A Quasar Wind Model

TL;DR

This paper proposes a comprehensive quasar wind model that explains the broad line region's structure and dynamics through combined radiative and magnetic forces, aiming to match observational data.

Contribution

It introduces a novel model integrating photoionization and magnetohydrodynamics to describe quasar broad line regions, which are too small for direct imaging.

Findings

Model predicts Doppler-broadened emission lines due to high-velocity gas.

Combines radiative and magnetic driving forces for gas acceleration.

Plans to test model predictions against microlensing and observational data.

Abstract

A quasar wind model is proposed to describe the spatial and velocity structure of the broad line region. This model requires detailed photoionization and magnetohydrodynamic simulation, as the broad line region it too small for direct spatial resolution. The emission lines are Doppler broadened, since the gas is moving at high velocity. The high velocity is attained by the gas from a combination of radiative and magnetic driving forces. Once this model is complete, the model predictions will be tested against recent microlensing data in conjunction with diverse existing observations.