Long-term evolution of dim isolated neutron stars

Ertan, Ünal; Çalışkan, Şirin; Benli, Onur; Alpar, M. A.

doi:10.1093/mnras/stu1523

Cited by 24 publications

(70 citation statements)

References 69 publications

(86 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…There are three basic disc parameters that are expected to be similar for the fallback discs of different systems: the X-ray irradiation efficiency (C), the minimum critical temperature below which the disc becomes viscously passive (T p ), and the α parameter of the kinematic viscosity (Shakura and Sunyaev, 1973). In this work, we use the same values of the C, T p , and α parameters as those employed earlier in the evolution models of individual AXP/SGRs (Benli and Ertan, 2016), XDINs (Ertan et al, 2014), and the three HBRPs with measured braking indices (Benli and Ertan, 2017).…”

Section: Model Parametersmentioning

confidence: 99%

Rotational and X-ray luminosity evolution of high-B radio pulsars

Benli

Ertan

2018

New Astronomy

View full text Add to dashboard Cite

In continuation of our earlier work on the long-term evolution of the so-called high--B radio pulsars (HBRPs) with measured braking indices, we have investigated the long-term evolution of the remaining five HBRPs for which braking indices have not been measured yet. This completes our source-by-source analyses of HBRPs in the fallback disc model that was also applied earlier to anomalous X-ray pulsars (AXPs), soft gamma repeaters (SGRs), and dim isolated neutron stars (XDINs). Our results show that the X-ray luminosities and the rotational properties of these rather different neutron star populations can be acquired by neutron stars with fallback discs as a result of differences in their initial conditions, namely the initial disc mass, initial period and the dipole field strength. For the five HBRPs, unlike for AXPs, SGRs and XDINs, our results do not constrain the dipole field strengths of the sources. We obtain evolutionary paths leading to the properties of HBRPs in the propeller phase with dipole fields sufficiently strong to produce pulsed radio emission.Comment: 14 pages, 3 figures, 1 table, accepted for publication in New Astronom

show abstract

Section: Model Parametersmentioning

confidence: 99%

Rotational and X-ray luminosity evolution of high-B radio pulsars

Benli

Ertan

2018

New Astronomy

View full text Add to dashboard Cite

show abstract

“…Considering alternatively an active fallback disk model, Ertan et al (2017Ertan et al ( , 2014 showed that such a disk is able to produce the X-ray properties and the optical excess of the XTINSs. Here, we use their model to check whether such a fallback disk can reproduce the measured NIR excess.…”

Section: Emission From Circumstellar Material?mentioning

confidence: 99%

“…The model also considers X-ray irradiation which is most relevant for the passive outer part of the disk. For details on the model and the model parameters for RX J0806.4-4123, we refer to Ertan et al (2017Ertan et al ( , 2014. The outer radius of the passive disk is not well known and depends on the initial disk conditions and the Xray luminosity in the early phase of evolution.…”

Section: Emission From Circumstellar Material?mentioning

confidence: 99%

“…In this model, magnetars and XTINSs are hot because they are heated by the decay of their large magnetic fields. In an alternative model, the observational properties of the XTINSs and magnetars are explained by formation of and influence by supernova fallback disks (e.g., Ertan et al 2014). However, the fallback disk model alone cannot explain the giant outbursts of magnetars.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Discovery of Extended Infrared Emission around the Neutron Star RXJ0806.4–4123* ^†

Posselt

Pavlov

Ertan

et al. 2018

ApJ

Self Cite

View full text Add to dashboard Cite

Following up on a faint detection of a near-infrared (NIR) source at the position of the X-ray thermal isolated neutron star RX J0806.4-4123, we present new Hubble Space Telescope (HST ) observations in the H-band. The NIR source is unambiguously detected with a Vega magnitude of 23.7 ± 0.2 (flux density of 0.40 ± 0.06 µJy at λ = 1.54 µm). The source position is coincident with the neutron star position, and the implied NIR flux is strongly in excess of what one would expect from an extrapolation of the optical-UV spectrum of RX J0806.4-4123. The NIR source is extended with a size of at least 0. 8 and shows some asymmetry. The conservative upper limit on the flux contribution of a point source is 50%. Emission from gas and dust in the ambient diffuse interstellar medium can be excluded as cause for the extended emission. The source parameters are consistent with an interpretation as either the first NIR-only detected pulsar wind nebula or the first resolved disk around an isolated neutron star.

show abstract

“…They suggested that XDINSs are supposed to be dead magnetars. In addition to these, two magnetars may have passive fallback disks (Wang et al 2006;Ertan et al (2014) interpret that XDINSs have gone through a past accretion phase with spin-down and emerged in their current state. In Figure 5, we could find that the radio-loud magnetars are above the death line.…”

Section: Discussionmentioning

confidence: 99%

Dependence of pulsar death line on the equation of state

Xia

Tong

Zhu

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Pulsar death line can be defined in P − P diagram. Traditionally, radio-loud pulsars are supposed to locate above the death line where is the radio-loud region. With the development of observational equipment, the observational properties of the neutron star are remarkably diverse. In P − P diagram, some of the special sources are radioquiet but lie above the death line. From the definition of the pulsar death line, different equation of states for neutron star or strange star results in different death lines. We discuss the influence of the equation of state on the pulsar death line and the possible link between different neutron star groups. The results show that central compact objects would be the small mass of self-bound strange stars, and rotating radio transients might be old pulsars on the verge of death. We suggest that PSR J2144-3933 is likely to be a large mass pulsar, which would be larger than 2.0M ⊙ . Multiple observational facts would help us to reveal the nature of pulsars.

show abstract

Long-term evolution of dim isolated neutron stars

Cited by 24 publications

References 69 publications

Rotational and X-ray luminosity evolution of high-B radio pulsars

Rotational and X-ray luminosity evolution of high-B radio pulsars

Discovery of Extended Infrared Emission around the Neutron Star RXJ0806.4–4123* ^†

Dependence of pulsar death line on the equation of state

Contact Info

Product

Resources

About

Long-term evolution of dim isolated neutron stars

Cited by 24 publications

References 69 publications

Rotational and X-ray luminosity evolution of high-B radio pulsars

Rotational and X-ray luminosity evolution of high-B radio pulsars

Discovery of Extended Infrared Emission around the Neutron Star RXJ0806.4–4123* †

Dependence of pulsar death line on the equation of state

Contact Info

Product

Resources

About

Discovery of Extended Infrared Emission around the Neutron Star RXJ0806.4–4123* ^†