Evidence of 1122 Hz X-Ray Burst Oscillations from the Neutron Star X-Ray Transient XTE J1739-285

Kaaret, Philip; Prieskorn, Zachary; Zand, J. J. M. in ’t; Brandt, S.; Lund, N.; Mereghetti, S.; Götz, D.; Kuulkers, E.; Tomsick, John A.

doi:10.1086/513270

Cited by 133 publications

(170 citation statements)

References 17 publications

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“…Rotational frequencies below millisecond are hard to be explained by a regular neutron star. An example of such a case is XTE J1739-285, which allegedly rotates with a frequency of 1122Hz [86]. Any odd looking neutron star is a potential candidate for an asymmetric dark star.…”

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confidence: 99%

Asymmetric dark matter stars

2015

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We study the possibility of asymmetric dark matter with self-interactions forming compact stable objects. We solve the Tolman-Oppenheimer-Volkoff equation and find the mass-radius relation of such "dark stars", their density profile and their Chandrasekhar mass limit. We consider fermionic asymmetric dark matter with Yukawa-type self-interactions appropriate for solving the well known problems of the collisionless dark matter paradigm. We find that in several cases the relativistic effects are significant.

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confidence: 99%

Asymmetric dark matter stars

2015

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“…Evidence for a burst oscillation at > 1000 Hz has already been reported, although the low significance of the signal means that it must be considered a candidate, at best. A peak at 1122 Hz was detected in the power-density spectrum of a 4-s interval late in the tail of a thermonuclear burst from the LMXB transient XTE J1739−285 [24]. However, no comparable power excess was detected at this frequency in other (nonoverlapping) intervals during the burst, nor in any of the other six bursts observed by RXTE.…”

Section: Burst Oscillationsmentioning

confidence: 89%

Accreting neutron star spins and the equation of state

Galloway,

Bassa,

Wang

et al. 2008

AIP Conference Proceedings

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Abstract. X-ray timing of neutron stars in low-mass X-ray binaries (LMXBs) with the Rossi X-ray Timing Explorer has since 1996 revealed several distinct high-frequency phenomena. Among these are oscillations during thermonuclear (type-I) bursts, which (in addition to persistent X-ray pulsations) are thought to trace the neutron star spin. The recent discoveries of 294 Hz burst oscillations in IGR J17191−2821, and 182 Hz pulsations in Swift J1756.9−2508, brings the total number of measured LMXB spin rates to 22. An open question is why the majority of the ≈ 100 known neutron stars in LMXBs show neither pulsations nor burst oscillations.Recent observations suggest that persistent pulsations may be more common than previously thought, although detectable intermittently, and in some cases at very low duty cycles. For example, the 377.3 Hz pulsations in HETE J1900.1−2455 were only present in the first few months of it's outburst, and have been absent since (although X-ray activity continues). Intermittent (persistent) pulsations have since been detected in a further two sources. In two of these three systems the pulsations appear to be related to the thermonuclear burst activity, but in the third (Aql X-1) they are not. This phenomenon offers new opportunities for spin measurements in known systems.Such measurements can constrain the poorly-known neutron star equation of state, and neutron stars in LMXBs offer observational advantages over rotation-powered pulsars which make the detection of more rapidly-spinning examples more likely. Even so, spin rates of at least 50% faster than the present maximum appear necessary to give constraints stringent enough to discriminate between the various models. Although the future prospects for such rapidly-spinning objects do not appear optimistic, several additional observational approaches are possible for LMXBs. The recent study of EXO 0748−676 is an example.

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“…In particular, the number of MSPs with spin frequencies > 620 Hz [20] may be small because the equilibrium spin rates of these stars are < 620 Hz or because their spin-up timescales are longer than their accretion phases. As an example, the timescale to reach the 1122 Hz spin frequency reported for XTE J1739−285 [43] is 400 Myr for a long-term average accretion rate of 10 −2Ṁ E and 3 Gyr for an accretion rate of 10 −3Ṁ E . The ranges of magnetic fields and accretion rates required are consistent with the other observed properties of neutron stars in LMXBs [69,78,20].…”

Section: Production Of Millisecond Pulsarsmentioning

confidence: 99%

Accreting Neutron Stars in Low-Mass X-Ray Binary Systems

Lamb

Boutloukos

2008

Astrophysics and Space Science Library

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Summary. Using the Rossi X-ray Timing Explorer (RossiXTE), astronomers have discovered that disk-accreting neutron stars with weak magnetic fields produce three distinct types of high-frequency X-ray oscillations. These oscillations are powered by release of the binding energy of matter falling into the strong gravitational field of the star or by the sudden nuclear burning of matter that has accumulated in the outermost layers of the star. The frequencies of the oscillations reflect the orbital frequencies of gas deep in the gravitational field of the star and/or the spin frequency of the star. These oscillations can therefore be used to explore fundamental physics, such as strong-field gravity and the properties of matter under extreme conditions, and important astrophysical questions, such as the formation and evolution of millisecond pulsars. Observations using RossiXTE have shown that some two dozen neutron stars in low-mass X-ray binary systems have the spin rates and magnetic fields required to become millisecond radio-emitting pulsars when accretion ceases, but that few have spin rates above about 600 Hz. The properties of these stars show that the paucity of spin rates greater than 600 Hz is due in part to the magnetic braking component of the accretion torque and to the limited amount of angular momentum that can be accreted in such systems. Further study will show whether braking by gravitational radiation is also a factor. Analysis of the kilohertz oscillations has provided the first evidence for the existence of the innermost stable circular orbit around dense relativistic stars that is predicted by strong-field general relativity. It has also greatly narrowed the possible descriptions of ultradense matter.

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Evidence of 1122 Hz X-Ray Burst Oscillations from the Neutron Star X-Ray Transient XTE J1739-285

Cited by 133 publications

References 17 publications

Asymmetric dark matter stars

Asymmetric dark matter stars

Accreting neutron star spins and the equation of state

Accreting Neutron Stars in Low-Mass X-Ray Binary Systems

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