Optical precursors to X‐ray binary outbursts

Russell, D. M.; Bramich, D. M.; Lewis, Fraser; AlMannaei, Aisha; Qaissieh, Thabet Al; Qasim, Ahlam Al; Yazeedi, Aisha Al; Baglio, Maria Cristina; Bernardini, F.; Elgalad, N.; Gabuya, Aldrin; Lasota, Jean–Pierre; Palado, Alejandro; Roche, P.; Shivkumar, Hinna; Udrescu, Silviu M.; Zhang, G.

doi:10.1002/asna.201913610

Cited by 41 publications

(38 citation statements)

References 28 publications

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“…MAXI J1348-630 was discovered as a bright X-ray transient on 2019 January 26 (Yatabe et al 2019) by the MAXI monitor onboard the International Space Station (Matsuoka et al 2009) and, thanks to immediate and intense multiwavelength follow-up observations, it was subsequently identified as a BH candidate (Chen et al 2019;Denisenko et al 2019;Kennea & Negoro 2019;Nesci & Fiocchi 2019;Sanna et al 2019;Russell, Baglio & Lewis 2019b;Russell et al 2019c). MAXI J1348-630 displayed a typical outburst that was followed by four reported subsequent hard state re-flares (Russell et al (Al Yazeedi et al 2019;Negoro et al 2019;Russell et al 2019d;Carotenuto et al 2020;Pirbhoy et al 2020;Shimomukai et al 2020;Zhang et al 2020b). While currently, no information is available on the BH inclination, mass, spin and companion star, it has been possible to measure a source distance D = 2.2 +0.5 −0.6 kpc (Chauhan et al 2021) from observations of H I absorption carried out with the Australian Square Kilometre Array Pathfinder (ASKAP) and with MeerKAT.…”

Section: Maxi J1348-630mentioning

confidence: 99%

The black hole transient MAXI J1348–630: evolution of the compact and transient jets during its 2019/2020 outburst

Carotenuto

Corbel

Tremou

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present the radio and X-ray monitoring campaign of the 2019/2020 outburst of MAXI J1348–630, a new black hole X-ray binary (XRB) discovered in 2019 January. We observed MAXI J1348–630 for ∼14 months in the radio band with MeerKAT and the Australia Telescope Compact Array (ATCA), and in the X-rays with MAXI and Swift/XRT. Throughout the outburst we detected and tracked the evolution of the compact and transient jets. Following the main outburst, the system underwent at least 4 hard-state-only re-flares, during which compact jets were again detected. For the major outburst, we observed the rise, quenching, and re-activation of the compact jets, as well as two single-sided discrete ejecta, launched ∼2 months apart and travelling away from the black hole. These ejecta displayed the highest proper motion (≳100 mas day−1) ever measured for an accreting black hole binary. From the jet motion, we constrain the ejecta inclination and speed to be ≤46○ and ≥0.69 c, and the opening angle and transverse expansion speed of the first component to be ≤6○ and ≤0.05 c. We also infer that the first ejection happened at the hard-to-soft state transition, before a strong radio flare, while the second ejection was launched during a short excursion from the soft to the intermediate state. After traveling with constant speed, the first component underwent a strong deceleration, which was covered with unprecedented detail and suggested that MAXI J1348–630 could be located inside a low-density cavity in the interstellar medium, as already proposed for XTE J1550–564 and H1743–322.

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Section: Maxi J1348-630mentioning

confidence: 99%

The black hole transient MAXI J1348–630: evolution of the compact and transient jets during its 2019/2020 outburst

Carotenuto

Corbel

Tremou

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…On 2019 July 30, Russell et al (2019b) reported a brightening in the optical i′-band from the direction of SAXJ1808, which is often a precursor to a full X-ray outburst (Russell et al 2019a). Although this predictor had not previously been tested for SAXJ1808 specifically, various X-ray, UV, and radio observatories were triggered to monitor SAXJ1808 over the following days.…”

Section: Introductionmentioning

confidence: 99%

Timing the Pulsations of the Accreting Millisecond Pulsar SAX J1808.4–3658 during Its 2019 Outburst

Bult

Chakrabarty

Arzoumanian

et al. 2020

ApJ

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In this paper we present a coherent timing analysis of the 401 Hz pulsations of the accreting millisecond X-ray pulsar SAX J1808.4-3658 during its 2019 outburst. Using observations collected with the Neutron Star Interior Composition Explorer (NICER), we establish the pulsar spin frequency and orbital phase during its latest epoch. We find that the 2019 outburst shows a pronounced evolution in pulse phase over the course of the outburst. These phase shifts are found to correlate with the source flux and are interpreted in terms of hot-spot drift on the stellar surface, driven by changes in the mass accretion rate. Additionally, we find that the long-term evolution of the pulsar spin frequency shows evidence for a modulation at the Earthʼs orbital period, allowing for pulsar timing based astrometry of this accreting millisecond pulsar.

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“…The optical monitoring data in B, V, R, i bands (B, V, R in the Vega system and i in the AB system) were taken with the 2-m Faulkes Telescope South (at Siding Spring, Australia) and Las Cumbres Observatory (LCO) 1-m robotic telescopes in Chile, South Africa and Australia (see 50,51 ). The Faulkes/LCO magnitudes were calculated using the 'X-ray Binary New Early Warning System' (XB-NEWS; see 52,53 for details) data analysis pipeline. To estimate the optical flux of SAX J1808.…”

Section: Methodsmentioning

confidence: 99%

Optical and ultraviolet pulsed emission from an accreting millisecond pulsar

Ambrosino,

Zanon,

Papitto

et al. 2021

Preprint

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Millisecond spinning, low magnetic field neutron stars are believed to attain their fast rotation in a 0.1-1 Gyr-long phase during which they accrete matter endowed with angular momentum from a low-mass companion star 1 . Despite extensive searches, coherent periodicities originating from accreting neutron star magnetospheres have been detected only at X-ray energies 2 and in ∼ 10% of the presently known systems 3 . Here we report the detection of optical and ultraviolet coherent pulsations at the X-ray period of the transient low mass X-ray binary system SAX J1808.4−3658, during an accretion outburst that occurred in August 2019 4 . At the time of the observations, the pulsar was surrounded by an accretion disc, displayed X-ray pulsations and its luminosity was consistent with magnetically funneled accretion onto the neutron star. Current accretion models fail to account for the luminosity of both optical and ultraviolet pulsations; these are instead more likely driven by synchrocurvature radiation 5,6 in the pulsar magnetosphere or just outside of it. This interpretation would imply that particle acceleration can take place even when mass accretion is going on, and opens up new perspectives in the study of coherent optical/UV pulsations from fast spinning accreting neutron stars in low-mass X-ray binary systems.Low mass X-ray binary (LMXB) systems hosting a weakly magnetic (∼ 10 8 G) neutron star are believed to be progenitors of millisecond radio pulsars. The evolutionary link between the

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Optical precursors to X‐ray binary outbursts

Cited by 41 publications

References 28 publications

The black hole transient MAXI J1348–630: evolution of the compact and transient jets during its 2019/2020 outburst

The black hole transient MAXI J1348–630: evolution of the compact and transient jets during its 2019/2020 outburst

Timing the Pulsations of the Accreting Millisecond Pulsar SAX J1808.4–3658 during Its 2019 Outburst

Optical and ultraviolet pulsed emission from an accreting millisecond pulsar

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