Neutron Star Atmospheres

Pavlov, G. G.; Shibanov, Yu. A.; Zavlin, V. E.; Meyer, R. D.

doi:10.1007/978-94-011-0159-2_8

Cited by 131 publications

(61 citation statements)

References 24 publications

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“…The observed part of the spectrum decreases with E slower than the ideal Wien spectrum because the radiation at higher energies comes from hotter layers (the H opacity strongly decreases with frequency). As a result, BB fits to the H atmosphere spectra give a temperature higher than the true effective temperature and an area smaller than the true emitting area (e.g., Pavlov et al 1995). If we adopt the H atmosphere hypothesis, the effective temperature of the Vela pulsar is below the predictions of the so-called standard models of the NS cooling (e.g., Tsuruta 1998), even if the pulsar is a factor of 2-3 older than its characteristic age (Lyne et al 1996).…”

Section: Discussionmentioning

confidence: 99%

“…The temperature and luminosity inferred from the BB fit correspond to an effective radius of emitting region about 1.3 km at a distance pc (Cha, Sembach, & Danks 1999 temperature, 1.3 MK, a larger radius, 3 km at 250 pc, and a surprisingly small photon index, (Ö gelman 1995). g ∼ 0.1 Page, Shibanov, & Zavlin (1996) fitted the same spectrum with the NS hydrogen atmosphere models (Pavlov et al 1995) and obtained a lower effective temperature and a larger :…”

mentioning

confidence: 86%

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The X-Ray Spectrum of the Vela Pulsar Resolved with the [ITAL]Chandra X-Ray Observatory[/ITAL]

Pavlov

Zavlin

Sanwal

et al. 2001

The Astrophysical Journal

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172

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We report the results of the spectral analysis of two observations of the Vela pulsar with the Chandra X-Ray Observatory. The spectrum of the pulsar does not show statistically significant spectral lines in the observed 0.25-8.0 keV band. Similar to middle-aged pulsars with detected thermal emission, the spectrum consists of two distinct components. The softer component can be modeled as a magnetic hydrogen atmosphere spectrum-for the pulsar magnetic field G and neutron star mass and radius km, we

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Section: Discussionmentioning

confidence: 99%

mentioning

confidence: 86%

The X-Ray Spectrum of the Vela Pulsar Resolved with the [ITAL]Chandra X-Ray Observatory[/ITAL]

Pavlov

Zavlin

Sanwal

et al. 2001

The Astrophysical Journal

Self Cite

208

172

View full text Add to dashboard Cite

show abstract

“…Spectra were grouped to ensure > 15 counts per energy bin and then fitted simultaneously in the 0.3-10 keV range. Assuming the NS origin of J1726, we applied the absorbed power law (PL), power law plus blackbody (PL+BB) and power law plus the magnetized hydrogen atmosphere (PL+NSA; Pavlov et al 1995) models. The PL component describes the magnetospheric emission while BB or NSA refer to the thermal emission from the NS surface.…”

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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“…Neutron star atmospheres have been studied theoretically by many authors (see, e.g., review papers by Pavlov et al 1995, Pavlov and, and references therein). Construction of the atmosphere models, especially for cold stars with the effective surface temperature T s < ∼ 10 6 K and strong magnetic fields 10 11 -10 14 G, is incomplete owing to serious theoretical problems concerned with the calculation of the equation of state and spectral opacity of the atmospheric plasma.…”

Section: Structure Of Neutron Starsmentioning

confidence: 99%

Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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We review the main neutrino emission mechanisms in neutron star crusts and cores. Among them are the well-known reactions such as the electron-positron annihilation, plasmon decay, neutrino bremsstrahlung of electrons colliding with atomic nuclei in the crust, as well as the Urca processes and neutrino bremsstrahlung in nucleon-nucleon collisions in the core. We emphasize recent theoretical achievements, for instance, band structure effects in neutrino emission due to scattering of electrons in Coulomb crystals of atomic nuclei. We consider the standard composition of matter (neutrons, protons, electrons, muons, hyperons) in the core, and also the case of exotic constituents such as the pion or kaon condensates and quark matter. We discuss the reduction of the neutrino emissivities by nucleon superfluidity, as well as the specific neutrino emission produced by Cooper pairing of the superfluid particles. We also analyze the effects of strong magnetic fields on some reactions, such as the direct Urca process and the neutrino synchrotron emission of electrons. The results are presented in the form convenient for practical use. We illustrate the effects of various neutrino reactions on the cooling of neutron stars. In particular, the neutrino emission in the crust is critical in setting the initial thermal relaxation between the core and the crust. Finally, we discuss the prospects of exploring the properties of supernuclear matter by confronting cooling simulations with observations of the thermal radiation from isolated neutron stars.

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Neutron Star Atmospheres

Cited by 131 publications

References 24 publications

The X-Ray Spectrum of the Vela Pulsar Resolved with the [ITAL]Chandra X-Ray Observatory[/ITAL]

The X-Ray Spectrum of the Vela Pulsar Resolved with the [ITAL]Chandra X-Ray Observatory[/ITAL]

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

Neutrino emission from neutron stars

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