Plasma Physics Initaitive
The TAP Plasma Physics Initiative uses theory and numerical simulation, combined with remote and in situ observations of space and astrophysical plasmas, to constrain fundamental questions about how energy, mass, and momentum are injected into, transported through, and removed from a wide variety of plasma systems throughout the Universe.
Join the Plasma Physics Mailing List
For meeting times and locations contact Plasma Physics Initiative Leads Joe Giacalone, Kris Klein, or Shuo Kong.
Upcoming Plasma Physics Initiative Lectures
TAP Plasma Physics Initiative Lectures are scheduled in the Spring Semester.
Check back in January for future guest announcements.
Fall 2023 to Spring 2025
Xianzhe Jia, University of Michigan
Visit Dates: March 3 - 6, 2025
TITLE: Extended MHD and Coupled Fluid-Kinetic Simulations of Planetary Magnetospheres: Applications to Mercury and Ganymede
Anna Tenerani, University of Texas at Austin
Visit Dates: December 1 - 6, 2025
TITLE: Coronal Heating and Solar Wind Acceleration: What are we Learning from Parker Solar Probe
Jason TenBarge, Princeton University
Visit Dates: September 20 - 30, 2023
TITLE:
New Perspectives on Diagnosing Electron Energization in Magnetic Reconnection
Affiliated Research Groups
Solar and Heliospheric Research Group
The Solar and Heliospheric Research Group seeks a greater understanding of the diverse plasma processes at work throughout our solar system and the universe. Research topics range from the physics of the solar interior and atmosphere to the solar wind, energetic particle transport, and acceleration processes. Email Profs. Joe Giacalone or Kris Klein for meeting details.
Kong Research Group
We investigate the multiphase structure of the interstellar medium, with an emphasis on molecular clouds as the primary sites of star formation. Our research focuses on elucidating the role of magnetic fields in the processes governing molecular cloud formation and subsequent star formation. To address these questions, we employ numerical simulations to model the relevant physical mechanisms and validate these models through comparison with multiwavelength astronomical observations obtained from a range of telescopes.