Nondetection of Gravitationally Redshifted Absorption Lines in the X-Ray Burst Spectra of GS 1826-24

Kong, Albert; Miller, J. M.; Méndez, Mariano; Cottam, J.; Lewin, W. H. G.; Paerels, F.; Kuulkers, E.; Wijnands, Rudy; Klis, M. van der

doi:10.1086/524137

Cited by 23 publications

(23 citation statements)

References 21 publications

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“…129 A long observation of the regular bursting source GS 1826-24 also failed to detect any absorption lines. 130 Recent, more encouraging results include the observation, albeit with limited spectral resolution, of absorption edges from Fe-peak elements in photospheric radius "superexpansion" bursts. 131 Higher spectral resolution observations of these superexpansion bursts (e.g., with Chandra 132 or XMM-Newton, 127 though an exposure time of ≈500 ks may be necessary) would be of great interest.…”

Section: A Absorption Features In X-ray Burstsmentioning

confidence: 99%

Classical novae and type I X-ray bursts: Challenges for the 21st century

2014

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Classical nova explosions and type I X-ray bursts are the most frequent types of thermonuclear stellar explosions in the Galaxy. Both phenomena arise from thermonuclear ignition in the envelopes of accreting compact objects in close binary star systems. Detailed observations of these events have stimulated numerous studies in theoretical astrophysics and experimental nuclear physics. We discuss observational features of these phenomena and theoretical efforts to better understand the energy production and nucleosynthesis in these explosions. We also examine and summarize studies directed at identifying nuclear physics quantities with uncertainties that significantly affect model predictions.

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Section: A Absorption Features In X-ray Burstsmentioning

confidence: 99%

Classical novae and type I X-ray bursts: Challenges for the 21st century

2014

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“…Therefore, the surface origin of the observed absorption features from EXO 0748-676 is not established yet. Besides, Kong et al (2007) did not find surface spectral lines from the combined XMM-Newton RGS spectra of 16 thermonuclear bursts from the neutron star LMXB GS 1826-24.…”

Section: Spectral Line Methodsmentioning

confidence: 86%

Measurement of neutron star parameters: A review of methods for low-mass X-ray binaries

Bhattacharyya

2010

Advances in Space Research

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Measurement of at least three independent parameters, for example, mass, radius and spin frequency, of a neutron star is probably the only way to understand the nature of its supranuclear core matter. Such a measurement is extremely difficult because of various systematic uncertainties. The lack of knowledge of several system parameter values gives rise to such systematics. Low mass X-ray binaries, which contain neutron stars, provide a number of methods to constrain the stellar parameters. Joint application of these methods has a great potential to significantly reduce the systematic uncertainties, and hence to measure three independent neutron star parameters accurately. Here we review the methods based on (1) thermonuclear X-ray bursts; (2) accretion-powered millisecond-period pulsations; (3) kilohertz quasi-periodic oscillations; (4) broad relativistic iron lines; (5) quiescent emissions; and (6) binary orbital motions.

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“…Several attempts in this direction have been made (e.g. Kong et al 2007;Galloway et al 2010b;in 't Zand et al 2013in 't Zand et al , 2017, but only in one case narrow spectral features were claimed to be seen (Cottam et al 2002). However, the later discovery of a high spin rate for this particular neutron star (552 Hz; Galloway et al 2010a) rules out that the putative lines originated from the stellar atmosphere (Lin et al 2010).…”

Section: Gravitationally Redshifted Lines and Edges During X-ray Burstsmentioning

confidence: 99%

Testing the Equation of State with Electromagnetic Observations

Degenaar

Suleimanov

2018

Astrophysics and Space Science Library

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Neutron stars are the densest, directly observable stellar objects in the universe and serve as unique astrophysical laboratories to study the behavior of matter under extreme physical conditions. This book chapter is devoted to describing how electromagnetic observations, particularly at X-ray, optical and radio wavelengths, can be used to measure the mass and radius of neutron stars and how this leads to constraints on the equation of state of ultra-dense matter. Having accurate theoretical models to describe the astrophysical data is essential in this effort. We will review different methods to constrain neutron star masses and radii, discuss the main observational results and theoretical developments achieved over the past decade, and provide an outlook of how further progress can be made with new and upcoming ground-based and space-based observatories.

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Nondetection of Gravitationally Redshifted Absorption Lines in the X-Ray Burst Spectra of GS 1826-24

Cited by 23 publications

References 21 publications

Classical novae and type I X-ray bursts: Challenges for the 21st century

Classical novae and type I X-ray bursts: Challenges for the 21st century

Measurement of neutron star parameters: A review of methods for low-mass X-ray binaries

Testing the Equation of State with Electromagnetic Observations

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