Polar Jet Simulation with the Alfvén Wave Solar Model (AWSoM)
Abstract
Coronal jets are being observed by multiple instruments at multiple wavelengths (SOHO, Yohkoh, STEREO, Hinode [Paraschiv (2010, 2015)]). Studying polar jets can lead to an improved understanding of the relations between magnetic field topology and reconnection as well as solar wind heating and acceleration.The thermodynamical evolution of the plasma is the focus of our work. We introduce a slowly accelerated rotating bipole field in the open region of the background magnetic field. Similar magnetic topology is also implied in observations. Our aim is to implement the formation and evolution of polar jets in the coronal hole region starting from the chromosphere up to the outer corona. The simulations show small-scale eruptive reconnection events. The self-consistent heating and acceleration of the solar wind in the AWSoM model [van der Holst (2014)] provides the opportunity to study the energetics of the jet phenomena. This study leads to the possibility of quantitative comparison of the simulation results to X-ray, EUV or white light observations.
- Publication:
-
Solar Heliospheric and INterplanetary Environment (SHINE 2015)
- Pub Date:
- July 2015
- Bibcode:
- 2015shin.confE..87S