Isolated Neutron Stars: Accretors and Coolers

Treves, A.; Turolla, R.; Zane, S.; Colpi, M.

doi:10.1086/316529

Cited by 156 publications

(183 citation statements)

References 108 publications

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“…ISM-accretion is proposed to make isolated NSs shine with weak soft X-rays luminosity (e.g., Treves et al 2000). For the X-ray luminosity of XDINS, ∼ (10 31 − 10 32 ) erg s −1 (Kaplan & van Kerkwijk 2009), one could estimate the accretion rate to beṀ X ∼ (10 10 −10 11 g s −1 , which should equal approximately the accretion rateṀ B proposed by Bondi (1952).…”

Section: Formation Of Plasma Atmosphere Of Strangeonmentioning

confidence: 99%

The Optical/UV Excess of X-Ray-dim Isolated Neutron Stars. I. Bremsstrahlung Emission from a Strangeon Star Atmosphere

Wang

Tong

et al. 2017

ApJ

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X-ray dim isolated neutron stars (XDINSs) are characterized by Planckian spectra in X-ray bands, but show optical/ultraviolet(UV) excesses which are the measured photometry exceeding that is extrapolated from X-ray spectra. To solve this problem, a radiative model of bremsstrahlung emission from a plasma atmosphere is established in the regime of strangeon star. A strangeon star atmosphere could simply be regarded as the upper layer of a normal neutron star. This plasma atmosphere, formed and maintained by the ISM-accreted matter due to the so-called strangeness barrier, is supposed to be of two-temperature. All the seven XDINS spectra could be well fitted by the radiative model, from optical/UV to X-ray bands. The fitted radiation radii of XDINSs are from 7 to 13 km, while the modelled electron temperatures are between 50 and 250 eV, except RX J0806.4-4123 with a radiation radius ∼ 3.5 km, indicating that this source could be a low-mass strangeon star candidate. This strangeon star model could further be tested by soft X-ray polarimetry, such as the Lightweight Asymmetry and Magnetism Probe which is expected to work on Chinese space station around 2020.

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Section: Formation Of Plasma Atmosphere Of Strangeonmentioning

confidence: 99%

The Optical/UV Excess of X-Ray-dim Isolated Neutron Stars. I. Bremsstrahlung Emission from a Strangeon Star Atmosphere

Wang

Tong

et al. 2017

ApJ

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“…Popov & Prokhorov 1998;Treves et al 2000;Agol & Kamionkowski 2002) were performed, for example, in the ROSAT catalog (e.g. Neuhäuser & Trümper 1999).…”

Section: Introductionmentioning

confidence: 99%

Probing isolated compact remnants with microlensing

Sartore

Treves

2010

A&A

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Aims. We consider isolated compact remnants (ICoRs), i.e. neutrons stars and black holes that do not reside in binary systems and therefore cannot be detected as X-ray binaries. ICoRs may represent ∼5 percent of the stellar mass budget of the Galaxy, but they are very hard to detect. Here we explore the possibility of using microlensing to identify ICoRs. Methods. In a previous paper we described a simulation of neutron star evolution in phase space in the Galaxy, taking into account the distribution of the progenitors and the kick at formation. Here we first reconsider the evolution and distribution of neutron stars and black holes with an added a bulge component. From the new distributions we calculate the microlensing optical depth, event rate and distribution of event time scales, comparing and contrasting the case of ICoRs and "normal stars". Results. We find that the contribution of remnants to optical depth is slightly lower than without kinematics, owing to the evaporation from the Galaxy. On the other hand, the relative contribution to the rate of events is a factor ∼5 higher. In all, ∼6−7 percent of the events are likely related to ICoRs. In particular, ∼30−40 percent of the events with duration >100 days are possibly related to black holes. Conclusions. It seems therefore that microlensing observations are a suitable tool to probe the population of Galactic ICoRs.

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“…RQINSs have previously been speculated to be related to AXPs and SGRs (see Treves et al 2000 for a review); however, using our model we describe how RQINSs are a natural consequence of the magnetic field decay due to vortex expulsion in quark stars.…”

Section: Radio-quiet Isolated Neutron Starsmentioning

confidence: 98%

Magnetic Field Decay and Period Evolution of Anomalous X-Ray Pulsarsin the Context of Quark Stars

Niebergal

Ouyed

Leahy

2006

ApJ

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We discuss a model wherein soft gamma-ray repeaters (SGRs), anomalous X-ray pulsars (AXPs), and radioquiet isolated neutron stars (RQINSs) are all compact objects exhibiting superconductivity, namely, color-flavorlocked quark stars. In particular, we calculate the magnetic field decay due to the expulsion of spin-induced vortices from the star's superfluid-superconducting interior, and the resultant spin-down rate. We find that for initial parameters characteristic of AXPs/SGRs ( , ), the magnetic field strengths 13 14 10 G ! B ! 10 G 3 s ! P ! 12 s and periods remain unchanged within a factor of 2 for timescales on the order of to yr given 5 75 # 10 5 # 10 a quark star of radius 10 km. Within these timescales, we show that the observed period clustering in RQINSs can be explained by compactness, and we calculate how the magnetic field and period evolve in a manner concurrent with RQINS observations.

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Isolated Neutron Stars: Accretors and Coolers

Cited by 156 publications

References 108 publications

The Optical/UV Excess of X-Ray-dim Isolated Neutron Stars. I. Bremsstrahlung Emission from a Strangeon Star Atmosphere

The Optical/UV Excess of X-Ray-dim Isolated Neutron Stars. I. Bremsstrahlung Emission from a Strangeon Star Atmosphere

Probing isolated compact remnants with microlensing

Magnetic Field Decay and Period Evolution of Anomalous X-Ray Pulsarsin the Context of Quark Stars

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