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Modified surface redshift of pulsars produced by magnetoplasma. (English) Zbl 1135.85001

Summary: The propagation of photons in the magnetoplasma medium of pulsar magnetosphere is studied in the framework of an effective metric theory. It is found that the surface redshift is induced by two factors: one coming from the gravitational field and another from the magnetoplasma. The magnetoplasma can shift the spectrum, and the modification of surface redshift of pulsars due to associated magnetoplasma can be the same extent as the gravitational redshift in particular cases via calculation.

MSC:

85A05 Galactic and stellar dynamics
85A25 Radiative transfer in astronomy and astrophysics
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References:

[1] Duncan R.C. and Thompson C. (1992). Astrophys. J. 392: L9 · doi:10.1086/186413
[2] Marsden D., (2001). Astrophys. J. 550: 397 · doi:10.1086/319701
[3] Zhang B., Xu R.X. and Qiao G.J. (2000). Astrophys. J. 545: L127 · doi:10.1086/317889
[4] Xu R.X. and Busse F. (2001). Astron. Astrophys. 371: 963 · doi:10.1051/0004-6361:20010450
[5] Xu R.X. (2002). Astrophys. J. 570: L65 · doi:10.1086/340993
[6] Asseo E. and Melikidze G.I. (1998). Mon. Not. R. Astron. Soc. 301: 59 · doi:10.1046/j.1365-8711.1998.01990.x
[7] Melrose D.B. and Gedalin M.E. (1999). Astrophys. J. 521: 351 · doi:10.1086/307539
[8] Gedalin M. and Gruman E. (2002). Phys. Rev. Lett. 88: 121101 · doi:10.1103/PhysRevLett.88.121101
[9] Cordes, J.M.: In: Hankins, T.H. et al. (eds.) The Magnetospheric Structure and Emission Mechanisms of Radio Pulsars, p. 253. Pedagogical University Press, Zielona Góra (1992)
[10] Mosquera Cuesta H.J. and Salim J.M. (2004). Astrophys. J. 608: 925 · doi:10.1086/378686
[11] Mosquera Cuesta H.J. and Salim J.M. (2004). Mon. Not. R. Astron. Soc. 354: L55 · doi:10.1111/j.1365-2966.2004.08375.x
[12] Gordon W. (1923). Ann. Phys. (Leipzig) 72: 421
[13] Schützhold R. (2002). Phys. Rev. Lett. 88: 061101 · doi:10.1103/PhysRevLett.88.061101
[14] Ji P.Y. (2001). Phys. Rev. E 64: 036501 · doi:10.1103/PhysRevE.64.036501
[15] Goldreich P. and Julian W. (1969). Astrophys. J. 157: 869 · doi:10.1086/150119
[16] Sturrock P.A. (1971). Astrophys. J. 164: 529 · doi:10.1086/150865
[17] Ruderman M.A. and Sutherland P.G. (1975). Astrophys. J. 196: 51 · doi:10.1086/153393
[18] Usov V.V. and Melrose D.B. (1996). Astrophys. J. 464: 306 · doi:10.1086/177321
[19] Manchester, R.N., Taylor, J.H.: Pulsars Freeman, SanFrancisco (1977)
[20] Melrose D.B. (1995). J. Astrophys. Astro. 16: 137 · doi:10.1007/BF02714830
[21] Broderick A. and Bland R. (2003). Mon. Not. R. Astron. Soc. 342: 1280 · doi:10.1046/j.1365-8711.2003.06618.x
[22] Lyutikov M. (1998). Mon. Not. R. Astron. Soc. 293: 447 · doi:10.1046/j.1365-8711.1998.01154.x
[23] Gedalin M. and Melrose D.B. (1998). Phys. Rev. E 57: 3399 · doi:10.1103/PhysRevE.57.3399
[24] Lyne A.G. and Lorimer D.R. (1994). Nature 369: 127 · doi:10.1038/369127a0
[25] Asseo E. (2003). Plasma Phys. Control. Fusion 45: 853 · doi:10.1088/0741-3335/45/6/302
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