On the spin-down of PSR B1509-58

Details On the spin-down of PSR B1509-58 On the spin-down of PSR B1509-58

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...422l..83k&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 422, no. 2, p. L83-L86

Astronomy and Astrophysics

Astronomy

106

Crab Nebula, Energy Dissipation, Pulsars, Spin Reduction, Stellar Models, Stellar Rotation, Supernova Remnants, Angular Momentum, Kinetic Energy, Magnetic Moments, Radio Telescopes, X Ray Astronomy

Scientific paper

The pulsar PSR B1509-58 is associated with the supernova remnant G320.4-1.2 (MSH 15-52) and has the largest pulse period derivative and the second smallest characteristic age after the Crab pulsar. Although PSR B1509-58 is the second youngest known pulsar, it has not glitched during an 11 yr data span and shows little timing noise, permitting an accurate study of its slowdown. We have measured its braking index to be n = 2.837 +/- 0.001 and its frequency third derivative = (-1.02 +/- 0.25) x 10-31/5-4. The third derivative is consistent with the value expected for a constant braking index and magnetic moment, although we cannot rule out models in which these quantities vary.

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