Quasi-regular X-Ray Bursts from GRS 1915+105 Observed with the IXAE: Possible Evidence for Matter Disappearing into the Event Horizon of the Black Hole

Paul, Biswajit; Agrawal, P. C.; Rao, A. R.; Vahia, M. N.; Yadav, J. S.; Seetha, S.; Kasturirangan, K.

doi:10.1086/311087

Cited by 54 publications

(30 citation statements)

References 21 publications

(26 reference statements)

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“…Figure 18 compares two simultaneous segments of the MECS and PDS of the E5 series containing six bursts. As already found by Paul et al (1998), bursts in both series occur at the same times, but those in the PDS are systematically narrower than those at lower energies. This effect cannot be entirely caused by the poorer S/N ratio of PDS data, as is clearly evident, for example, from the burst occurring at 180 s or that at 350 s. Moreover, PDS pulses appear generally at the end of the MECS bursts and this finding is in agreement with the spectral hardening in the course of the bursts.…”

Section: Energy Dependence Of the Bursts' Structuresupporting

confidence: 83%

“…Other RXTE observations of the same class were described by Vilhu & Nevalainen (1998), Paul et al (1998), and Yadav et al (1999), who presented the results of a long pointing of GRS 1915+105 performed in June 1997 with the IXAE onboard the IRS-P3 satellite. On that occasion the source was in the ρ class for about five days, then changed to the κ class in which it remained for a similar time and afterwards returned to the former one.…”

Section: Introductionmentioning

confidence: 87%

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The complex behaviour of the microquasar GRS 1915+105 in theρclass observed with BeppoSAX

Massaro¹,

Ventura

Massa

et al. 2010

A&A

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GRS 1915+105 was observed byBeppoSAX for about 10 days in October 2000. For about 80% of the time, the source was in the variability class ρ, characterised by a series of recurrent bursts. We describe the results of the timing analysis performed on the MECS (1.6-10 keV) and PDS (15-100 keV) data. The X-ray count rate from GRS 1915+105 showed an increasing trend with different characteristics in the various energy bands: in the bands (1.6-3 keV) and (15-100 keV), it was nearly stable in the first part of the pointing and increased in a rather short time by about 20%, while in the energy range (3-10 keV) the increase had a smoother trend. Fourier and wavelet analyses detect a variation in the recurrence time of the bursts, from 45-50 s to about 75 s, which appear well correlated with the count rate. From the power distribution of peaks in Fourier periodograms and wavelet spectra, we distinguished between the regular and irregular variability modes of the ρ class, which are related to variations in the count rate in the 3-10 keV range. We identified two components in the burst structure: the slow leading trail, and the pulse, superimposed on a rather stable level. Pulses are generally structured in a series of peaks and their number is related to the regularity modes: the mean number of peaks is lower than 2 in the regular mode and increases up to values higher than 3 in the irregular mode. We found that the change in the recurrence time of the regular mode is caused by the slow leading trails, while the duration of the pulse phase remains far more stable. The evolution in the mean count rates shows that the time behaviour of both the leading trail and the baseline level are very similar to those observed in the 1.6-3 and 15-100 keV ranges, while that of the pulse follows the peak number. These differences in the time behaviour and count rates at different energies indicate that the process responsible for the pulses must produce the strongest emission between 3 and 10 keV, while that associated with both the leading trail and the baseline dominates at lower and higher energies.

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Section: Energy Dependence Of the Bursts' Structuresupporting

confidence: 83%

Section: Introductionmentioning

confidence: 87%

The complex behaviour of the microquasar GRS 1915+105 in theρclass observed with BeppoSAX

Massaro¹,

Ventura

Massa

et al. 2010

A&A

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“…The most striking features of these bursts are slow exponential rise, sharp linear decay and hardening of spectrum as burst progresses (Paul et al 1998). The decay time scales are shorter than the rise time scales.…”

Section: Resultsmentioning

confidence: 99%

X-ray bursts from the galactic X-ray transient source GRS 1915+105

Yadav¹,

Rao²

2001

Advances in Space Research

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We have analyzed publicly available RXTE/PCAs archival data of GRS 1915+105 during its burst/flaring state. The burst cycle ranges from 30 to 1300 s. These bursts are different from the type I and type II classical bursts seen in Low Mass X-ray Binaries (LMXBs) in terms of their temporal and spectral properties. We have classified these bursts on the basis of properties observed during the quiescent (low flux) phase. The 2 -10 Hz QPOs are present during the quiescent phase and disappear during the burst phase of all types of these X-ray bursts. The duration of the quiescent phase can be explained assuming an outflow from the post-shock regions and the catastrophic Compton cooling.

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“…Observations and theoretical interpretations of broad X-ray lines (particularly, the iron K α line) in AGNs are actively discussed in a number of papers (Yaqoob et al, 1996;Wanders et al, 1997;Sulentic et al, 1998a,b;Paul et al, 1998;Bianchi & Matt, 2002;Turner et al, 2002;Levenson et al, 2002). The results of numerical simulations are also presented in the framework of different physical assumptions on the origin of the broad emissive iron K α line in the nuclei of Seyfert galaxies (Matt et al, 1992a,b;Bromley et al, 1997;Pariev & Bromley, 1997, 1998Cui et al, 1998;Bromley et al, 1998;Pariev et al, 2001;Ma, 2003Ma, , 2002bKaras et al, 2001b).…”

Section: Introductionmentioning

confidence: 99%

The iron Kα lines as a tool for magnetic field estimations in non-flat accretion flows

John¹,

Bao²

2004

New Astronomy

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Observations of AGNs and microquasars by ASCA, RXTE, Chandra and XMM-Newton indicate the existence of broad X-ray emission lines of ionized heavy elements in their spectra. Such spectral lines were discovered also in X-ray spectra of neutron stars and X-ray afterglows of GRBs. Recently, Zakharov et al. (2003) described a procedure to estimate an upper limit of the magnetic fields in regions from which X-ray photons are emitted. The authors simulated typical profiles of the iron Kα line in the presence of magnetic field and compared them with observational data in the framework of the widely accepted accretion disk model. Here we further consider typical Zeeman splitting in the framework of a model of non-flat accretion flows, which is a generalization of previous consideration into non-equatorial plane motion of particles emitting X-ray photons. Using perspective facilities of space borne instruments (e.g. Constellation-X mission) a better resolution of the blue peak structure of iron Kα line will allow to evaluate the magnetic fields with higher accuracy.

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Quasi-regular X-Ray Bursts from GRS 1915+105 Observed with the IXAE: Possible Evidence for Matter Disappearing into the Event Horizon of the Black Hole

Cited by 54 publications

References 21 publications

The complex behaviour of the microquasar GRS 1915+105 in theρclass observed with BeppoSAX

The complex behaviour of the microquasar GRS 1915+105 in theρclass observed with BeppoSAX

X-ray bursts from the galactic X-ray transient source GRS 1915+105

The iron Kα lines as a tool for magnetic field estimations in non-flat accretion flows

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