Modelling the compact jet in MAXI J1836-194 with disc-driven shocks

Péault, Mathias; Malzac, J.; Coriat, M.; Russell, Thomas; Koljonen, K. I. I.; Belmont, R.; Corbel, S.; Drappeau, S.; Ferreira, Jonathan; Petrucci, Pierre-Olivier; Rodríguez, J.; Russell, D. M.

doi:10.1093/mnras/sty2796

Cited by 23 publications

(42 citation statements)

References 44 publications

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“…As the source sample is small, it is difficult to definitively determine whether jet speed increases with Eddington fraction, in line with past predictions (Vadawale et al 2003;Fenderetal.2004Fenderetal. , 2009, measurements of two tracks in the radio/X-ray correlation for BHXBs (Russell et al 2015), and more recent modelling (Péault et al 2019). However, Fig.…”

Section: Jet Speedmentioning

confidence: 99%

Measuring fundamental jet properties with multiwavelength fast timing of the black hole X-ray binary MAXI J1820+070

Tetarenko

Casella

Miller-Jones

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present multi-wavelength fast timing observations of the black hole X-ray binary MAXI J1820+070 (ASASSN-18ey), taken with the Karl G. Jansky Very Large Array (VLA), Atacama Large Millimeter/Sub-Millimeter Array (ALMA), Very Large Telescope (VLT), New Technology Telescope (NTT), Neutron Star Interior Composition Explorer (NICER), and XMM-Newton. Our data set simultaneously samples ten different electromagnetic bands (radio – X-ray) over a 7-hour period during the hard state of the 2018–2019 outburst. The emission we observe is highly variable, displaying multiple rapid flaring episodes. To characterize the variability properties in our data, we implemented a combination of cross-correlation and Fourier analyses. We find that the emission is highly correlated between different bands, measuring time-lags ranging from hundreds of milliseconds between the X-ray/optical bands to minutes between the radio/sub-mm bands. Our Fourier analysis also revealed, for the first time in a black hole X-ray binary, an evolving power spectral shape with electromagnetic frequency. Through modelling these variability properties, we find that MAXI J1820+070 launches a highly relativistic ($\Gamma =6.81^{+1.06}_{-1.15}$) and confined ($\phi =0.45^{+0.13}_{-0.11}$ deg) jet, which is carrying a significant amount of power away from the system (equivalent to ∼0.6 L1 − 100keV). We additionally place constraints on the jet composition and magnetic field strength in the innermost jet base region. Overall, this work demonstrates that time-domain analysis is a powerful diagnostic tool for probing jet physics, where we can accurately measure jet properties with time-domain measurements alone.

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Section: Jet Speedmentioning

confidence: 99%

Measuring fundamental jet properties with multiwavelength fast timing of the black hole X-ray binary MAXI J1820+070

Tetarenko

Casella

Miller-Jones

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Effects such as jet collimation or inclination might be included, for instance. This work will be done by coupling our code with the jet spectral code ISHEM (Malzac 2014;Péault et al 2019), and thus will also further address the possibility of dark jets (Drappeau et al 2017). Additionally, our face-on disk is inconsistent with our edge-on estimates of the jet emission: this discrepancy will be solved in the future.…”

Section: Open Questionsmentioning

confidence: 99%

A unified accretion-ejection paradigm for black hole X-ray binaries

Marcel

Ferreira

Clavel

et al. 2019

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Context. Transient X-ray binaries (XrB) exhibit very different spectral shapes during their evolution. In luminosity-color diagrams, their behavior in X-rays forms q-shaped cycles that remain unexplained. In Paper I, we proposed a framework where the innermost regions of the accretion disk evolve as a response to variations imposed in the outer regions. These variations lead not only to modifications of the inner disk accretion rate ṁin, but also to the evolution of the transition radius rJ between two disk regions. The outermost region is a standard accretion disk (SAD), whereas the innermost region is a jet-emitting disk (JED) where all the disk angular momentum is carried away vertically by two self-confined jets. Aims. In the previous papers of this series, it has been shown that such a JED–SAD disk configuration could reproduce the typical spectral (radio and X-rays) properties of the five canonical XrB states. The aim of this paper is now to replicate all X-ray spectra and radio emission observed during the 2010–2011 outburst of the archetypal object GX 339-4. Methods. We used the two-temperature plasma code presented in two previous papers (Papers II and III) and designed an automatic ad hoc fitting procedure that for any given date calculates the required disk parameters (ṁin,rJ) that fit the observed X-ray spectrum best. We used X-ray data in the 3–40 keV (RXTE/PCA) spread over 438 days of the outburst, together with 35 radio observations at 9 GHz (ATCA) dispersed within the same cycle. Results. We obtain the time distributions of ṁin(t) and rJ(t) that uniquely reproduce the X-ray luminosity and the spectral shape of the whole cycle. In the classical self-absorbed jet synchrotron emission model, the JED–SAD configuration also reproduces the radio properties very satisfactorily, in particular, the switch-off and -on events and the radio-X-ray correlation. Although the model is simplistic and some parts of the evolution still need to be refined, this is to our knowledge the first time that an outburst cycle is reproduced with such a high level of detail. Conclusions. Within the JED–SAD framework, radio and X-rays are so intimately linked that radio emission can be used to constrain the underlying disk configuration, in particular, during faint hard states. If this result is confirmed using other outbursts from GX 339-4 or other X-ray binaries, then radio could be indeed used as another means to indirectly probe disk physics.

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“…There are indications that matter in compact jets could be accelerated up to bulk Lorentz factors j ࣠ 3.5 (e.g. Ribó, Dhawan & Mirabel 2004;Russell et al 2015;Péault et al 2019;Saikia et al 2019;Tetarenko et al 2019). No radio emission is usually detected during the soft state, as compact jets are strongly quenched (Fender et al 1999;Corbel et al 2000), by at least 3.5 orders of magnitude (Russell et al 2019a;Maccarone et al 2020).…”

mentioning

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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Modelling the compact jet in MAXI J1836-194 with disc-driven shocks

Cited by 23 publications

References 44 publications

Measuring fundamental jet properties with multiwavelength fast timing of the black hole X-ray binary MAXI J1820+070

Measuring fundamental jet properties with multiwavelength fast timing of the black hole X-ray binary MAXI J1820+070

A unified accretion-ejection paradigm for black hole X-ray binaries

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

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