Thermal Properties of the Middle-Aged Pulsar J1741–2054

Карпова, А В; Danilenko, A.; Shibanov, Yu. A.; Shternin, P. S.; Zyuzin, D.

doi:10.1088/0004-637x/789/2/97

Cited by 16 publications

(27 citation statements)

References 25 publications

(36 reference statements)

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“…Modeling the photon index as a function of distance from the pul- sar using a linear regression fit with a constant function in SHERPA, we obtain Γ = 1.67 ± 0.06 for the trail. The global PWN index derived from the SHERPA fit and the values we obtained in Table 3 are consistent with Karpova et al (2014) and Marelli et al (2014), who derived Γ = 1.74 ± 0.07 and Γ = 1.78 ± 0.15 respectively for the PWN.…”

Section: Pwn and Its Extended X-ray Trailsupporting

confidence: 90%

“…The emission is well described by a point source, with the exception of the artifact feature (identified in cyan). We thus see no conclusive evidence of other small-scale structure in the immediate region surrounding the pulsar, consistent with the results reported by Karpova et al (2014).…”

Section: X-ray Imagingsupporting

confidence: 86%

“…We obtained N H = (1.20 (Wilms et al 2000). Modeling the spectrum with a power-law plus blackbody model, we obtained a photon index of Γ = 2.68 ± 0.04 and a blackbody spectrum with a temperature of kT eff = 61.7 ± 3.0 eV, in excellent agreement with the results reported by Marelli et al (2014) and Karpova et al (2014). Omitting the pile-up correction yields similar values.…”

Section: Spectral Analysis Of the X-ray Emission Of Thesupporting

confidence: 85%

“…Romani et al (2010) also suggested that there are asymmetries in the small scale structure surrounding the pulsar, which they associate with a compact 2.5 ′′ equatorial toroidal structure. Marelli et al (2014) and Karpova et al (2014) performed a spectral analysis of the pulsar emission using XMM-Newton and Chandra and determined that a twocomponent (blackbody plus power-law) model is required to obtain satisfactory spectral fits.…”

Section: Detected a 20mentioning

confidence: 99%

“…They discovered that the region around the pulsar appears to be slightly extended and they associate this feature with the equatorial torus of the PWN. Using the same data as analyzed here, Karpova et al (2014) searched for evidence of such structure by performing fits to a two-dimensional Gaussian convolved with PSF models generated for each observation. They find no evidence for any small-scale extended features other than for a small emission feature associated with a known mirror artifact 14 .…”

Section: X-ray Imagingmentioning

confidence: 99%

See 4 more Smart Citations

X-Ray Analysis of the Proper Motion and Pulsar Wind Nebula for PSR J1741-2054

Auchettl

Slane

Romani

et al. 2015

ApJ

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We obtained six observations of PSR J1741-2054 using the Chandra ACIS-S detector totaling ∼300 ks. By registering this new epoch of observations to an archival observation taken 3.2 years earlier using X-ray point sources in the field of view, we have measured the pulsar proper motion at µ = 109 ± 10mas yr −1 in a direction consistent with the symmetry axis of the observed Hα nebula. We investigated the inferred past trajectory of the pulsar but find no compelling association with OB associations in which the progenitor may have originated. We confirm previous measurements of the pulsar spectrum as an absorbed power law with photon index Γ=2.68±0.04, plus a blackbody with an emission radius of (4.5 +3.2 −2.5 )d 0.38 km, for a DM-estimated distance of 0.38d 0.38 kpc and a temperature of 61.7 ± 3.0 eV. Emission from the compact nebula is well described by an absorbed power law model with a photon index of Γ = 1.67±0.06, while the diffuse emission seen as a trail extending northeast of the pulsar shows no evidence of synchrotron cooling. We also applied image deconvolution techniques to search for small-scale structures in the immediate vicinity of the pulsar, but found no conclusive evidence for such structures.

