Formation of the 255-Kev Annihilation Line Near the Magnetic Poles of Pulsars V
JETP Letters, Vol. 79, No. 6, 2004, pp. 241–244. Translated from Pis’ma v Zhurnal Éksperimental’noÏ i TeoreticheskoÏ Fiziki, Vol. 79, No. 6, 2004, pp. 299–302. Original Russian Text Copyright © 2004 by Kontorovich, Flanchik. Formation of the 255-keV Annihilation Line near the Magnetic Poles of Pulsars V. M. Kontorovich1, 2 and A. B. Flanchik2 1 Institute of Radio Astronomy, National Academy of Sciences of Ukraine, Kharkov, 61002 Ukraine 2 Kharkov State University, Kharkov, 61077 Ukraine Received December 22, 2003; in final form, February 17, 2004 The possibility of existance is discussed for pulsars emitting soft γ radiation near their magnetic poles upon the annihilation of ultrarelativistic positrons from the magnetosphere and electrons from the surface of a star. With an increase in the energy of incident positrons, the photon energy of this backward radiation tends to a constant 2 value mec /2 = 255 keV. This radiation is shown to be directed opposite to the positron flux direction. © 2004 MAIK “Nauka/Interperiodica”. PACS numbers: 97.60.Gb; 97.10.Ld; 98.70.Rz 1. A pulsar is a source of electromagnetic radiation and, with allowance for the general-relativity effects, over a wide range from radio waves to hard γ radiation the coefficient A is given by the formula [5, 6] 8 γ up to a photon energy of 10 MeV. As is known, rays 3ΩB ω can be emitted due to both ultrarelativistic electrons A = -------------0 4---- cosαε+ cosφ sinα . (2) 2 cR Ω 0 m and positrons moving in a strong magnetic field and various collision processes between charged particles.
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