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Radio emission

(low frequency)

Microwave emission

Radio emission

How can radio diagnostics help identify and constrain solar high-energy processes?

Complementing in-situ observations (e.g., PSP, SolO and Wind) using microwave/radio imaging spectroscopy by constrain on the location, timing and energetics of flare-accelerated nonthermal electrons.

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In the corona:

  • Where and how the magnetic reconnection occur?
  • Where how the released magnetic energy is converted to other forms? x-point v.s. cusp region?
  • Pathways of electrons escaping?
  • Does flare scale matter?
  • Radio emission associated with coronal activities in optical/UV/EUV?

What is the connections between the solar high-energy processes and the space weather phenomena?

Decipher reconnection signatures using microwave/radio imaging spectroscopy

to map the dynamic evolving coronal physical properties in and around the reconnection site during flares

  • Magnetic field (strength and direction)
  • Energetics/trajectories of flare-accelerated nonthermal electrons
  • Thermal plasma context

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Sijie Yu (New Jersey Institute of Technology)

SPHERE 2022

Wang et al. in prep

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