The Reflares and Outburst Evolution in the Accreting Millisecond Pulsar Sax J1808.4–3658: A Disk Truncated Near Co-Rotation?

Patruno, A.; Maitra, D.; Curran, P. A.; D’Angelo, Caroline; Fridriksson, Joel K.; Russell, D. M.; Middleton, Matthew; Wijnands, Rudy

doi:10.3847/0004-637x/817/2/100

Cited by 52 publications

(61 citation statements)

References 126 publications

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“…The presence of several optical re-flares is one of the most relevant characteristics of the outburst decay of MAXI J1807+132. This kind of phenomena has been observed previously in cataclysmic variables (e.g., Patterson et al 1998) but also in several BH transients such as XTE J1118+480, XTE J1859+226, and GRO J0422+32 (see Zurita et al 2006, and references therein) and NSs systems (e.g., Torres et al 2008;Patruno et al 2016). These binaries have orbital periods of 4.1, 6.6, and 5.1 hr, respectively (Corral-Santana et al 2016).…”

Section: On the Nature Of The Compact Objectsupporting

confidence: 75%

The complex evolution of the X-ray binary transient MAXI J1807+132 along the decay of its discovery outburst

Jiménez-Ibarra

Muñoz-Darias

Padilla

et al. 2018

Monthly Notices of the Royal Astronomical Society

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MAXI J1807+132 is an X-ray transient discovered during the decay of an outburst in 2017. We present optical and X-ray monitoring of the source over more than 125 days, from outburst to quiescence. The outburst decay is characterized by the presence of several re-flares with a quasi-periodic recurrence time of ∼ 6.5 days. We detect broad H and He emission lines during outburst, characteristic of transient low mass X-ray binaries. These emission lines show strong variability from epoch to epoch and, in particular, during the early stages are found embedded into deep and very broad absorption features. The quiescent spectrum shows Hα in emission and no obvious signatures of the donor star. XMM-Newton and Swift spectra can be fitted with standard X-ray models for accreting black-holes and neutron stars, although the obtained spectral parameters favour the latter scenario. Conversely, other observables such as the optical/X-ray flux ratio, the likely systemic velocity (γ ∼ −150 km s −1 ) and the re-flares recurrence time suggest a black hole nature. We discuss all the above possibilities with emphasis on the strong similarities of MAXI J1807+132 with short orbital period systems.

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Section: On the Nature Of The Compact Objectsupporting

confidence: 75%

The complex evolution of the X-ray binary transient MAXI J1807+132 along the decay of its discovery outburst

Jiménez-Ibarra

Muñoz-Darias

Padilla

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…The minioutbursts usually occur when the source is close to the quiescence. These features have been observed in several BH transients, e.g., A0620−00, GRO J0422+32, XTE J1650−500, XTE J1752−233 and MAXI J1659−152 (Kuulkers 1998;Callanan et al 1995;Shrader et al 1997;Tomsick et al 2004;Russell et al 2012;Jonker et al 2012;Homan et al 2013), and also in several neutron star (NS) LMXBTs, e.g., SAX J1808.4−3658 and XTE J1701−407 (Patruno et al 2009(Patruno et al , 2016Degenaar et al 2011). Interestingly, similar minioutbursts features have also been observed in WZ Sge type dwarf novae (DN, Kuulkers et al 1996;Kuulkers 2000;Kato et al 2004).…”

Section: Introductionmentioning

confidence: 89%

Detection of X-ray spectral state transitions in mini-outbursts of black hole transient GRS 1739−278

Yan¹,

Yu²

2017

Monthly Notices of the Royal Astronomical Society

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We report the detection of the state transitions and hysteresis effect in the two minioutbursts of the black hole (BH) transient GRS 1739−278 following its 2014 major outburst. The X-ray spectral evolutions in these two mini-outbursts are similar to the major outburst, in spite of their peak luminosities and the outburst durations are one order of magnitude lower. We found the L hard−to−soft and the L peak,soft of the mini-outbursts also follow the correlation previous found in other X-ray binaries. The L hard−to−soft of the mini-outbursts is still higher than that of the persistent BH binary Cyg X-1, which supports that there is a link between the maximum luminosity a source can reach in the hard state and the corresponding non-stationary accretion represented by substantial rate-of-change in the mass accretion rate during flares/outbursts. The detected luminosity range of these two mini-outbursts is roughly in 3.5×10The X-ray spectra of other BH transients at such low luminosities are usually dominated by a power-law component, and an anti-correlation is observed between the photon index and the X-ray luminosity below 1% L Edd . So the detection of X-ray spectral state transitions indicates that the accretion flow evolution in these two mini-outbursts of GRS 1739−278 are different from other BH systems at such low-luminosity regime.

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“…The X-ray light curves of SAX J1808.4-3658 are similar between different outbursts. After a quick rise to the outburst peak, the source slowly decays for 15-20 days, followed by a faster decay over ≈ 3 days, after which the source reflares for a few tens of days, each reflare lasting a few days (Patruno et al 2016b). Episodic accretion of matter in the propeller regime could be the mechanism behind the reflares (Patruno et al 2016b).…”

Section: Sax J18084-3658mentioning

confidence: 99%

Disc–jet coupling in low-luminosity accreting neutron stars

Tudor

Miller-Jones

Patruno

et al. 2017

Monthly Notices of the Royal Astronomical Society

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In outburst, neutron star X-ray binaries produce less powerful jets than black holes at a given X-ray luminosity. This has made them more difficult to study as they fade towards quiescence. To explore whether neutron stars power jets at low accretion rates (L X 10 36 erg s −1 ), we investigate the radio and X-ray properties of three accreting millisecond X-ray pulsars (IGR J17511-3057, SAX J1808.4-3658 and IGR J00291+5934) during their outbursts in 2015, and of the non-pulsing neutron star Cen X-4 in quiescence (2015) and in outburst (1979). We did not detect the radio counterpart of IGR J17511-3057 in outburst or of Cen X-4 in quiescence, but did detect IGR J00291+5934 and SAX J1808.4-3658, showing that at least some neutron stars launch jets at low accretion rates. While the radio and X-ray emission in IGR J00291+5934 seem to be tightly correlated, the relationship in SAX J1808.4-3658 is more complicated. We find that SAX J1808.4-3658 produces jets during the reflaring tail, and we explore a toy model to ascertain whether the radio emission could be attributed to the onset of a strong propeller. The lack of a universal radio/X-ray correlation, with different behaviours in different neutron star systems (with various radio/X-ray correlations; some being radio faint and others not), points at distinct disk-jet interactions in individual sources, while always being fainter in the radio band than black holes at the same X-ray luminosity.

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The Reflares and Outburst Evolution in the Accreting Millisecond Pulsar Sax J1808.4–3658: A Disk Truncated Near Co-Rotation?

Cited by 52 publications

References 126 publications

The complex evolution of the X-ray binary transient MAXI J1807+132 along the decay of its discovery outburst

The complex evolution of the X-ray binary transient MAXI J1807+132 along the decay of its discovery outburst

Detection of X-ray spectral state transitions in mini-outbursts of black hole transient GRS 1739−278

Disc–jet coupling in low-luminosity accreting neutron stars

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