Discovery of Nearly Coherent Oscillations with a Frequency of ∼567 H[CLC]z[/CLC] during Type I X-Ray Bursts of the X-Ray Transient and Eclipsing Binary X1658−298

Wijnands, Rudy; Strohmayer, Tod E.; Franco, L.

doi:10.1086/319128

Cited by 58 publications

(75 citation statements)

References 24 publications

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“…- ( Strohmayer et al 1996;(11) van Straaten et al 2001;(12) Kaaret et al 2003;(13) Smith et al 1997;(14) Muno et al 2000, (15) Zhang et al 1998;(12) Cumming & Bildsten 2000;(13) Wijnands et al 2001;(18) Wijnands et al 2002;(19) Wijnands et al 2003;(20) Strohmayer et al 1998;(21) Miller 2000;(22) Strohmayer 1999;(23) Strohmayer et al 1997b;(24) Kaaret et al 2002;(25) Natalucci et al 1999;(26) Hartman et al 2003. predicted frequency drifts match the observed drifts, and (2) the final frequency is stable and characteristic to each object because it only depends on the crust's properties, which do not change from burst to burst.…”

Section: Nonradial Modes As Burst Oscillationsmentioning

confidence: 99%

Surface Modes on Bursting Neutron Stars and X‐Ray Burst Oscillations

Piro

Bildsten

2005

ApJ

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Accreting neutron stars (NSs) often show coherent modulations during type I X-ray bursts, called burst oscillations. We consider whether a nonradial mode can serve as an explanation for burst oscillations from those NSs that are not magnetic. We find that a surface wave in the shallow burning layer changes to a crustal interface wave as the envelope cools, a new and previously uninvestigated phenomenon. The surface modulations decrease dramatically as the mode switches, explaining why burst oscillations often disappear before burst cooling ceases. When we include rotational modifications, we find mode frequencies and drifts consistent with those observed. The large NS spin (%270-620 Hz) needed to make this match implies that accreting NSs are spinning at frequencies %4 Hz above the burst oscillation. Since the long-term stable asymptotic frequency is set by the crustal interface wave, the observed late-time frequency drifts are a probe of the composition and temperature of NS crusts. We compare our model with the observed drifts and persistent luminosities of X-ray burst sources and find that NSs with a higher average accretion rate show smaller drifts, as we predict. Furthermore, the drift sizes are consistent with crusts composed of iron-like nuclei, as expected for the ashes of the He-rich bursts that are exhibited by these objects.

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Section: Nonradial Modes As Burst Oscillationsmentioning

confidence: 99%

Surface Modes on Bursting Neutron Stars and X‐Ray Burst Oscillations

Piro

Bildsten

2005

ApJ

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“…In 1999 April, the source was detected after more then 20 yr of quiescence (inÏt Zand et al 1999). Observations of the source were obtained with the PCA on board the RXT E (e.g., Wachter, Smale, & Bailyn 2000 ;Wijnands, Strohmayer, & Franco 2001), with BeppoSAX , and with XMM-Newton (Sidoli et al 2001). With these observations, an updated orbital ephemeris was obtained by Wachter et al (2000) and Oosterbroek et al (2001).…”

Section: Mxb 1659[298mentioning

confidence: 99%

The Burst Behavior of the Eclipsing Low‐Mass X‐Ray Binary MXB 1659−298

Wijnands

Muno

Miller

et al. 2002

ApJ

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We present a detailed study of the correlations between the burst properties and the inferred mass accretion rate for the X-ray transient MXB 1659[298. The bursts that exhibited oscillations were observed when the source was at a relatively high mass accretion rate, similar to what has been seen for other sources. However, owing to the limited number of observations at lower mass accretion rates, no bursts were observed at such accretion rates, and it is still possible that when MXB 1659[298 accretes at such low-mass accretion rates, bursts can occur that might still exhibit burst oscillations. No clear correlations were found between the di †erent burst properties and the accretion rate, in contrast to what has been found for KS 1731[260 and 4U 1728[34, but similar to what has been reported for Aql X-1. However, this lack of correlation for MXB 1659[298 and Aql X-1 might be due to the limited range of the mass accretion rate observed for those sources compared to KS 1731[260 and 4U 1728[34.

