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Coherent Curvature Emission in Pulsar Magnetospheres: Non-dipolar Geometric Effects

Published online by Cambridge University Press:  25 April 2016

Qinghuan Luo
Qinghuan Luo*
Affiliation:
Research Centre for Theoretical Astrophysics, School of Physics, University of Sydney, NSW 2006
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Abstract

The effects of the specific geometry of the magnetic field (such as field lines with torsion) on curvature emission and absorption in pulsar magnetospheres are discussed. Curvature maser emission can arise from two effects: the curvature drift, as has already been discussed in the literature, and field line torsion as discussed here in detail for the first time. Maser emission due to field line torsion can operate only when the Lorentz factor is larger than a certain value. However, when the Lorentz factor of electrons or positrons is sufficiently high, curvature masering is due to both curvature drift and magnetic field line torsion. The optical depth in the case of field line torsion is estimated. It is shown that if torsion is due to rotation, the resultant luminosity should be dependent on the rotation period in such a way that shorter periods correspond to larger luminosities.

Type
Galactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 10 , Issue 3 , 1993 , pp. 258 - 262
Copyright
Copyright © Astronomical Society of Australia 1993

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References

Beskin, V.S., Gurevich, A.V. and Istomin, Ya.N., 1988, Astrophys. Space Sci., 146, 205.Google Scholar
Blandford, R.D., 1975, Mon. Not. R. astr. Soc., 170, 551.Google Scholar
Blaskiewicz, M., Cordes, J.M. and Wasserman, I., 1991, Astrophys. J., 370, 643.Google Scholar
Cheng, A. F. and Ruderman, M.A., 1980, Astrophys.|J., 235, 576.Google Scholar
Goldreich, P. and Julian, W.H., 1969, Astrophys. J., 157, 869.Google Scholar
Davies, J.G., Lyne, A.G., Smith, F.G., Izvekova, V.A., Kuzmin, A.D. and Shitov, Y.P., 1984, Mon. Not. R. astr. Soc., 211, 57.Google Scholar
Jackson, J.D., 1968, Classical Electromagnetic Field, John Wiley and Son, New York.Google Scholar
Luo, Q., 1992, in preparation.Google Scholar
Luo, Q. and Melrose, D.B., 1992a, Proc Astron. Soc. Aust., 10, in press.Google Scholar
Luo, Q. and Melrose, D.B., 1992b, Mon. Not. R. astr. Soc., 258,616.Google Scholar
Machabeli, G.Z., 1991, Plasma Phys. Contr. Fusion, 33, 1227.CrossRefGoogle Scholar
Machabeli, G.Z., and Usov, V.V., 1989, Sov. Astron. Lett., 15, 393.Google Scholar
Malov, I.F. and Suleimanova, S.A., 1991, Astrofizika, 31, 551.Google Scholar
Malov, I.F., 1991, Sov. Astron. Lett., 17, 254.Google Scholar
Melrose, D.B., 1978, Astrophys. J., 225, 557.Google Scholar
Michel, F.C., 1990, Theory of Neutron Star Magnetospheres, Chicargo University Press.Google Scholar
Nambu, M., 1989, Plasma Phys. Contr. Fusion, 31, 143.Google Scholar
Ruderman, M.A., 1991, Astrophys. J., 366, 261; 382, 576; 587.Google Scholar
Ruderman, M.A., and Sutherland, P.G., 1975, Astrophys. J., 196, 51.Google Scholar
Shitov, Y.P., 1983, Sov. Astron. J., 27, 314.Google Scholar
Schwinger, J., 1949, Phys. Rev., 75, 1912.Google Scholar
Zheleznyakov, V.V. and Shaposhnikov, V.E., 1979, Aust. J. Phys., 32, 49.Google Scholar