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Section: Pwn and Its Extended X-ray Trailsupporting

confidence: 90%

Section: X-ray Imagingsupporting

confidence: 86%

Section: Spectral Analysis Of the X-ray Emission Of Thesupporting

confidence: 85%

Section: Detected a 20mentioning

confidence: 99%

Section: X-ray Imagingmentioning

confidence: 99%

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X-Ray Analysis of the Proper Motion and Pulsar Wind Nebula for PSR J1741-2054

Auchettl

Slane

Romani

et al. 2015

ApJ

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The γ-ray Pulsar J0633+0632 in X-rays

Danilenko

Shternin

Карпова

et al. 2015

Publ. Astron. Soc. Aust.

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We analysed Chandra observations of the bright Fermi pulsar J0633+0632 and found evidence of an absorption feature in its spectrum at 804 +42 −26 eV (the errors are at 90% confidence) with equivalent width of 63 +47 −36 eV. In addition, we analysed in detail the X-ray spectral continuum taking into account correlations between the interstellar absorption and the distance to the source. We confirm early findings that the spectrum contains non-thermal and thermal components. The latter is equally well described by the blackbody and magnetised atmosphere models and can be attributed to the emission from the bulk of the stellar surface in both cases. The distance to the pulsar is constrained in a range of 1-4 kpc from the spectral fits. We infer the blackbody surface temperature of 108 +22 −14 eV, while for the atmosphere model, the temperature, as seen by a distant observer, is 53 +12 −7 eV. In the latter case, J0633+0632 is one of the coldest middle-aged isolated neutron stars. Finally, it powers an extended pulsar wind nebula whose shape suggests a high pulsar proper motion. Looking backwards the direction of the presumed proper motion, we found a likely birthplace of the pulsar-the Rosette nebula, a 50-Myr-old active star-forming region located at about 1.5 • from the pulsar. If true, this constrains the distance to the pulsar in the range of 1.2-1.8 kpc.

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The neutron star in HESS J1731−347: Central compact objects as laboratories to study the equation of state of superdense matter

Klochkov

Suleimanov

Pühlhofer

et al. 2014

A&A

118

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Context. Central compact objects (CCOs) in supernova remnants are isolated thermally emitting neutron stars (NSs). They are most probably characterized by a magnetic field strength that is roughly two orders of magnitude lower than that of most of the radio and accreting pulsars. The thermal emission of CCOs can be modeled to obtain constraints on the physical parameters of the star such as its mass, radius, effective temperature, and chemical composition.Aims. The CCO in HESS J1731−347 is one of the brightest objects in this class. Starting from 2007, it was observed several times with different X-ray satellites. Here we present our analysis of two new XMM-Newton observations of the source performed in 2013 which increase the total exposure time of the data available for spectral analysis by a factor of about five compared to the analyses presented before. Methods. We use our numerical spectral models for carbon and hydrogen atmospheres to fit the spectrum of the CCO. From our fits, we derive constraints on the physical parameters of the emitting star such as its mass, radius, distance, and effective temperature. We also use the new data to derive new upper limits on the source pulsations and to confirm the absence of a long-term flux and spectral variability.Results. The analysis shows that atmosphere models are clearly preferred by the fit over the blackbody spectral function. Under the assumption that the X-ray emission is uniformly produced by the entire star surface (supported by the lack of pulsations), hydrogen atmosphere models lead to uncomfortably large distances of the CCO, above 7-8 kpc. On the other hand, the carbon atmosphere model formally excludes distances above 5-6 kpc and is compatible with the source located in the Scutum-Crux (∼3 kpc) or NormaCygnus (∼4.5 kpc) Galactic spiral arm. We provide and discuss the corresponding confidence contours in the NS mass-radius plane. The measured effective temperature indicates that the NS is exceptionally hot for the estimated age of ∼30 kyr. We discuss possible cooling scenarios to explain this property, as well as possible additional constraints on the star mass and radius from cooling theory.

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Thermal Properties of the Middle-Aged Pulsar J1741–2054

Cited by 16 publications

References 25 publications

X-Ray Analysis of the Proper Motion and Pulsar Wind Nebula for PSR J1741-2054

X-Ray Analysis of the Proper Motion and Pulsar Wind Nebula for PSR J1741-2054

The γ-ray Pulsar J0633+0632 in X-rays

The neutron star in HESS J1731−347: Central compact objects as laboratories to study the equation of state of superdense matter

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