Large optical modulations during 2018 outburst of MAXI J1820 + 070 reveal evolution of warped accretion disc through X-ray state change

Author:

Thomas Jessymol K1,Charles Philip A2,Buckley David A H13ORCID,Kotze Marissa M13,Lasota Jean-Pierre45ORCID,Potter Stephen B16ORCID,Steiner James F7,Paice John A28ORCID

Affiliation:

1. South African Astronomical Observatory, Observatory Road, Observatory, 7925 Cape Town, RSA

2. Department of Physics & Astronomy, University of Southampton, Southampton SO17 1BJ, UK

3. Department of Physics, University of the Free State, PO Box 339, Bloemfontein 9300, South Africa

4. Institut d’Astrophysique de Paris, CNRS et Sorbonne Université, UMR 7095, 98bis Bd Arago, F-75014 Paris, France

5. Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, PL-00-716 Warsaw, Poland

6. Department of Physics, University of Johannesburg, PO Box 524, Auckland Park 2006, South Africa

7. Center for Astrophysics, Harvard-Smithsonian, 60 Garden St, Cambridge, MA 02138, USA

8. Inter-University Centre for Astronomy and Astrophysics, Pune, Maharashtra 411007, India

Abstract

ABSTRACT The black hole X-ray transient MAXI J1820 + 070  (= ASSASN-18ey) discovered in 2018 March was one of the optically brightest ever seen, which has resulted in very detailed optical outburst light curves being obtained. We combine them here with X-ray and radio light curves to show the major geometric changes the source undergoes. We present a detailed temporal analysis that reveals the presence of remarkably high amplitude (>0.5 mag) modulations, which evolve from the superhump (16.87 h) period towards the presumed orbital (16.45 h) period. These modulations appear ∼87 d after the outburst began, and follow the Swift/BAT hard X-ray light curve, which peaks 4 d before the radio flare and jet ejection, when the source undergoes a rapid hard to soft state transition. The optical modulation then moves closer to the orbital period, with a light-curve peak that drifts slowly in orbital phase from ∼0.8 to ∼0.3 during the soft state. We propose that the unprecedentedly large amplitude modulation requires a warp in the disc in order to provide a large enough radiating area, and for the warp to be irradiation driven. Its sudden turn-on implies a change in the inner disc geometry that raises the hard X-ray-emitting component to a height where it can illuminate the warped outer disc regions.

Funder

CNES

STFC

UGC

UKIERI

University of Southampton

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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1. The Delayed Radio Emission in the Black Hole X-Ray Binary MAXI J1348-630;The Astrophysical Journal Letters;2024-07-01

2. Black hole accretion in the outburst of X-ray binaries;Chinese Science Bulletin;2024-07-01

3. Plunging region emission in the X-ray binary MAXI J0637−430;Monthly Notices of the Royal Astronomical Society: Letters;2024-06-14

4. Tracking the X-Ray Polarization of the Black Hole Transient Swift J1727.8–1613 during a State Transition;The Astrophysical Journal;2024-06-01

5. Continuum emission from within the plunging region of black hole discs;Monthly Notices of the Royal Astronomical Society;2024-05-13

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