Abstract Details

Name: Sriyasriti Acharya
Affiliation: Indian Institute of Technology, Indore
Conference ID: ASI2020_209
Title : Kink Instability: Its Impact on the Variability and Emission Features Observed in Blazar Jets
Authors and Co-Authors : Sriyasriti Acharya, Nikhil Sanjay Borse, Dr. Bhargav Vaidya
Abstract Type : Poster
Abstract Category : Extragalactic Astronomy
Abstract : One of the characteristic features seen among the radio-loud Active Galactic Nuclei (AGNs) is the presence of a relativistic jet in a direction perpendicular to the plane of the underlying accretion disk. These jets exhibit multi-timescale variability, cover a wide spectrum of length scales and can have emission up to a length of mega-parsec in radio bands. These magnetically dominated jet becomes kinetically dominated and remains stable at parsec scales. The processes responsible for such energy dissipation and stability are still under debate. Magnetohydrodynamical (MHD) instabilities are believed to be one of the plausible mechanisms for dissipation of magnetic energy that could possibly trigger jet radiation and particle acceleration. However, the effect of these instabilities on the observed features of jets is still unanswered. Addressing this, in this talk, I will focus on the impact of magnetic kink instability on the observed Blazar variability and emission pattern. I will present our recent results on parameter study that provides constraints on simulating relativistic jets, by solving the ideal MHD equations using the widely used PLUTO code. The role of kink (m = 1) mode instability is explored through three-dimensional relativistic MHD simulations of current-carrying cylindrical plasma columns with force-free equilibrium conditions. As the presence of kink instability leads to the formation of the helical structure of jet, the effect of different viewing angles on the emission features is studied in this work. The simulations are carried out with both periodic and outflow boundary configuration containing a strong toroidal magnetic field, a bulk Lorentz factor of 5, with different density and pressure profiles.