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On the evolution of the radio pulsar PSR J1734-3333

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Çalışkan, Şirin and Ertan, Ünal and Alpar, M. Ali and Trümper, J. E. and Kylafis, N. D. (2013) On the evolution of the radio pulsar PSR J1734-3333. Monthly Notices of the Royal Astronomical Society, 431 (2). pp. 1136-1142. ISSN 0035-8711 (Print) 1365-2966 (Online)

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Official URL: http://dx.doi.org/10.1093/mnras/stt234

Abstract

Recent measurements showed that the period derivative of the ‘hig h-B’ radio pulsar PSR J1734−3333 is increasing with time. For neutron stars evolving with fallback disks, this rotational behavior is expected in certain phases of the long-term evolution. Using the same model as employed earlier to explain the evolution of anomalous X-ray pulsars and soft gamma-ray repeaters, we show that the period,the first and second period derivatives and the X-ray luminosity of this source can simultaneously acquire the observed values for a neutron star evolving with a fallback disk. We find that the required strength of the dipole field that can produce the source properties is in the range of 10^12 − 10^13 G on the pole of the neutron star. When the model source reaches the current state properties of PSR J1734−3333, accretion onto the star has not started yet, allowing the source to operate as a regular radio pulsar. Our results imply that PSR J1734−3333 is at an age of ∼3×10^4 −2×10^5years. Such sources will have properties like the X-ray dim isolated neutron stars or transient AXPs at a later epoch of weak accretion from the diminished fallback disk.

Item Type:Article
Uncontrolled Keywords:accretion, accretion discs; stars: neutron; pulsars: individual: PSR J1734-3333
Subjects:Q Science > QB Astronomy > QB460-466 Astrophysics
Q Science > QC Physics
ID Code:21751
Deposited By:Ünal Ertan
Deposited On:26 Sep 2013 09:52
Last Modified:01 Aug 2019 10:52

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