Heating_Effect_of_Solar_Corona_Presentation.pptx
- 1. Heating Effect of Solar Corona • Rishi Shukla • University Roll No.: 2310014275038 • Supervisor: Dr. Punit Kumar • Department of Physics, University of Lucknow • Session: 2024–25
- 2. Abstract • • Plasma waves exist across solar system bodies including the Sun. • • They transport energy and particles from the solar core to the interplanetary medium. • • These waves provide insights into energy distribution in solar plasma. • • Focus on electrostatic (ES) and electromagnetic (EM) plasma waves.
- 3. Introduction • • Plasma waves are ubiquitous in solar and space environments. • • They play a role in particle acceleration and energy transport. • • Generated by ~50 known plasma instabilities. • • Carry information about the solar plasma conditions.
- 4. Solar Plasma Environment • • Sun has three major regions: core, photosphere, corona. • • Plasma density and temperature vary greatly across regions. • • Plasma parameters (Density, Temperature, Magnetic Field) vary significantly.
- 5. Space Missions Studying Plasma Waves • • Key missions: Helios, ISEE-3, Ulysses, WIND, ACE, STEREO. • • Instruments onboard: Magnetometers, electric field probes, plasma wave detectors. • • L1 point is optimal for studying undisturbed solar plasma waves.
- 6. Plasma Wave Generation Near the Sun • • Triggered by instabilities like bump-on-tail and heat-flux instability. • • Waves: Langmuir, Whistler, Ion Acoustic, Alfven waves. • • Plasma wave generation and propagation towards Earth.
- 7. Waves in the Solar Wind • • Observed by WIND spacecraft. • • Ion acoustic and Alfven waves result from instabilities and beam interactions. • • Pulse-like Alfvenic disturbances recorded in solar wind.
- 8. Types of Plasma Instabilities • • Langmuir waves (f ~ fpe): Electron beam • • Ion acoustic waves: Ion beam • • Whistler waves: Heat-flux • • Electron acoustic waves: Electron beam
- 9. Unresolved Scientific Issues • • Role of waves in stream interactions and energy loss. • • Incomplete understanding of wave-particle interactions. • • Need for better instruments to resolve open questions. • • Estimation of local plasma parameters still challenging.
- 10. Conclusion • • Plasma waves are crucial for understanding solar plasma. • • Direct observation near the Sun is challenging. • • Missions at L1 help trace wave origins. • • Future missions must include advanced wave detection systems.