On the evolution of the radio pulsar PSR J1734−3333

Çalışkan, Şirin; Ertan, Ünal; Alpar, M. A.; Trümper, J.; Kylafis, N. D.

doi:10.1093/mnras/stt234

Cited by 28 publications

(20 citation statements)

References 27 publications

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“…Main disk parameters used in the present work are very similar to those employed in our earlier work to explain the X-ray enhancements and the evolution of AXP and SGRs (Ertan et al 2009, Ç alışkan & Ertan 2012, Ç alışkan et al 2013. The model sources with the dipole field strength in the 0.5 − 1.0 × 10 12 G range on the pole of the star and with the initial periods greater than ∼ 55 ms can reach the X-ray luminosity and the rotational properties of Swift J1822.3-1606 simultaneously.…”

Section: Discussionmentioning

confidence: 88%

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X-Ray Enhancement and Long-Term Evolution of Swift J1822.3–1606

Benli

Çalışkan

Ertan

et al. 2013

ApJ

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We investigate the X-ray enhancement and the long-term evolution of the recently discovered, second "low-B magnetar" Swift J1822.3-1606 in the frame of the fallback disk model. During a soft gamma burst episode, the inner disk matter is pushed back to larger radii forming a density gradient at the inner disk. Subsequent relaxation of the inner disk could account for the observed Xray enhancement light curve of Swift J1822.3-1606. We obtain model fits to the X-ray data with basic disk parameters similar to those employed to explain the X-ray outburst light curves of other anomalous X-ray pulsars and soft gamma repeaters. The long period (8.4 s) of the neutron star can be reached by the effect of the disk torques in the long-term accretion phase (1 − 3 × 10 5 yr). The currently ongoing X-ray enhancement could be due to a transient accretion epoch or the source could still be in the accretion phase in quiescence. Considering these different possibilities, we determine the model curves that could represent the long-term rotational and the X-ray luminosity evolution of Swift J1822.3-1606, which constrain the strength of the magnetic dipole field to the range of 1 − 2 × 10 12 G on the surface of the neutron star.

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Section: Discussionmentioning

confidence: 88%

“…(2009), Alpar et al (2011), andÇ alışkan et al (2013). Here, we briefly describe the basic long-term evolutionary phases of a neutron star evolving with a fallback disk.…”

Section: Long-term Evolution Of Swift J18223-1606mentioning

confidence: 99%

X-Ray Enhancement and Long-Term Evolution of Swift J1822.3–1606

Benli

Çalışkan

Ertan

et al. 2013

ApJ

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“…We use the code developed to investigate the long-term evolution of AXPs and SGRs (see Ertan & Erkut 2008;Ertan et al 2009;Alpar et al 2011;Ç alışkan et al 2013 for details and applications). We examine the period, the period derivative and the total X-ray luminosity evolution of the model sources, tracing the initial conditions, namely the initial period, P0, strength of the magnetic dipole field on the pole of the star, B0, and the initial disk mass, M d .…”

Section: Modelmentioning

confidence: 99%

Long-term evolution of dim isolated neutron stars

Ertan¹,

Çalışkan²,

Benli³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The dim isolated neutron stars (XDINs) have periods in the same range as the anomalous X-ray pulsars (AXPs) and the soft gamma-ray repeaters (SGRs). We apply the fallback disk model, which explains the period clustering and other properties of AXP/SGRs, to the six XDINs with measured periods and period derivatives. Present properties of XDINs are obtained in evolutionary scenarios with surface dipole magnetic fields B 0 ∼ 10 12 G. The XDINs have gone through an accretion epoch with rapid spin-down earlier, and have emerged in their current state, with the X-ray luminosity provided by neutron star cooling and no longer by accretion. Our results indicate that the known XDINs are not likely to be active radio pulsars, as the low B 0 , together with their long periods place these sources clearly below the "death valley".

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“…In this section, we investigate the long-term X-ray luminosity and rotational evolution of SGR 0501+4516 with a fallback disc (for details and applications of this model see Ertan et al 2009;Alpar et al 2011;Benli et al 2013;Ç alışkan et al 2013). We solve the diffusion equation for a geometrically thin disc.…”

Section: Long-term Evolution Of Sgr 0501+4516mentioning

confidence: 99%

Long-term evolution, X-ray outburst and optical/infrared emission of SGR 0501+4516

Benli

Çalışkan

Ertan

2015

Monthly Notices of the Royal Astronomical Society

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We have analyzed the long-term evolution and the X-ray outburst light curve of SGR 0501+4516 in the frame of the fallback disc model. We have shown that the X-ray luminosity, period and period derivative of this typical soft gamma repeater can be achieved by a neutron star with a large range of initial disc masses provided that the source has a magnetic dipole field of ∼ 1.4 × 10 12 G on the pole of the star. At present, the star is accreting matter from the disc, which has an age ∼ 3 × 10 4 yr, and will remain in the accretion phase until t ∼ 2-5 × 10 5 yr depending on the initial disc mass. With its current rotational rate, this source is not expected to give pulsed radio emission even if the accretion on to the star is hindered by some mechanism. The X-ray enhancement light curve of SGR 0501+4516 can be accounted for by the same model applied earlier to the X-ray enhancement light curves of other anomalous X-ray pulsars/soft gamma repeaters with the same basic disc parameters. We have further shown that the optical/IR data of SGR 0501+4516 is in good agreement with the emission from an irradiated fallback disc with the properties consistent with our long-term evolution model.

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On the evolution of the radio pulsar PSR J1734−3333

Cited by 28 publications

References 27 publications

X-Ray Enhancement and Long-Term Evolution of Swift J1822.3–1606

X-Ray Enhancement and Long-Term Evolution of Swift J1822.3–1606

Long-term evolution of dim isolated neutron stars

Long-term evolution, X-ray outburst and optical/infrared emission of SGR 0501+4516

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