Coronal dimmings and what they tell us about solar and stellar coronal mass ejections
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| Main Authors: | , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| author | Veronig, Astrid M. Dissauer, Karin Kliem, Bernhard Downs, Cooper Hudson, Hugh S. Jin, Meng Osten, Rachel Podladchikova, Tatiana Prasad, Avijeet Qiu, Jiong Thompson, Barbara Tian, Hui Vourlidas, Angelos |
| author_facet | Veronig, Astrid M. Dissauer, Karin Kliem, Bernhard Downs, Cooper Hudson, Hugh S. Jin, Meng Osten, Rachel Podladchikova, Tatiana Prasad, Avijeet Qiu, Jiong Thompson, Barbara Tian, Hui Vourlidas, Angelos |
| contents | Coronal dimmings associated with coronal mass ejections (CME) from the Sun have gained much attention since the late 1990s when they were first observed in high-cadence imagery of the SOHO/EIT and Yohkoh/SXT instruments. They appear as localized sudden decreases of the coronal emission at extreme ultraviolet (EUV) and soft X-ray (SXR) wavelengths, that evolve impulsively during the lift-off and early expansion phase of a CME. Coronal dimmings have been interpreted as "footprints" of the erupting flux rope and also as indicators of the coronal mass loss by CMEs. However, these are only some aspects of coronal dimmings and how they relate to the overall CME/flare process. The goal of this review is to summarize our current understanding and observational findings on coronal dimmings, how they relate to CME simulations, and to discuss how they can be used to provide us with a deeper insight and diagnostics of the triggering of CMEs, the magnetic connectivities and coronal reconfigurations due to the CME as well as the replenishment of the corona after an eruption. In addition, we go beyond a pure review by introducing a new, physics-driven categorization of coronal dimmings based on the magnetic flux systems involved in the eruption process. Finally, we discuss the recent progress in studying coronal dimmings on solar-like and late-type stars, and to use them as a diagnostics for stellar coronal mass ejections and their properties. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2505_19228 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Coronal dimmings and what they tell us about solar and stellar coronal mass ejections Veronig, Astrid M. Dissauer, Karin Kliem, Bernhard Downs, Cooper Hudson, Hugh S. Jin, Meng Osten, Rachel Podladchikova, Tatiana Prasad, Avijeet Qiu, Jiong Thompson, Barbara Tian, Hui Vourlidas, Angelos Solar and Stellar Astrophysics Coronal dimmings associated with coronal mass ejections (CME) from the Sun have gained much attention since the late 1990s when they were first observed in high-cadence imagery of the SOHO/EIT and Yohkoh/SXT instruments. They appear as localized sudden decreases of the coronal emission at extreme ultraviolet (EUV) and soft X-ray (SXR) wavelengths, that evolve impulsively during the lift-off and early expansion phase of a CME. Coronal dimmings have been interpreted as "footprints" of the erupting flux rope and also as indicators of the coronal mass loss by CMEs. However, these are only some aspects of coronal dimmings and how they relate to the overall CME/flare process. The goal of this review is to summarize our current understanding and observational findings on coronal dimmings, how they relate to CME simulations, and to discuss how they can be used to provide us with a deeper insight and diagnostics of the triggering of CMEs, the magnetic connectivities and coronal reconfigurations due to the CME as well as the replenishment of the corona after an eruption. In addition, we go beyond a pure review by introducing a new, physics-driven categorization of coronal dimmings based on the magnetic flux systems involved in the eruption process. Finally, we discuss the recent progress in studying coronal dimmings on solar-like and late-type stars, and to use them as a diagnostics for stellar coronal mass ejections and their properties. |
| title | Coronal dimmings and what they tell us about solar and stellar coronal mass ejections |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2505.19228 |