Model atmospheres for X-ray bursting neutron stars

London, Richard A.; Taam, R. E.; Howard, W. M.

doi:10.1086/164330

Cited by 124 publications

(141 citation statements)

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“…These model spectra describe the observed X-ray spectra of X-ray bursting NSs in Low-Mass X-ray Binaries (LMXBs), and they are close to diluted blackbody spectra with a hardness factor f c ∼ 1.5 -1.9 (London et al 1986;Lapidus et al 1986, Madej 1991Pavlov et al 1991). But these model atmospheres with Compton scattering taken into account are not calculated for relatively cool atmospheres with T eff < 10 MK.…”

Section: Introductionsupporting

confidence: 59%

“…It is well known that the Compton down-scattering determines the shape of emergent model spectra of hotter NS atmospheres with T eff ∼ 20 MK and close to Eddington limit (London et al 1986;Lapidus et al 1986;Ebisuzaki 1987). These model spectra describe the observed X-ray spectra of X-ray bursting NSs in Low-Mass X-ray Binaries (LMXBs), and they are close to diluted blackbody spectra with a hardness factor f c ∼ 1.5 -1.9 (London et al 1986;Lapidus et al 1986, Madej 1991Pavlov et al 1991).…”

Section: Introductionmentioning

confidence: 97%

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Importance of Compton scattering for radiation spectra of isolated neutron stars

Suleimanov

Werner

2007

Astrophys Space Sci

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Abstract. Model atmospheres of isolated neutron stars with low magnetic field are calculated with Compton scattering taking into account. Models with effective temperatures 1, 3 and 5 MK, with two values of surface gravity (log g = 13.9 and 14.3), and different chemical compositions are calculated. Radiation spectra computed with Compton scattering are softer than the computed with Thomson scattering at high energies (E> 5 keV) for hot (T eff > 1 MK) atmospheres with hydrogen-helium composition. Compton scattering is more significant to hydrogen models with low surface gravity. The emergent spectra of the hottest (T eff > 3 MK) model atmospheres can be described by diluted blackbody spectra with hardness factors ∼ 1.6 -1.9. Compton scattering is less important for models with solar abundance of heavy elements.

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Section: Introductionsupporting

confidence: 59%

Section: Introductionmentioning

confidence: 97%

Importance of Compton scattering for radiation spectra of isolated neutron stars

Suleimanov

Werner

2007

Astrophys Space Sci

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“…Electron scattering dominates the opacity in the neutron star atmosphere, leading to deviations from the original Planckian spectrum (van Paradijs 1982;London et al 1984London et al , 1986see also Titarchuk 1994;Madej 1997, and references therein). Similarly, electron scattering in a disk corona (e.g.…”

Section: Type I X-ray Burstsmentioning

confidence: 99%

Photospheric radius expansion X-ray bursts as standard candles

Kuulkers

Hartog

Zand³

et al. 2003

A&A

366

448

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Abstract. We examined the maximum bolometric peak luminosities during type I X-ray bursts from the persistent or transient luminous X-ray sources in globular clusters. We show that for about two thirds of the sources the maximum peak luminosities during photospheric radius expansion X-ray bursts extend to a critical value of 3.79±0.15×10 38 erg s −1 , assuming the total X-ray burst emission is entirely due to black-body radiation and the recorded maximum luminosity is the actual peak luminosity. This empirical critical luminosity is consistent with the Eddington luminosity limit for hydrogen poor material. Since the critical luminosity is more or less always reached during photospheric radius expansion X-ray bursts (except for one source), such bursts may be regarded as empirical standard candles. However, because significant deviations do occur, our standard candle is only accurate to within 15%. We re-evaluated the distances to the twelve globular clusters in which the X-ray bursters reside.

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“…After 70 s the flux starts to decrease, signifying the end of the Eddington-limited phase. At that time the spectrum shows a hardening lasting approximately 40 s, which may be caused by Comptonization of the thermal photons against a hot receding atmosphere (London et al 1986;Madej et al 2004). The simultaneous radius measurements are most probably biased by this systematic effect and do not represent true variations of the photospheric size.…”

Section: Spectramentioning

confidence: 99%

Achromatic late-time variability in thermonuclear X-ray bursts

Zand

Ballantyne

2010

A&A

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An unusual Eddington-limited thermonuclear X-ray burst was detected from the accreting neutron star in 2S 0918-549 with the Rossi X-ray Timing Explorer. The burst commenced with a brief (40 ms) precursor and maintained near-Eddington fluxes during the initial 77 s. These characteristics are indicative of a nova-like expulsion of a shell from the neutron star surface. Starting 122 s into the burst, the burst shows strong (87 ± 1% peak-to-peak amplitude) achromatic fluctuations for 60 s. We speculate that the fluctuations are caused by Thompson scattering by fully-ionized inhomogeneities in a resettling accretion disk that was disrupted by the effects of super-Eddington fluxes. An expanding shell may be the necessary prerequisite for the fluctuations.

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Model atmospheres for X-ray bursting neutron stars

Cited by 124 publications

References 0 publications

Importance of Compton scattering for radiation spectra of isolated neutron stars

Importance of Compton scattering for radiation spectra of isolated neutron stars

Photospheric radius expansion X-ray bursts as standard candles

Achromatic late-time variability in thermonuclear X-ray bursts

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