Abstract
Under the assumption of a pulsar's magnetic field originating from the net polarized spin of its neutrons, and by using the post-Newtonian approximated torsion in the fifth order in (v/c), the spin precession arising from torsion is coordinate dependent, which influences the magnetic field of the pulsar and makes the magnetic inclination close to the rotation axis. Assuming the possibility of the magnetic inclination density to be in random alignment at the initial time, our theoretical calculations show that most pulsars should have smaller inclinations at the age of 106-107 yr, and that the inclination decreases with the increasing age of the pulsar. This fits the theoretical calculations and astronomically observed distribution.
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References
Hehl, F. W., Von der Heyde, R., Kerlick, G. D., and Nester, J. M. (1976).Rev. Mod. Phys. 48, 393; Hehl, F. W. (1985).Found. Phys. 15, 451; Hehl, F. W., McCrea, J. D., Mielke, F. W., and Ne'eman, Y. (1989).Found Phys. 19, 1075.
Hayashi, K., Shirafuji, T. (1979).Phys. Rev. D15, 3524.
Stoeger, W. R. (1985).Gen. Rel. Grav. 17, 981.
Audretsch, J. (1981).Phys. Rev. D 24, 470.
Nitsch, J. (1980). InCosmology and Gravitation, P. G. Bergmann and V. De Sabbata, eds. (Plenum Press, New York).
Rumpf, H. (1980). InCosmology and Gravitation, P. G. Bergmann and V. De Sabbata, eds. (Plenum Press, New York).
Neville, D. E. (1980).Phys. Rev. D 25, 573.
De Sabbata, V., and Gasperini, M. (1985).Introduction to Gravitation (World Scientific, Singapore).
Yasskin, P. B., Stoeger, W. R. (1980).Phys. Rev. D21, 1081.
Ruderman, M. A. (1972).Rev. Astron. Astrophys. 10, 427.
Ruderman, M. A., and Sutherland, P. G. (1973).Nature 246, 93.
Levy, E. H., and Rose, W. K. (1974).Nature 250, 41.
Yang, G. C. (1983).Phys. Lett. 120B, 201.
Boccaletti, D., De Sabbata, V., and Gualdi, C. (1965).Nuovo Cimento 36, 685.
Shapiro, S. L., and Teukolsky, S. A. (1983).Black Holes, White Dwarfs and Neutron Stars (Wiley & Sons, New York).
Pines, D. (1980).J, Phys. Collog. 41, 111.
Smith, F. G. (1977).Pulsars (Cambridge University Press, Cambridge).
Mashhoon, B. (1988).Phys. Rev. Lett. 62, 2639.
Hehl, F. W., and Ni, W. T. (1990).Phys. Rev. D42, 2045.
Feynman, R. P., Leiton, R. B., and Sands, M. (1966).The Feynman Lectures of Physics (Addison-Wesley, New York).
Gunn, J. E., and Ostriker, J. P. (1969).Nature 221, 454.
Manchester, R. N., and Lyne, A. G. (1977).Mon. Not. R. Astr. Soc. 181, 761; Lyne, A. G., and Manchester, R. N. (1988).Mon. Not. R. Astr. Soc. 234, 477.
Wu, X.-J. (1983). InProc. Academia Sinica-Max-Planck Society Workshop on High Energy Astrophysics, J. Yang, ed. (Science Press/ Gordon Breach, Bei**g).
Taylor, J. H., and Manchester, R. N. (1980).Five College Astronomy Observatory Pulsar List.
Kerlick, G. D. (1975).Astrophys. J. 185, 631.
De Sabbata, V., and Gasperini, M. (1980).Lett. Nuovo Cimento 27, 133.
Back, D. C., and Kulkarni, S. R. (1990).Phys. Today 3, 26; Bailee, M. (1989).Astrophys. J. 34, 917.
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This essay received an honorable mention in 1990 from the Gravity Research Foundation-Ed.
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Zhang, Cm., Yang, Gc., Chen, Fp. et al. Is there evidence for torsion?. Gen Relat Gravit 24, 359–371 (1992). https://doi.org/10.1007/BF00760412
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DOI: https://doi.org/10.1007/BF00760412