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The braking index of PSR J1734-3333 and the magnetar population

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arxiv 1109.2740 v1 pith:YRNKYCOE submitted 2011-09-13 astro-ph.HE astro-ph.SR

Cristobal M. Espinoza , Andrew Lyne , Michael Kramer , Richard N. Manchester , Victoria Kaspi This is my paper · ORCID
classification astro-ph.HEastro-ph.SR
keywords brakingpropertiesindexj1734-3333periodpulsarsrotation-poweredderivative
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PSR J1734-3333 is a radio pulsar rotating with a period P=1.17 s and slowing down with a period derivative Pdot=2.28 x 10^{-12}, the third largest among rotation-powered pulsars. These properties are midway between those of normal rotation-powered pulsars and magnetars, two populations of neutron stars that are notably different in their emission properties. Here we report on the measurement of the second period derivative of the rotation of PSR J1734-3333 and calculate a braking index n=0.9 +- 0.2. This value is well below 3, the value expected for an electromagnetic braking due to a constant magnetic dipole, and indicates that this pulsar may soon have the rotational properties of a magnetar. While there are several mechanisms which could lead to such a low braking index, we discuss this observation, together with the properties exhibited by some other high-Pdot rotation-powered pulsars, and interpret it as evidence of a possible evolutionary route for magnetars through a radio-pulsar phase, supporting a unified description of the two classes of object.

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Cited by 2 Pith papers

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  1. A Log-Uniform Initial Magnetic Field Distribution Explains Pulsar and Magnetar Populations through Magnetic Inclination Alignment

    astro-ph.HE 2026-06 unverdicted novelty 5.0 of 10

    Magnetic inclination alignment with timescale proportional to B to the minus two suppresses observed numbers of strong-field neutron stars, unifying pulsars and magnetars under one log-uniform initial B distribution.

  2. Understanding the Neutron Star Population with the SKAO Telescopes

    astro-ph.HE 2026-07 accept novelty 3.5 of 10

    SKAO AA* and AA4 surveys are projected to discover thousands of ordinary pulsars and ~800–1000 MSPs, enabling population synthesis, mass measurements and tests of gravity and emission physics.

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