GINGA observations of quasi-periodic oscillations in type II bursts from the Rapid Burster

Dotani, Tadayasu; Mitsuda, K.; Inoue, Hajime; Tanaka, Yasuyuki; Kawai, N.; Tawara, Yuzuru; Makishima, K.; Paradijs, J. van; Penninx, W.; Klis, M. van der; Tan, J.; Lewin, W. H. G.

doi:10.1086/168393

Cited by 22 publications

(33 citation statements)

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“…This may be related to the weak magnetic Ðeld. Presence of two accreting paths is also suspected in the other type II burster, the Rapid Burster, based on the observations of quasi-periodic oscillations (Dotani et al 1990). Two accretion paths may, therefore, be common to neutron stars that produce type II bursts.…”

Section: T He Pulsed Emissionmentioning

confidence: 99%

ASCAObservations of GRO J1744−28

Nishiuchi

Koyama

Maeda

et al. 1999

ApJ

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We report the ASCA results of the bursting X-ray pulsar GRO J1744[28, which was observed in 1996 February and 1997 March. The source Ñux in the 2È10 keV band was 2.0 ] 10~8 ergs s~1 cm2 in 1996 and 5.0 ] 10~9 ergs s~1 cm2 in 1997. We detected 12 and 17 type II bursts during the two observations, with mean bursting intervals of about 27 min and 37 min. Each burst is followed by an intensity dip with the depleted Ñux depending on the burst Ñuence. The energy spectra are approximated by an absorbed power law with additional structure around 6È7 keV. The constant absorption column, (5È 6) ] 1022 cm~2, independent of the observation dates and emission phases (persistent, burst, and dip) is interpreted as an interstellar absorption. The source may be actually located near the Galactic center, at a distance of 8.5 kpc. The structure in the energy spectrum at 6È7 keV is most probably due to iron and may be reproduced by a disk line model with additional broadening mechanism.

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Section: T He Pulsed Emissionmentioning

confidence: 99%

ASCAObservations of GRO J1744−28

Nishiuchi

Koyama

Maeda

et al. 1999

ApJ

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“…Quasi-periodic oscillations (QPO) in the range 12-7 Hz have been observed in the type II bursts and in the persistent emission between the bursts; their behavior is very complex (Tawara et al 1982; Stella et al 1988a, b;Dotani et al 1990;Lubin et al 1991;Rutledge et al 1995; LVT93; LVT95). Dotani et al (1990) showed that during the type II bursts the oscillations are due to a periodic modulation without phase jumps whose frequency changes by up to 125%.…”

Section: L39mentioning

confidence: 99%

“…Dotani et al (1990) showed that during the type II bursts the oscillations are due to a periodic modulation without phase jumps whose frequency changes by up to 125%. The frequency shifts can explain the width of the QPO peaks in the power density spectra.…”

Section: L39mentioning

confidence: 99%

“…In 1985 August, the type II burst spectra were harder than the average spectrum of the persistent emission between the bursts (Stella et al 1988b). Very globally, the spectrum of the persistent emission was very soft during the ''dip'' just after a burst, then it rapidly increased in hardness, after which it gradually decreased to become very soft again during the ''dip'' just prior to the next burst.Quasi-periodic oscillations (QPO) in the range 12-7 Hz have been observed in the type II bursts and in the persistent emission between the bursts; their behavior is very complex (Tawara et al 1982; Stella et al 1988a, b;Dotani et al 1990;Lubin et al 1991;Rutledge et al 1995; LVT93; LVT95). Dotani et al (1990) showed that during the type II bursts the oscillations are due to a periodic modulation without phase jumps whose frequency changes by up to 125%.…”

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A Comparison between the Rapid Burster and GRO J1744–28

Lewin

Rutledge

Kommers

et al. 1996

ApJ

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A comparison between the rapid burster and GRO J1744-28Lewin, W.H.G.; Rutledge, R.E.; Kommers, J.M.; van Paradijs, J.A.; Kouveliotou, C. General rightsIt is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: http://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. ABSTRACT Twenty years ago, the Rapid Burster (MXB 1730Ϫ335) was discovered. Its most salient feature was the occurrence of rapidly repetitive type II X-ray bursts, the release of gravitational potential energy due to spasmodic accretion onto a compact object. This is almost certainly due to an accretion disk instability whose origin is still not understood. With the recent appearance of GRO J1744Ϫ28, the Rapid Burster is no longer the only system to produce such bursts. Both systems are transient low-mass X-ray binaries in which the accretor is a neutron star. The Rapid Burster, located in a globular cluster, also produces type I bursts which are due to thermonuclear flashes on the neutron star's surface; no X-ray pulsations are observed. Its neutron star magnetic field is therefore relatively weak. In contrast, strong X-ray pulsations have been observed in the persistent flux as well as in the type II bursts from GRO J1744Ϫ28, but no type I bursts have been observed. Thus, the magnetic field of the neutron star in this system is probably stronger than is the case of the Rapid Burster. The fact that type II bursts occur in both systems may bring us closer to an understanding of the mechanism(s?) that produces them. Subject headings: stars: neutron -X-rays: general -X-rays: bursts THE RAPID BURSTERThe Rapid Burster (MXB 1730Ϫ335) was discovered in March of 1976 during observations with the SAS 3 observatory (Lewin et al. 1976). Extensive reviews of this source and its complex behavior are given by Lewin, Van Paradijs, & Taam (1993, 1995; these two reviews are hereafter referred to as LVT93, LVT95. We mention here some of the most salient features of the Rapid Burster and refer the reader largely to LVT93 and LVT95 for references.The Rapid Burster is located at a distance of 110 kpc in the highly reddened globular cluster Liller 1. It is a low-mass X-ray binary and a recurrent transient. There are 1125 known low-mass X-ray binaries (van Paradijs 1995), all produce a persistent flux of X-rays, the result of a release of gravitational potential energy. Approximately 40 of them also ex...

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“…Phenomena probably related to QPOs occur in (a) the black hole candidate system LMC X-1 [208], (b) the 1983 August 1 gamma ray burster [209], (c) the rapid burster [210], and (d) several massive …”

Section: Quasi-periodic Oscillations (Qpos)mentioning

confidence: 99%