., Stinebring, D.R., p.130.Google Scholar
van den Heuvel, E.: 1984, J. Astron. Astrophys., 5, 209.Google Scholar
van den Heuvel, E.: 1987, this volume.Google Scholar
Xia, X.Y., Deng, Z.G., and Huang, J.H.: 1986, in preparation.Google Scholar