Wind Braking in Neutron Stars

Details Wind Braking in Neutron Stars Wind Braking in Neutron Stars

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.1204h&link_type=abstract

American Astronomical Society, HEAD meeting #10, #12.04

Astronomy and Astrophysics

Astronomy

Scientific paper

There is mounting evidence that relativistic winds are indeed present in pulsars and related objects. This leads to the consideration of an extra mechanism for its braking, as discussed by some available published works, and has a series of observable consequences. We discuss the application of dipole+wind models to radio pulsars and isolated neutron stars (INS), explicitely solved for its simplest version. We then relate the braking index n and jerk parameter m to observed quantities and compare them to the available data, specifically predicting n and m for the sample of radio pulsars, PSR B1931+24 (a key object for which winds have been well-determined) and RXJ 1856-37. Several features of the wind affecting the evolution of these objects are pointed out and discussed, including the initial period, age and magnetic field determinations.
Supported by FAPESP, Sao Paulo and CNPq, Brazil

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