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Asgari-Targhi Lab
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A lab that explores how magnetic fields and turbulence heat the Sun's atmosphere.
AboutAbout the lab
What heats the Sun's atmosphere: magnetic fields and turbulence
The Asgari-Targhi Lab studies the Sun's magnetic fields and plasma turbulence.
The lab investigates how the motion of plasma involving magnetic fields and turbulence determines the structure and evolution of the solar atmosphere, from the photosphere to the corona.
From this, the lab aims to uncover how the corona is heated and how the solar wind is accelerated.
The lab extends the same perspective to the magnetic fields of stars and galaxies, combining numerical models, analysis of observational data, and theory.
Key terms
- Corona
- The thin, extremely hot layer of gas that extends outward from the Sun's surface
- Solar wind
- The continuous stream of plasma that flows out from the Sun and through the solar system
- Magnetic reconnection
- A phenomenon in which the connectivity of magnetic field lines is rearranged, releasing stored magnetic energy
ResearchResearch themes
The lab investigates how the motion of plasma involving magnetic fields and turbulence determines the structure and evolution of the solar atmosphere. By combining numerical modeling, analysis of observational data, and theoretical plasma physics, it aims to connect small-scale turbulence with large-scale magnetic phenomena.
*Illustrative imageMagnetic Fields and Turbulence in the Solar Atmosphere
The lab studies how the motion of plasma involving magnetic fields and turbulence governs the structure and evolution of the solar atmosphere, from the photosphere to the corona.
*Illustrative imageCoronal Heating and the Solar Wind
The lab considers that these processes in the solar atmosphere cause the heating of the corona and the acceleration of the solar wind, and it is working to uncover the mechanisms behind them.
*Illustrative imageMagnetic Fields of Stars and Galaxies
Extending its research beyond the Sun, the lab investigates how similar plasma and magnetic field behavior around stars and in galactic magnetic fields affects energy transport, turbulence, and magnetic reconnection.
MembersFaculty
- ProfessorASGARI-TARGHI Mahboubeh
VoicesStudent voices
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Seki LabFaculty of Science, Department of Earth and Planetary PhysicsSolar-planetary system physics, electromagnetosphere physics…The information on this page is compiled by the LabLog team from the lab's public information and interviews. For corrections or removal requests, please contact LabLog, not the lab.
Report an errorAbout the images
The top and research theme images are illustrative and were not taken at the lab. They are cropped from Wikimedia Commons images.
- Top image: “Traceimage” NASA / Public domain (cropped)
- Magnetic Fields and Turbulence in the Solar Atmosphere: “Solar granulation” PetrusQ / CC BY 4.0 (cropped)
- Coronal Heating and the Solar Wind: “05 Coronal Mass Ejection ( )” NASA/SOHO / Public domain (cropped)
- Magnetic Fields of Stars and Galaxies: “Messier83 - Heic1403a” Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA) Acknowledgement: William Blair (Johns Hopkins University) / Public domain (cropped)
- Related lab (Shimizu Lab): “SOLAR-B artists concept” NASA/GSFC/C. Meaney / Public domain (cropped)
- Related lab (Amano Lab): “Supernova Remnant SN 1006” X-ray: NASA/CXC/Rutgers/G.Cassam-Chenaï, J.Hughes et al.; Radio: NRAO/AUI/NSF/GBT/VLA/Dyer, Maddalena & Cornwell; Optical: Middlebury College/F.Winkler, NOAO/AURA/NSF/CTIO Schmidt & DSS / CC BY 4.0 (cropped)
- Related lab (Saito-Shinohara Lab (Space Plasma Division)): “Aurora borealis over Eielson Air Force Base, Alaska” United States Air Force photo by Senior Airman Joshua Strang / Public domain (cropped)
- Related lab (Seki Lab): “Aurora Australis From ISS” ISS Expedition 23 crew / Public domain (cropped)
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