Browsing by Author "Finkbeiner, Bernd"

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Open Access
Effects of radiation damping on particle motion in pulsar vacuum fields
(1989) Finkbeiner, Bernd; Herold, Heinz; Ertl, Thomas; Ruder, Hanns
The effects of radiation reaction on the motion of charged particles are studied in strong electric and magnetic fields with special attention to the vacuum near-field region of an oblique rotator. For strong radiation damping a local velocity field is derived from the Lorentz-Dirac equation, which efficiently describes the motion of electrons and positrons in the whole range of typical pulsar parameters. The velocity field makes it possible to define regions in the inner magnetosphere, where particle trapping occurs due to the radiation losses. By numerical integration of particle trajectories from the pulsar surface, regions around the magnetic poles are found which are defined by particle emission into the wave zone. The shapes of the escape regions on the pulsar surface are determined to a considerable extent by the presence of the accumulation regions.
Open Access
Particle motion in pulsar magnetospheres
(1987) Finkbeiner, Bernd; Ertl, Thomas; Herold, Heinz; Ruder, Hanns
This report discusses some new results we found in studying the trajectories of single charged particles in the vacuum magnetosphere of a pulsar using the oblique rotator model. We believe that investigations of individual particles in the vicinity of the star can be useful for a better understanding of some fundamental problems of pulsar physics, e.g. the global structure of the magnetosphere or the pulsar radiation.
Open Access
Self-consistent modelling of pulsar magnetospheres
(1989) Herold, Heinz; Ertl, Thomas; Finkbeiner, Bernd; Ruder, Hanns
The magnetosphere of a rapidly rotating, strongly magnetized neutron star with aligned magnetic and rotational axes (parallel rotator) is modelled numerically. Including the radiation of the particles accelerated to relativistic energies as an efficient damping mechanism, we obtain a quasi-stationary selfconsistent solution to this classical problem. The numerical simulation, which was started from the well-known vacuum solution, yields a global magnetospheric structure that can be characterized by two regions of oppositely charged particles, which eventually produce a relativistic pulsar wind, separated by a vacuum gap of considerable extent.
Open Access
Self-consistent modelling of pulsar magnetospheres
(1987) Ertl, Thomas; Herold, Heinz; Finkbeiner, Bernd; Ruder, Hanns
We report on some progress that we have achieved by numerically modelling the magnetosphere of an aligned rotator where the rotation axis is parallel to the magnetic axis of the neutron star. Here, the unipolar induction, which should be responsible for populating the magnetosphere with charged particles pulled out from the neutron star surface via field emission can be studied in purity, whereas electromagnetic wave effects are neglected.
Open Access
Self-consistent numerical modelling of pulsar magnetospheres
(1992) Herold, Heinz; Ertl, Thomas; Finkbeiner, Bernd; Ruder, Hanns
The magnetosphere of a rapidly rotating, strongly magnetized neutron star with aligned magnetic and rotational axes (parallel rotator) is modelled numerically. Including the radiation of the particles accelerated to relativistic energies as an efficient damping mechanism, we obtain a quasi-stationary self-consistent solution to this classical problem. The numerical simulation,which was started from the well-known vacuum solution, yields a global magnetospheric structure that can be characterized by two regions of oppositely charged particles, which eventually produce a relativistic pulsar wind, separated by a vacuum gap of considerable extent.
Open Access
Towards a self-consistent modelling of pulsar magnetospheres
(1987) Herold, Heinz; Ertl, Thomas; Finkbeiner, Bernd; Ruder, Hanns
The numerical modelling of the general case of an oblique rotator is a very complicated time-dependent 3-dimensional problem and in its full extent probably outside the capicity of present.day computers. A considerable simplification occurs if one can assume that the essential effects may be understood by modelling the magnetosphere of an aligned rotator (where the rotation axis is parallel to the magnetic axis of the neutron star). This assumption is only reasonable for small obliqueness, since by this approach all electromagnetic wave effects are not taken into account.