A Deep<i>Chandra</i>Survey of the Globular Cluster 47 Tucanae: Catalog of Point Sources

Heinke, C. O.; Grindlay, Jonathan E.; Edmonds, P. D.; Cohn, H. N.; Lugger, P. M.; Camilo, F.; Bogdanov, Slavko; Freire, P. C. C.

doi:10.1086/429899

Cited by 228 publications

(374 citation statements)

References 114 publications

(289 reference statements)

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“…MSPs in globular cluster 47 Tuc provide yet another example suggesting that the observations put even stronger constraint on T ∞ eff than (8). This globular cluster is particularly good for X-ray studies, because it is close (D ≈ 4.5 kpc) and weakly absorbed (cluster NH ≈ 1.3 × 10 20 cm −2 , e.g., Heinke et al 2005 The X-ray luminosity of MSPs with high spin-down power can be even larger. However, they have power-law X-ray spectrum and a high fraction of pulsed emission (see, e.g., section 4.2 in Ng et al 2014).…”

Section: X-ray and Uv Observations Of Mspsmentioning

confidence: 99%

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: 99%

R modes and neutron star recycling scenario

Chugunov¹,

Gusakov²,

Kantor

2017

Monthly Notices of the Royal Astronomical Society

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“…Heinke et al 2005). The single temperature mekal model was rejected by the worse fit (χ 2 /d.o.f.=157/135).…”

Section: X-ray Spectramentioning

confidence: 99%

XMM–Newtonstudies of the supernova remnant G350.0−2.0

Карпова¹,

Shternin²,

Zyuzin³

et al. 2016

Mon. Not. R. Astron. Soc.

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We report the results of XMM-Newton observations of the Galactic mixed-morphology supernova remnant G350.0−2.0. Diffuse thermal X-ray emission fills the north-western part of the remnant surrounded by radio shell-like structures. We did not detect any X-ray counterpart of the latter structures, but found several bright blobs within the diffuse emission. The X-ray spectrum of the most part of the remnant can be described by a collisionally-ionized plasma model vapec with solar abundances and a temperature of ≈ 0.8 keV. The solar abundances of plasma indicate that the X-ray emission comes from the shocked interstellar material. The overabundance of Fe was found in some of the bright blobs. We also analysed the brightest point-like X-ray source 1RXS J172653.4−382157 projected on the extended emission. Its spectrum is well described by the two-temperature optically thin thermal plasma model mekal typical for cataclysmic variable stars. The cataclysmic variable source nature is supported by the presence of a faint (g ≈ 21) optical source with non-stellar spectral energy distribution at the X-ray position of 1RXS J172653.4−382157. It was detected with the XMM-Newton optical/UV monitor in the U filter and was also found in the archival Hα and optical/near-infrared broadband sky survey images. On the other hand, the X-ray spectrum is also described by the power law plus thermal component model typical for a rotation powered pulsar. Therefore, the pulsar interpretation of the source cannot be excluded. For this source, we derived the upper limit for the pulsed fraction of 27 per cent.

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“…the core-collapsed cluster NGC 6397 (Cohn et al 2010) and the massive cluster 47 Tuc (Heinke et al 2005), will shed light on the effect of cluster parameters.…”

Section: Very Close Binaries Revealed Through X-ray Emissionmentioning

confidence: 99%

The M 4 Core Project with HST: I. Overview and first epoch

et al. 2013

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We present an overview of the ongoing Hubble Space Telescope large program GO-12911. The program is focused on the core of M 4, the nearest Galactic globular cluster, and the observations are designed to constrain the number of binaries with massive companions (black holes, neutron stars, or white dwarfs) by measuring the "wobble" of the luminous (mainsequence) companion around the center of mass of the pair, with an astrometric precision of ∼ 50 μas. The high spatial resolution and stable medium-band PSFs of WFC3/UVIS will make these measurements possible. In this work we describe (i) the motivation behind this study, (ii) our observing strategy, (iii) the many other investigations enabled by this unique data set, and which of those our team is conducting, and (iv) a preliminary reduction of the first-epoch dataset collected on

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A DeepChandraSurvey of the Globular Cluster 47 Tucanae: Catalog of Point Sources

Cited by 228 publications

References 114 publications

R modes and neutron star recycling scenario

R modes and neutron star recycling scenario

XMM–Newtonstudies of the supernova remnant G350.0−2.0

The M 4 Core Project with HST: I. Overview and first epoch

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