Evolution of Pulsars on the P-P Diagram

Yusifov, I. M.; Alpar, M. A.; Gok, F.; Huseyinov, O. H.

doi:10.1007/978-94-011-0159-2_22

Cited by 9 publications

(2 citation statements)

References 6 publications

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“…Alternatively, the debris disks around isolated neutron stars may result from the captured interstellar medium (e.g., Popov et al 2000). The fallback disk model was recently adopted to account for the observational characteristics of anomalous X-ray pulsars (Yusifov et al 1995;Chattterjee et al 2000;Alpar 2001). Such disks can also influence pulsar braking indices and timing ages.…”

Section: Rratsmentioning

confidence: 99%

On the Nature of Part-Time Radio Pulsars

2006

ApJ

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The recent discovery of rotating radio transients and the quasi-periodicity of pulsar activity in the radio pulsar PSR B1931ϩ24 has challenged the conventional theory of radio pulsar emission. Here we suggest that these phenomena could be due to the interaction between the neutron star magnetosphere and the surrounding debris disk. The pattern of pulsar emission depends on whether the disk can penetrate the light cylinder and efficiently quench the processes of particle production and acceleration inside the magnetospheric gap. A precessing disk may naturally account for the switch-on/off behavior in PSR B1931ϩ24.

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Section: Rratsmentioning

confidence: 99%

On the Nature of Part-Time Radio Pulsars

2006

ApJ

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“…We suggest (see also Gvaramadze 1999a; cf. Yusifov et al 1995;Istomin & Komberg 2000) that just this effect is responsible for the present high spindown rate of PSR B 1509-58, i.e. that the pulsar loses its rotational energy mainly due to the acceleration of protons of the ambient medium arriving at the light surface at the rateṀ :…”

Section: The Spin-down Of Psr B 1509-58mentioning

confidence: 99%

On the age of PSR B 1509-58

Gvaramadze

2001

A&A

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Abstract. It is generally accepted that the PSR B 1509-58 is associated with the supernova remnant (SNR) MSH 15-52 (G 320.4-01.2). The spin-down age of the pulsar is 1700 years, while the size and the general appearance of the SNR suggest that this system is much older. A few possible explanations of this discrepancy have been put forward. We offer an alternative one and suggest that the high spin-down rate of the pulsar characterizes only a relatively short period of its (present) spin history, and that the enhanced braking torque is connected with the interaction between the pulsar's magnetosphere and the dense matter of a circumstellar clump (created during the late evolutionary stages of the supernova (SN) progenitor star). Our suggestion implies that the "true" age of PSR B 1509-58 could be much larger than the spin-down age, and therefore the SNR MSH 15-52 is a middle-aged remnant similar to the Vela SNR (G 263.9-3.3). We also suggest that the dense (neutral) gas of the circumstellar clump could be responsible for the enhanced neutral hydrogen absorption towards PSR B 1509-58, and that the optical emission of an optical counterpart for PSR B 1509-58 should rather be attributed to a bow shock around this pulsar than to the pulsar itself.

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Associations of different types of neutron star with supernova remnants

Tagieva

Ankay

2003

Astronomical & Astrophysical Transactions

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Evolution of Pulsars on the P-P Diagram

Cited by 9 publications

References 6 publications

On the Nature of Part-Time Radio Pulsars

On the Nature of Part-Time Radio Pulsars

On the age of PSR B 1509-58

Associations of different types of neutron star with supernova remnants

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