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The recurring transient outbursts in low-mass X-ray binaries (LMXBs) provideideal laboratories to study the accretion process. Unlike their supermassiverelatives, LMXBs are far too small and distant to be imaged directly.Fortunately, phase-resolved spectroscopy can provide an alternative diagnosticto study their highly complex, time-dependent accretion discs. The primaryspectral signature of LMXBs are strong, disc-formed emission lines detected atoptical wavelengths. The shape, profile, and appearance/disappearance of theselines change throughout a binary orbit, and thus, can be used to trace howmatter in these discs behaves and evolves over time. By combining a\textit{Swift} multi-wavelength monitoring campaign, phase-resolvedspectroscopy from the Gran Telescopio Canarias (GTC) and Liverpool Telescope,and modern astrotomography techniques, we find a clear empirical connectionbetween the line emitting regions and physical properties of the X-rays heatingthe disc in the black hole LMXB MAXI J1820+070 during its 2018 outburst. Inthis paper, we show how these empirical correlations can be used as aneffective observational tool for understanding the geometry and structure of aLMXB accretion disc and present further evidence for an irradiation-drivenwarped accretion disc present in this system.

An empirical connection between line-emitting regions and X-rays heating the accretion disc in BH-LMXB MAXI J1820$+$070