Numerical studies of the axisymmetric pulsar magnetosphere
A numerical model based on the assumption that pulsars are spinning magnetized neutron stars is studied. A two-fluid model which includes inertial terms coupled self-consistently with Maxwell's equations is used. In this first paper of the series the case with aligned rotation and magnetic axes is examined with the assumption that the only source of charged particles is the star itself. It is found that under these conditions the magnetic field lines are closed everywhere and the particles in the equatorial region close to the light cylinder R/sub L/ reach sufficiently high energies to escape from the magnetosphere. With the Crab pulsar parameters, 1x10$sup 38$ ergs s$sup -1$ are carried away by relativistic particles and an equatorial region of high energy density is found near R/sub L/. A tentative conclusion is made that the described behavior is due to the assumption regarding the source of particles which results in 100 percent charge separation and a space-charge-limited emission from the star. In this space-charge-limited regime not enough current is available to open the field lines, but the electrostatic forces are large enough to force motion across the field lines. An artificially large particle rest mass has been used in this paper to ensure a smoother transition between the nonrelativistic and highly relativistic regions of space. Solutions which correspond to an essentially negligible rest mass in the nonrelativistic region will be discussed in subsequent papers. (AIP)
- Research Organization:
- Atlas Computer Laboratory, Chilton, Eng.
- Sponsoring Organization:
- USDOE
- NSA Number:
- NSA-33-024028
- OSTI ID:
- 4057678
- Journal Information:
- Astrophys. J., v. 202, no. 3, pp. 762-772, Other Information: Orig. Receipt Date: 30-JUN-76
- Country of Publication:
- United States
- Language:
- English
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