General Relativistic Modification of a Pulsar Electromagnetic Field

Abstract

We consider an exterior electromagnetic field surrounding a rotating star endowed with a dipole magnetic field in the context of general relativity. The analytic solution for a stationary configuration is obtained, and the general relativistic modifications and the implications for pulsar radiation are investigated in detail. We find that the general relativistic corrections of both the electric field strength and the curvature radii of magnetic field lines tend to enhance the curvature radiation photon energy.Comment: 11 pages, 9 figures, accepted for publication in Prog. Theor. Phy

Particle motion and electromagnetic fields of rotating compact gravitating objects with gravitomagnetic charge

“…Starting the pioneering paper of Deutsch [1] it was proved that due to the rotation of highly magnetized star the electric field is induced. The general relativistic effect of dragging of inertial frames is very important in pulsar magnetosphere [2,3] and is considered to be a source of additional electric field of general relativistic origin (see, e.g., [4][5][6][7]). …”

Summary of Parallel Session: “Relativistic and Particle Astrophysics”

“…for PSR 1937+214, the field intensity increases by 10.5 ± 3.7 % due to the curved spacetime and this will increase the frequency by the same amount. On the other hand, in case (ii), modification of the field lines in the magnetosphere leads to modulation of the frequency of curvature radiation 32 : the radius of curvature of the field lines decreases due to the curved spacetime and this will increase the frequency in an inverse manner. -The author also investigates GR effects on polarization of the curvature radiation; by computing the Stokes parameters 33 in curved spacetime.…”

Stationary electromagnetic fields in the exterior of a slowly rotating relativistic star: a description beyond the low-frequency approximation

“…The functions g 1 and h 1 are obtained from . where the constant c 1 is given by the values at the surface ( r = R ) such as α R =α ( R ), We have assumed that the stellar surface behaves as a perfect conductor so that the following boundary condition can be imposed at the stellar surface: E θ + B r α −1 ϖ R sin θ= 0. Note that these analytic solutions have already been derived elsewhere (e.g. Konno & Kojima 2000; Rezzolla et al 2001a,b).…”

“…Ginzburg & Ozernoy 1964; Anderson & Cohen 1970; Petterson 1974) and in slowly rotating space‐times (e.g. Muslimov & Tysgan 1992; Muslimov & Harding 1997; Konno & Kojima 2000).…”