19-23 October 2020
Europe/Prague timezone
Please, give us your feedback in the Survey

Modeling of Wind -fed accretion in HMXBs using GRMHD code

20 Oct 2020, 11:10


Ishika Palit (Center for theoretical physics PAS)


Accretion disks in High mass X-ray binaries (HMXB's) are mostly fed by the stellar wind from their companion star. These winds also affect the observed X-ray spectra arising from the hot coronal flow.
Cygnus X-1 and its companion star, HDE-226868 is one of such HMXBs. It is one of the brightest X-ray sources observed and shows the X-ray intensity variations in both the soft and hard X-rays. I will present my recent work on 2D numerical modeling using GRMHD code - HARM, replicating such focused, clumpy wind from the binary companion fed for accretion onto the black hole. We model an inviscid, non-magnetized, transonic accretion flow with a low angular momentum profile. I will talk about how we model transonic accretion and my prescribed time-dependent boundary conditions in this code. I will further discuss how it affects the hydrodynamics of the flow in the relativistic framework and what information it reflects on the Power Density Spectra (PDS)

Primary authors

Ishika Palit (Center for theoretical physics PAS) Agnieszka Janiuk (CTP PAS) Bozena Czerny (Center for Theoretical Physics)

Presentation Materials