X-ray nova A0620-00 - Celestial position and low-energy flux

Doxsey, R.; Jernigan, G.; Hearn, D. R.; Bradt, H.; Buff, J.; Clark, G. W.; Delvaille, J. P.; Epstein, A.; Matilsky, T.; Mayer, W.; McClintock, Jeffrey E.; Rappaport, S.; Richardson, J. D.; Schnopper, H.

doi:10.1086/182006

Cited by 17 publications

(14 citation statements)

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“…Parts of these data have been reported by Doxsey et al (1976), Matilsky et al (1976) and Plaks (1991). We used the data as re-analysed by Plaks (1991), i.e.…”

Section: X-raymentioning

confidence: 63%

“…No modulation larger than ∼3% over timescales 200 s-2 d was seen during the rise and at maximum (Ariel V SSE, 2-18 keV, Elvis et al 1975). Near X-ray maximum also down to 0.2 msec no evidence for pulsations were reported (SAS-3 slat collimator system, 1.5-60 keV, Doxsey et al 1976). During the first months after maximum there was no evidence for periodic fluctuations or the shot noise variability seen in e.g.…”

Section: Outburstmentioning

confidence: 96%

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A 0620 - 00 revisited: a black-hole transient case-study

Kuulkers

1998

New Astronomy Reviews

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For the first time we have performed a detailed study of the X-ray, optical and infrared light curves and an intercomparison between these wavelengths (including radio) of the 1975/1976 outburst of the famous black-hole transient A 0620−00 (Nova Mon 1975, V616 Mon). We also investigated the optical behaviour up to a year after the main outburst. This study enabled us to find some new features, which have not been discussed before.During the various stages of the outburst of A 0620−00 we found the X-rays lag the optical on the order of ∼5 to ∼20 days. Moreover, we found evidence that the activity associated with the secondary maximum started even earlier in the infrared. This suggests that most of the processes associated with the outburst occur in the outer parts of the accretion disk.Although various drops in intensity (lasting on the order of a day or more) in the optical and X-ray outburst light curves of A 0620−00 have been reported before, we identified some new ones. One such X-ray 'dip' only appeared in the soft X-rays (1.5-6 keV) whereas at higher energies ( 6 keV) the intensity slightly increases. This shows that the X-ray spectrum pivots near ∼6 keV around that time. In the optical we found evidence for another local maximum around that time (so-called 'intermediate' maximum). The 'intermediate' maximum appears ∼30 days after the secondary maximum, which is close to the viscous time scale of an irradiated accretion disk. We suggest this feature to be an 'echo' of the secondary maximum. At the end of the outburst another local maximum occurs. Since the time difference between the peak of the tertiary maximum and this local maximum is also on the order of the viscous time scale we suggest that this feature is an 'echo' of the tertiary maximum. We find that drops in the optical and X-ray intensity before and during the rise to tertiary maximum are also present in various other short period soft X-ray transients (SXTs). They always occur ∼150 days after the start of the outburst.Although the X-ray spectrum of A 0620−00 gradually softens during the decay from outburst, we find for the first time that it starts to harden again ∼100-150 days after the start of the outburst, similar to that seen in GS 2000+25 and GS 1124−68. This suggests we witness the transition from the so-called high to low state identified in black-hole X-ray binaries. We note that the time of spectral hardening in Preprint submitted to Elsevier Preprint 1 October 2018A 0620−00, GS 2000+25 and GS 1124−68 is simultaneous with the occurrence of the drops in optical and X-ray intensity.We also show that the optical outburst amplitude and the shape of the optical outburst light curve of A 0620−00 closely resembles those of the cataclysmic variable AL Com (where the compact star is a white dwarf). This strengthens the similarity in outburst and quiescent properties of the SXTs and 'Tremendous Outburst Amplitude Dwarf novae' (TOADs) or WZ Sge stars, and shows that in general the optical outburst light curves of both groups are governed...

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“…Parts of these data have been reported by Doxsey et al (1976), Matilsky et al (1976) and Plaks (1991). We used the data as re-analysed by Plaks (1991), i.e.…”

Section: X-raymentioning

confidence: 63%

Section: Outburstmentioning

confidence: 96%

A 0620 - 00 revisited: a black-hole transient case-study

Kuulkers

1998

New Astronomy Reviews

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“…These observations all show fairly soft spectra with characteristic peak temperatures around a few keV (e.g., Carpenter et al 1976 ;Citterio et al 1976 ;Doxsey et al 1976 ;Long & Kestenbaum 1978) conÐrming that this system indeed looked like GRS 1124[68 in the VHS and HS. After about D100 days, we have to rely on the broadband data, so in Figure 1 (lower panels) we have plotted ratios of count rates in the hard and soft X-ray bands for both objects.…”

Section: X-ray Outbursts Of Grs 1124[68 and A0620[00mentioning

confidence: 85%

Optical Light Curves of the Black Hole Binaries GRS 1124−68 and A0620−00 in Outburst: The Importance of Irradiation

Esin

Kuulkers

McClintock

et al. 2000

ApJ

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We test whether the model proposed by Esin et al. to explain X-ray observations of the black hole soft X-ray transient GRS 1124[68 in outburst can also explain the optical light curves of a similar object, A0620[00. We show that to reproduce the observed X-ray to optical Ñux ratio in A0620[00, we need to assume X-ray irradiation of the outer disk that is signiÐcantly in excess of what is expected for a standard planar disk. With enhanced irradiation, the Esin et al. model can reproduce the optical evolution of A0620[00 in outburst very well. Though we Ðnd that optical observations of GRS 1124[68 also imply enhanced X-ray heating of the outer disk, the irradiation appears to be a factor of D3 weaker in this system than in A0620[00. This is surprising, since GRS 1124[68 has a larger disk. We speculate that enhanced irradiation may be due to disk warping, and that the degree of warping di †ers between the two binaries.

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“…A0620-00 is an example of an X-ray nova which was well observed at both X-ray and optical wavelengths. The simultaneous eruptions in both spectral regions with Z,x /L opt ~ 103 (Doxsey et al 1976) contrasts with the negligible X-ray emission from the optical nova Nova Cygni 1975 which had L^/ L opt < 10~3 (Hoffmann et al 1976). Early suggestions th a t non-thermal processes in optical classical nova erup tions could account for X-ray novae (Brecher & Morrison 1975;Eachus et al 1976) are no longer tenable.…”

Section: X-ray Novae and Related Sourcesmentioning

confidence: 98%

A comparison of optical and X-ray novae

Bath

1979

Proc. R. Soc. Lond. A

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The similarities and differences between optical novae and transient X-ray novae are discussed. Both classes almost certainly require a semi-detached binary structure. Present theoretical models of classical novae account for the outburst in terms of a nuclear burning runaway in the accreted material on the white dwarf within a semi-detached binary system. In the case of the dwarf novae and the transient X-ray sources, unstable accretion events are the generally accepted model. Mechanisms that could generate unstable accretion events are described.

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X-ray nova A0620-00 - Celestial position and low-energy flux

Cited by 17 publications

References 0 publications

A 0620 - 00 revisited: a black-hole transient case-study

A 0620 - 00 revisited: a black-hole transient case-study

Optical Light Curves of the Black Hole Binaries GRS 1124−68 and A0620−00 in Outburst: The Importance of Irradiation

A comparison of optical and X-ray novae

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