A cold neutron star in the transient low-mass X-ray binary HETE J1900.1–2455 after 10 yr of active accretion

Degenaar, N.; Ootes, L. S.; Reynolds, M. T.; Wijnands, Rudy; Page, Dany

doi:10.1093/mnrasl/slw197

Cited by 36 publications

(54 citation statements)

References 57 publications

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“…Thus, leaving a detailed analysis of X-ray observations for each MSP beyond the scope of this paper, we assume that MSPs should (generally) be colder than the transiently accreting NSs with the measured surface temperature. To get an idea of the possible upper limit on the MSP surface temperature we rely on observations of MXB 1659−298 (assumed distance to the source D = 10 kpc and X-ray absorption column density NH = (2.0 ± 0.2) × 10 21 cm −2 ), IGR 00291+5934 (D = 4 kpc and NH = 2.8 × 10 21 cm −2 ), and HETE J1900.1-2455 (D ≈ 4.7 kpc and NH ≈ 2.2 × 10 21 cm −2 ), reported by Cackett et al (2008), Heinke et al (2009), andDegenaar et al (2017). For all of them the effective surface temperature was estimated as T ∞ eff ≈ 6.3×10 5 K. Note that, for these objects both absorption column density and distances are relatively large in comparison to typical fast MSPs (with ν > 250 Hz).…”

Section: X-ray and Uv Observations Of Mspsmentioning

confidence: 81%

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R modes and neutron star recycling scenario

Chugunov¹,

Gusakov²,

Kantor

2017

Monthly Notices of the Royal Astronomical Society

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To put new constraints on the r-mode instability window, we analyse the formation of millisecond pulsars (MSPs) within the recycling scenario, making use of three sets of observations: (a) X-ray observations of neutron stars (NSs) in low-mass X-ray binaries; (b) timing of millisecond pulsars; and (c) X-ray and UV observations of MSPs. As shown in previous works, r-mode dissipation by shear viscosity is not sufficient to explain observational set (a), and enhanced r-mode dissipation at the red-shifted internal temperatures T ∞ ∼ 10 8 K is required to stabilize the observed NSs. Here, we argue that models with enhanced bulk viscosity can hardly lead to a self-consistent explanation of observational set (a) due to strong neutrino emission, which is typical for these models (unrealistically powerful energy source is required to keep NSs at the observed temperatures). We also demonstrate that the observational set (b) , combined with the theory of internal heating and NS cooling, provides evidence of enhanced r-mode dissipation at low temperatures, T ∞ ∼ 2×10 7 K. Observational set (c) allows us to set an upper limit on the internal temperatures of MSPs, T ∞ < 2 × 10 7 K (assuming a canonical NS with the accreted crust). Recycling scenario can produce MSPs at these temperatures only if r-mode instability is suppressed in the whole MSP spin frequency range (ν 750 Hz) at temperatures 2 × 10 7 T ∞ 3 × 10 7 K, providing thus a new constraint on the r-mode instability window. These observational constraints are analysed in more details in application to the resonance uplift scenario of Gusakov et al. (2014b,a).

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Section: X-ray and Uv Observations Of Mspsmentioning

confidence: 81%

“…1, temperature for HETE J1900.1-2455 was updated according to Degenaar et al (2017), T ∞ eff = 6.3×10 5 K). At least 8 NSs among them are predicted to be r-mode unstable within the minimal r-mode instability model.…”

Section: X-ray Observations Of Transiently Accreting Neutron Stars Inmentioning

confidence: 99%

R modes and neutron star recycling scenario

Chugunov¹,

Gusakov²,

Kantor

2017

Monthly Notices of the Royal Astronomical Society

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“…The data for HETE J1900.1-2455 consist of one observation from which the temperature is derived and several upper limits, so that the cooling curve cannot be used to distinguish the envelope composition [58]. We include both heavy and light envelopes in Table III for HETE J1900.1-2455.…”

Section: Comparison With Observationsmentioning

confidence: 99%

“…The temperature of HETE J1900.1-2455 is based on a single observation [58] and may drop to a lower value in the future. Figure 8 shows that if HETE J1900.1-2455 has a light element envelope, the degree of neutron and proton pairing in the core would begin to be constrained if the effective temperature dropped below ≈ 40 eV.…”

Section: Comparison With Observationsmentioning

confidence: 99%

Lower limit on the heat capacity of the neutron star core

et al. 2017

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We show that observations of the core temperature of transiently-accreting neutron stars combined with observations of an accretion outburst give a lower limit to the neutron star core heat capacity. For the neutron stars in the low mass X-ray binaries KS 1731-260, MXB 1659-29, and XTE J1701-462, we show that the lower limit is a factor of a few below the core heat capacity expected if neutrons and protons in the core are paired, so that electrons provide the dominant contribution to the heat capacity. This limit rules out a core dominated by a quark color-flavor-locked (CFL) phase, which would have a much lower heat capacity. Future observations of or limits on cooling during quiescence will further constrain the core heat capacity.

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“…The steady luminosity decrease of these sources into quiescence can provide information on crust composition and properties [22][23][24][25] and limit the core heat capacity [26] (in some cases even for shorter outbursts the crust can come out of equilibrium, see [27,28]). …”

Section: A Thermal States Of Sxrtsmentioning

confidence: 99%

Cooling of neutron stars in soft x-ray transients

Steiner

2017

Phys. Rev. C

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Thermal states of neutron stars in soft X-ray transients (SXRTs) are thought to be determined by "deep crustal heating" in the accreted matter that drives the quiescent luminosity and cooling via emission of photons and neutrinos from the interior. In this study, we assume a global thermal steady-state of the transient system and calculate the heating curves (quiescent surface luminosity as a function of mean accretion rate) predicted from theoretical models, taking into account variations in the equations of state, superfluidity gaps, thickness of the light element layer and a phenomenological description of the direct Urca threshold. We further provide a statistical analysis on the uncertainties in these parameters, and compare the overall results with observations of several SXRTs, in particular the two sources containing the coldest (SAX J1808.4-3658) and the hottest (Aql X-1) neutron stars. Interpretation of the observational data indicates that the direct Urca process is required for the most massive stars and also suggests small superfluid gaps.

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A cold neutron star in the transient low-mass X-ray binary HETE J1900.1–2455 after 10 yr of active accretion

Cited by 36 publications

References 57 publications

R modes and neutron star recycling scenario

R modes and neutron star recycling scenario

Lower limit on the heat capacity of the neutron star core

Cooling of neutron stars in soft x-ray transients

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