Speaker
Description
Coronal dimmings on the Sun are transient reductions in coronal plasma
emissions, often associated with Coronal Mass Ejections (CMEs) triggered
by solar flares or filament eruptions. These dimmings typically last
between 3 to 12 hours, characterized by a rapid decrease in intensity
followed by a gradual recovery. In this study, we conduct a differential
emission measure (DEM) analysis using a Sun-as-a-star approach to
explore the relationship between dimming depth and emission measures
across various temperature bands. We utilize data from the Atmospheric
Imaging Assembly (AIA) aboard the Solar Dynamics Observatory (SDO) to
perform DEM analysis on six CME-associated events, including four
flaring events and two filament eruptions. Our results indicate that
while the temperature band for maximum dimming varies across events,
significant dimmings are predominantly observed in the 5.85–6.45 log K
temperature range. Emission in hotter temperature bands shows little or
no dimming. Additionally, we calculate the DEM-weighted temperature of
the corona and observe a temperature difference between pre-event
conditions and the peak dimming phase. Interestingly, we detect signs of
coronal heating in the early stages of the dimming, suggesting complex
thermal responses in the corona during CME evolution. These findings
provide critical insights into the coronal response to CME events and
the associated heating of coronal plasma. Furthermore, they enhance our
understanding of the solar-stellar connection and have significant
implications for space weather forecasting.
| Contribution Type | Poster |
|---|---|
| Theme | Solar - Stellar Connections |
