Unifying neutron stars getting to GUNS

Igoshev, Andrei P.; Попов, С. Б.; Turolla, R.

doi:10.1002/asna.201312029

Cited by 15 publications

(11 citation statements)

References 32 publications

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“…The attempt to explain the different manifestations of neutron stars (e.g. Mereghetti 2011) in the context of a unified evolutionary picture is one of the current challenges in the study of neutron stars (Kaspi 2010;Igoshev et al 2014). In the P − Ṗ diagram, shown in Fig.…”

Section: Introductionmentioning

confidence: 99%

XMM-Newton observations of PSR J0726−2612, a radio-loud XDINS

Rigoselli

Mereghetti

Suleimanov

et al. 2019

A&A

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We present the results of an XMM-Newton observation of the slowly rotating (P = 3.4 s), highly magnetized (B ≈ 3×10 13 G) radio pulsar PSR J0726−2612. A previous X-ray observation with the Chandra satellite showed that some of the properties of PSR J0726−2612 are similar to those of the X-ray Dim Isolated Neutron Stars (XDINSs), a small class of nearby slow pulsars characterized by purely thermal X-ray spectra and undetected in the radio band. We confirm the thermal nature of the X-ray emission of PSR J0726−2612, which can be fit by the sum of two blackbodies with temperatures kT 1 = 0.074 +0.006 −0.011 keV and kT 2 = 0.14 +0.04 −0.02 keV and emitting radii R 1 = 10.4 +10.8 −2.8 km and R 2 = 0.5 +0.9 −0.3 km, respectively (assuming a distance of 1 kpc). A broad absorption line modeled with a Gaussian profile centred at 0.39 +0.02 −0.03 keV is required in the fit. The pulse profile of PSR J0726−2612 is characterized by two peaks with similar intensity separated by two unequal minima, a shape and pulsed fraction that cannot be reproduced without invoking magnetic beaming of the X-ray emission. The presence of a single radio pulse suggests that in PSR J0726−2612 the angles that the dipole axis and the line of sight make with the rotation axis, ξ and χ respectively, are similar. This geometry differs from that of the two radio-silent XDINSs with a double peaked pulse profile similar to that of PSR J0726−2612, for which ξ ∼ 90 • and χ ∼ 45 • have been recently estimated. These results strengthen the similarity between PSR J0726−2612 and the XDINSs and support the possibility that the lack of radio emission from the latter might simply be due to an unfavourable viewing geometry.

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Section: Introductionmentioning

confidence: 99%

XMM-Newton observations of PSR J0726−2612, a radio-loud XDINS

Rigoselli

Mereghetti

Suleimanov

et al. 2019

A&A

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“…The main classes of NSs include standard radio pulsars (PSRs), the soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs), the nearby cooling NSs called the "Magnificent Seven" (M7), the rotating radio transients (RRATs), and the central compact objects (CCOs) in supernova remnants (SNRs). The evolutionary scenario called the "grand unification for NSs" (GUNS) (Kaspi 2010;Igoshev, Popov & Turolla 2014), attempts to explain this variety of sources. Population synthesis studies have meanwhile yielded fruitful results.…”

Section: Introductionmentioning

confidence: 99%

Post-fall-back evolution of multipolar magnetic fields and radio pulsar activation

Igoshev¹,

Elfritz²,

Попов³

2016

Mon. Not. R. Astron. Soc.

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It has long been unclear if the small-scale magnetic structures on the neutron star (NS) surface could survive the fall-back episode. The study of the Hall cascade (Cumming, Arras & Zweibel 2004;Wareing & Hollerbach 2009) hinted that energy in small scales structures should dissipate on short timescales. Our new 2D magneto-thermal simulations suggest the opposite. For the first ∼10 kyrs after the fall-back episode with accreted mass 10 −3 M , the observed NS magnetic field appears dipolar, which is insensitive to the initial magnetic topology. In framework of the Ruderman & Sutherland (1975) vacuum gap model during this interval, non-thermal radiation is strongly suppressed. After this time the initial (i.e. multipolar) structure begins to re-emerge through the NS crust. We distinguish three evolutionary epochs for the re-emergence process: the growth of internal toroidal field, the advection of buried poloidal field, and slow Ohmic diffusion. The efficiency of the first two stages can be enhanced when small-scale magnetic structure is present. The efficient re-emergence of high order harmonics might significantly affect the curvature of the magnetospheric field lines in the emission zone. So, only after few 10 4 yrs would the NS starts shining as a pulsar again, which is in correspondence with radio silence of central compact objects (CCOs). In addition, these results can explain the absence of good candidates for thermally emitting NSs with freshly re-emerged field among radio pulsars (Bogdanov, Ng & Kaspi 2014), as NSs have time to cool down, and supernova remnants can already dissipate.

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“…The idea of unifying different types of young isolated NSs in one evolutionary framework (Kaspi 2010) looks very promising (see for example, Viganò et al 2013;Igoshev, Popov, & Turolla 2014 and references and discussions therein). The concept of buried magnetic field (Bernal et al 2010;Ho 2011;Viganò & Pons 2012) might be once more ingredient necessary to fulfill the program of 'Grand unification of neutron stars'.…”

Section: Unification Of Nssmentioning

confidence: 99%

Central Compact Objects in Kes 79 and RCW 103 as ‘Hidden’ Magnetars with Crustal Activity

Попов

Kaurov

Kaminker

2015

Publ. Astron. Soc. Aust.

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We propose that observations of 'hidden' magnetars in central compact objects can be used to probe crustal activity of neutron stars with large internal magnetic fields. Estimates based on calculations by Perna & Pons, Pons & Rea and Kaminker et al. suggest that central compact objects, which are proposed to be 'hidden' magnetars, must demonstrate flux variations on the time scale of months-years. However, the most prominent candidate for the 'hidden' magnetars -CXO J1852.6+0040 in Kes 79 -shows constant (within error bars) flux. This can be interpreted by lower variable crustal activity than in typical magnetars. Alternatively, CXO J1852.6+0040 can be in a high state of variable activity during the whole period of observations. Then we consider the source 1E161348−5055 in RCW103 as another candidate. Employing a simple 2D-modelling we argue that properties of the source can be explained by the crustal activity of the magnetar type. Thus, this object may be supplemented for the three known candidates for the 'hidden' magnetars among central compact objects discussed in literature.

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Unifying neutron stars getting to GUNS

Cited by 15 publications

References 32 publications

XMM-Newton observations of PSR J0726−2612, a radio-loud XDINS

XMM-Newton observations of PSR J0726−2612, a radio-loud XDINS

Post-fall-back evolution of multipolar magnetic fields and radio pulsar activation

Central Compact Objects in Kes 79 and RCW 103 as ‘Hidden’ Magnetars with Crustal Activity

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