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“…X-ray spectroscopy during burst rise also supports the inference that X-ray emission is localized on the neutron star near the onset of bursts. Strohmayer, Zhang, & Swank (1997) found that during burst rise the flux is underluminous compared with intervals later in the Strohmayer et al (1996); (2) Strohmayer, Zhang, & Swank (1997); (3) Mendez & van der Klis (1999); (4) ; (5) Strohmayer et al (1998b); (6) Strohmayer et al (1998a); (7) Miller (1999); (8) Mendez et al (1998); (9) Markwardt, Strohmayer & Swank (1999) (10) Smith, Morgan, & Bradt (1997); (11) Wijnands & van der Klis (1997); (12) Muno et al (2000); (13) van Straaten et al (2000); (14) Franco (2000); (15) ; (16) Zhang et al (1998); (17) Ford (1999); (18) Wijnands, Strohmayer & Franco (2000); (19) Boirin et al (2000); (20) Galloway et al (2000); (21) Chakrabarty (2000); (22) Heise (2000); (23) Ford (2000) burst which have the same observed black body temperature, suggesting that during th...…”

Section: Oscillations At Burst Onsetmentioning

confidence: 99%

“…They suggested that such a large change, ∼ 1.3% might be inconsistent with expansion of the thermonuclear burning layer because of the magnitude of the implied height change of ∼ 80 m. Wijnands, Strohmayer & Franco (2000) found a ∼ 5 Hz frequency shift in a burst from 4U 1658-298 with a 567 Hz oscillation, which may also be uncomfortably large given current estimate of the expansion of burning layers (Cumming & Bildsten 2000). Note, however, that the current theoretical estimates do not include the rotational lowering of the effective surface gravity and are also hydrostatic calculations.…”

Section: Coherence Of Burst Oscillationsmentioning

confidence: 99%

Oscillations during thermonuclear X-ray bursts: A new probe of neutron stars

Strohmayer¹

2001

AIP Conference Proceedings

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High amplitude, nearly coherent X-ray brightness oscillations during thermonuclear X-ray bursts were discovered with the Rossi X-ray Timing Explorer (RXTE) in early 1996. Spectral and timing evidence strongly supports the conclusion that these oscillations are caused by rotational modulation of the burst emission and that they reveal the spin frequency of neutron stars in low mass X-ray binaries, a long sought goal of X-ray astronomy. Studies carried out over the past year have led to the discovery of burst oscillations in four new sources, bringing to ten the number with confirmed burst oscillations. I review the status of our knowledge of these oscillations and indicate how they can be used to probe the physics of neutron stars. For a few burst oscillation sources it has been proposed that the strongest and most ubiquitous frequency is actually the first overtone of the spin frequency and hence that two nearly antipodal hot spots are present on the neutron star. This inference has important implications for both the physics of thermonuclear burning as well as the mass -radius relation for neutron stars, so its confirmation is crucial. I discuss recent attempts to confirm this hypothesis for 4U 1636-53, the source for which a signal at the putative fundamental (290 Hz) has been claimed. INTRODUCTIONSince its launch in December, 1995 NASA's Rossi X-ray Timing Explorer has provided astronomers with a fundamental new view of neutron stars, and in particular those which are accreting in binary systems. Since the discovery of rapidly rotating neutron stars as millisecond radio pulsars it has been suspected that neutron stars in low mass X-ray binaries (LMXB) are spun up to millisecond periods by the capture of angular momentum via mass transfer from an accretion disk. Efforts to confirm this hypothesis by detecting millisecond X-ray pulsars in LMXBs went unrewarded for many years. This situation changed dramatically with the advent of RXTE. Within a few months of its launch RXTE observations had provided strong evidence suggesting that neutron stars in LMXB are spinning with frequencies ≥ 300 Hz. These first indications came with the discovery of high frequency (millisecond) X-ray brightness oscillations, "burst oscillations," during thermonuclear (Type I) X-ray bursts from several neutron star LMXB systems (see Strohmayer et al. 1996;Smith, Morgan & Bradt 1997;Zhang et al. 1996).As of this writing burst oscillation detections have been claimed for a total of ten different LMXB systems, with four of these only appearing in the past few months (see Strohmayer et

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Discovery of Nearly Coherent Oscillations with a Frequency of ∼567 H[CLC]z[/CLC] during Type I X-Ray Bursts of the X-Ray Transient and Eclipsing Binary X1658−298

Cited by 58 publications

References 24 publications

Surface Modes on Bursting Neutron Stars and X‐Ray Burst Oscillations

Surface Modes on Bursting Neutron Stars and X‐Ray Burst Oscillations

The Burst Behavior of the Eclipsing Low‐Mass X‐Ray Binary MXB 1659−298

Oscillations during thermonuclear X-ray bursts: A new probe of neutron stars

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