| Name: | Santhiya P S |
| Affiliation: | International Centre for Theoretical Sciences |
| Conference ID : | ASI2024_691 |
| Title : | Study of Accretion Disk-Jet Symbiosis using General Relativistic Magnetohydrodynamic Simulations |
| Authors : | Santhiya P S1, Tushar Mondal1, Indu Dihingia2, Pallavi Bhat1, Prayush Kumar1 |
| Authors Affiliation: | 1 International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bangalore -560089, India
2 Tsung-Dao Lee Institute, Shanghai Jiao-Tong University, Shanghai, 520 Shengrong Road, 201210, People’s Republic of China |
| Mode of Presentation: | Poster |
| Abstract Category : | High Energy Phenomena, Fundamental Physics and Astronomy |
| Abstract : | Astrophysical jets are powerful collimated outflows observed to arise from active galactic nuclei (AGN) that can extend up to galactic scales. Though there have been theoretical models formulated to explain the dynamics of jets, their formation and evolution are poorly understood. Limited observational evidence and some theoretical investigations speculate that the spin and mass of the black holes along with the magnetic flux in their vicinity decide the power of these jets. Observations of γ-rays and spectral lines from AGNs and gamma ray burst (GRB) sources show a correlation between jet power and accretion-disk luminosity (R S Nemmen et. al 2012 Science,
338(6113), 1445-1448, G Ghisellini et. al 2014 Nature, 515(7527), 376-378).Several observations also confirm the signature of dynamically dominant magnetic fields in the vicinity of central black holes (R P Eatough et. al 2013 Nature, 501(7467), 391-394, M Zamaninasab et. al 2014 Nature, 510(7503), 126-128). The study of disk-jet symbiosis could help us understand the dynamics of these complicated yet highly energetic systems.
We perform direct numerical simulations of disk-jet using the publically available General Relativistic Magnetohydrodynamic code called Black-Hole Accretion Code (BHAC). We use these simulations to compute the disk luminosity via energy budget considerations and jet power from Poynting flux and kinetic energy of the flow. Our preliminary findings show a correlation between these quantities. We perform a parameter scan over spin, magnetic field strength and mass accretion rate to analyse the range in which these correlations hold. |
