We are a Astrophysics team under SSERD IPD working on finding a relation that accounts for the mass transfer from a companion star to a black hole, which would help us conclude the mass conservation and find if there is any discrepancy, which we call as the ghost mass and use reference systems for validation of ghost mass problem and accounting for the discrepancy using models/computation.
Having been inspired from the Cygnus-X1 system, the goal was to set up a similar binary system model and analyse some fundamental properties. We introduce a hypothetical binary system that consists of a stellar mass black hole, and an intermediate mass main sequence star. The base model builds up on the fact that mass from the star transfers to the black-hole via accretion. This leads to the inclusion of different types of mass transfers that take place in this whole process: Mass transfers due to stellar winds, Roche lobe overflows, advective outflows from the accretion disk, and astrophysical jets.
Upon closer look, these mass transfers are actually the cause of mass losses that occurs during the transfer from a star to a black-hole. So, not all the mass is conserved. This mass discrepancy we term as Ghost Mass. The mass gained by the black-hole is not equivalent to the mass lost by the star.
Our work in summary started off with intense literature review of what systems we could take into consideration, and what mass transfers we could account for. Having singled those out, we then proceeded with our analysis in the following manner:
We obtained the following results for the 3 systems:
And a simulation of a binary system in Unity made by our Adrian boii
We are really enthusiastic and hopeful to talk with you and exchange ideas, recieve feedback and answer queries. Please feel free to drop a message using any of the mediums below. It was nice meeting you. Themks xD
