Model Atmospheres of Magnetic Neutron Stars

Shibanov, Yu. A.; Zavlin, V. E.; Pavlov, G. G.; Ventura, J.

doi:10.1007/978-94-011-0159-2_9

Cited by 73 publications

(106 citation statements)

References 3 publications

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“…Our method of calculation has been tested by a comparison to models for magnetized NS atmospheres (Shibanov et al 1992;Pavlov et al 1994;Ho & Lai 2001;Özel 2001;. Model atmospheres with partially ionized hydrogen are compared to models computed by Ho et al (2007).…”

Section: Methods Of Atmosphere Structure Calculationsmentioning

confidence: 99%

Models of magnetized neutron star atmospheres: thin atmospheres and partially ionized hydrogen atmospheres with vacuum polarization

Suleimanov

Potekhin

Werner

2009

A&A

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Context. Observed X-ray spectra of some isolated magnetized neutron stars display absorption features, sometimes interpreted as ion cyclotron lines. Modeling the observed spectra is necessary to check this hypothesis and to evaluate neutron star parameters. Aims. We develop a computer code for modeling magnetized neutron star atmospheres in a wide range of magnetic fields (10 12 −10 15 G) and effective temperatures (3 × 10 5 −10 7 K). Using this code, we study the possibilities to explain the soft X-ray spectra of isolated neutron stars by different atmosphere models. Methods. The atmosphere is assumed to consist either of fully ionized electron-ion plasmas or of partially ionized hydrogen. Vacuum resonance and partial mode conversion are taken into account. Any inclination of the magnetic field relative to the stellar surface is allowed. We use modern opacities of fully or partially ionized plasmas in strong magnetic fields and solve the coupled radiative transfer equations for the normal electromagnetic modes in the plasma. Results. Spectra of outgoing radiation are calculated for various atmosphere models: fully ionized semi-infinite atmosphere, thin atmosphere, partially ionized hydrogen atmosphere, or novel "sandwich" atmosphere (thin atmosphere with a hydrogen layer above a helium layer). Possibilities of applications of these results are discussed. In particular, the outgoing spectrum using the "sandwich" model is constructed. Thin partially ionized hydrogen atmospheres with vacuum polarization are shown to be able to improve the fit to the observed spectrum of the nearby isolated neutron star RBS 1223 (RX J1308.8+2127).

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Section: Methods Of Atmosphere Structure Calculationsmentioning

confidence: 99%

Models of magnetized neutron star atmospheres: thin atmospheres and partially ionized hydrogen atmospheres with vacuum polarization

Suleimanov

Potekhin

Werner

2009

A&A

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“…5.6 Spectra of magnetic atmospheres Shibanov et al (1992) calculated spectra from strongly magnetized NS atmospheres, which was assumed to be fully ionized. Later they created a database of model spectra and included it in the XSPEC package (Arnaud 1996) under the name NSA.…”

Section: Bound-bound and Bound-free Transitionsmentioning

confidence: 99%

Neutron Stars—Thermal Emitters

2014

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Confronting theoretical models with observations of thermal radiation emitted by neutron stars is one of the most important ways to understand the properties of both, superdense matter in the interiors of the neutron stars and dense magnetized plasmas in their outer layers. Here we review the theory of thermal emission from the surface layers of strongly magnetized neutron stars, and the main properties of the observational data. In particular, we focus on the nearby sources for which a clear thermal component has been detected, without being contaminated by other emission processes (magnetosphere, accretion, nebulae). We also discuss the applications of the modern theoretical models of the formation of spectra of strongly magnetized neutron stars to the observed thermally emitting objects.

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“…In the early models of magnetized neutron star atmospheres (e.g., Pavlov & Shibanov 1978;Shibanov et al 1992;, the authors considered moderate magnetic fields B ∼ 10 11 -10 12 G, where the proton Landau quantization is unimportant. More recently, observational evidence has accumulated that some of the isolated neutron stars are probably magnetars, which have fields of B ∼ 10 14 G (see, e.g., the review by Mereghetti 2008 and references therein).…”

Section: Proton Cyclotron Harmonicsmentioning

confidence: 99%

Cyclotron harmonics in opacities of isolated neutron star atmospheres

Potekhin

2010

A&A

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Some X-ray dim isolated neutron stars (XDINS) and central compact objects in supernova remnants (CCO) contain absorption features in their thermal soft X-ray spectra. It has been hypothesized that this absorption may relate to periodic peaks in free-free absorption opacities, caused by either Landau quantization of electron motion in magnetic fields B < ∼ 10 11 G or analogous quantization of ion motion in magnetic fields B > 10 13 G. Here, I review the physics behind cyclotron quantum harmonics in free-free photoabsorption, discuss different approximations for their calculation, and explain why the ion cyclotron harmonics (beyond the fundamental) cannot be observed.

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Model Atmospheres of Magnetic Neutron Stars

Cited by 73 publications

References 3 publications

Models of magnetized neutron star atmospheres: thin atmospheres and partially ionized hydrogen atmospheres with vacuum polarization

Models of magnetized neutron star atmospheres: thin atmospheres and partially ionized hydrogen atmospheres with vacuum polarization

Neutron Stars—Thermal Emitters

Cyclotron harmonics in opacities of isolated neutron star atmospheres

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