3D Solar Flare Modeling

Brock Parker

Montana State University Solar Physics REU 2022

Dr. Chunming Zhu

Weeks 1-2 Weeks 3-4 Weeks 5-6 Weeks 7-8 Weeks 9-10 Home Files

About Me

My name is Brock Parker, and I am currently a rising senior at the University of Wyoming. I am pursuing a dual major in Astronomy and Physics, as well as a dual minor in Honors and Mathematics. Over the summer of 2022, I am participating in the Montana State University Solar Physics REU program to gain more experience in other areas of physics and research, as well as improve and garner useful research skills.

REU Project

Over the course of the summer, I am working with Dr. Chunming Zhu to characterize the heating coefficient between the 1600 Angstrom solar flare data and the corresponding heating functions, as well as using this data to generate light curves to compare with the observed light curves. The end goal is to create three dimensional images of the solar flares using HMI data with the simulated flares and flare locations to compare to observed flares.

Current Research

My current research interests involve transiting exoplanets and observational astronomy, which I have been conducting under the guidance of Dr. Chip Kobulnicky at the University of Wyoming.


bparke13@uwyo.edu | brockaustin09@gmail.com

Research Project

Brock Parker, Dr. Chunming Zhu

Solar flares are incredibly intense and violent bursts of radiation in the solar atmosphere. Current models suggest that their origin involves the twisting and recombination of magnetic fields in the solar atmosphere, however there is much debate about the true nature of the heating of these solar flares. Basic models imploy the notion of one intense burst of energy deposition into the solar flare, in the form of an impulsive function at the feet of the solar flare. However, as the flare moves through the upper atmosphere, magnetic fields recombine, releasing energy near the top peak of the flare, subsequently heating it more. Additionally, there are multiple methods through which flares can deposit their energy back into the solar atmosphere.

Using data from the Solar Dynamics Observatory, which images the sun in multiple different ultraviolent and extreme ultraviolet passbands along with recording the magnetic field strength, this project will aim to model these solar flares in both zero and three dimensions, as well as derive flare energy, and compare all values to the observed flare. In total, this methodology will work towards understanding the heating and cooling of solar flare loops and the plasma contained inside.

References

Chunming Zhu, et al. 2018, ApJ, 856, 27.

J. A. Klimchuk, et al. 2008, ApJ, 682, 1351.

Jiong Qiu, et al. 2012, ApJ, 752, 124.

Jiong Qiu and Longcope, Dana 2016, ApJ, 820, 14.

Paul Boerner, et al. 2012, Solar Physics, 275, 41.

R. Rosner, et al. 1978, ApJ, 220, 634.

Brock Parker