The Need for Plasma Astrophysics in Understanding Life Cycles of Active Galaxies

TL;DR

This paper advocates for integrating plasma astrophysics into active galaxy studies, emphasizing improved observational resolution, laboratory experiments, and advanced simulations to better understand jet formation, magnetic fields, and accretion processes.

Contribution

It highlights the necessity of combining observational, experimental, and theoretical approaches to advance understanding of active galaxy phenomena.

Findings

Enhanced resolution of VLA can resolve jet structures at kpc scales.

Laboratory plasma experiments can elucidate key astrophysical processes.

Developing comprehensive models will connect large-scale phenomena with relativistic physics.

Abstract

In this White Paper, we emphasize the need for and the important role of plasma astrophysics in the studies of formation, evolution of, and feedback by Active Galaxies. We make three specific recommendations: 1) We need to significantly increase the resolution of VLA, perhaps by building an EVLA-II at a modest cost. This will provide the angular resolution to study jets at kpc scales, where, for example, detailed Faraday rotation diagnosis can be done at 1GHz transverse to jets; 2) We need to build coordinated programs among NSF, NASA, and DOE to support laboratory plasma experiments (including liquid metal) that are designed to study key astrophysical processes, such as magneto-rotational instability (origin of angular momentum transport), dynamo (origin of magnetic fields), jet launching and stability. Experiments allowing access to relativistic plasma regime (perhaps by intense lasers and magnetic fields) will be very helpful for understanding the stability and dissipation physics of jets from Supermassive Black Holes; 3) Again through the coordinated support among the three Agencies, we need to invest in developing comprehensive theory and advanced simulation tools to study the accretion disks and jets in relativistic plasma physics regime, especially in connecting large scale fluid scale phenomena with relativistic kinetic dissipation physics through which multi-wavelength radiation is produced.