Investigation of the middle corona with SWAP and a data-driven non-potential coronal magnetic field model
| Autor: | Lisa Upton, Duncan H. Mackay, Matthew J. West, Karen A. Meyer, Dana-Camelia Talpeanu |
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| Přispěvatelé: | Science & Technology Facilities Council, European Research Council, University of St Andrews. Applied Mathematics |
| Jazyk: | angličtina |
| Rok vydání: | 2020 |
| Předmět: |
010504 meteorology & atmospheric sciences
Scale (ratio) corona [Sun] Extreme ultraviolet lithography FOS: Physical sciences Image processing Astrophysics 01 natural sciences Article Sun modelling 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics QB Astronomy Sun: magnetic fields 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) QC 0105 earth and related environmental sciences QB Physics Spacecraft Sun: corona business.industry Conjunction (astronomy) Detector Astronomy and Astrophysics 3rd-DAS Corona Magnetic field QC Physics Astrophysics - Solar and Stellar Astrophysics magnetic fields [Sun] Space and Planetary Science Sun: modelling Physics::Space Physics business |
| Zdroj: | Solar Physics |
| Popis: | The large field-of-view of the Sun Watcher using Active Pixel System detector and Image Processing (SWAP) instrument on board the PRoject for Onboard Autonomy 2 (PROBA2) spacecraft provides a unique opportunity to study extended coronal structures observed in EUV in conjunction with global coronal magnetic field simulations. A global non-potential magnetic field model is used to simulate the evolution of the global corona from 1 September 2014 to 31 March 2015, driven by newly emerging bipolar active regions determined from Helioseismic and Magnetic Imager (HMI) magnetograms. We compare the large-scale structure of the simulated magnetic field with structures seen off-limb in SWAP EUV observations. In particular, we investigate how successful the model is in reproducing regions of closed and open structures; the scale of structures; and compare the evolution of a coronal fan observed over several rotations. The model is found to accurately reproduce observed large-scale off-limb structures. When discrepancies do arise they mainly occur off the east solar limb due to active regions emerging on the far side of the Sun, which cannot be incorporated into the model until they are observed on the Earth-facing side. When such ``late'' active region emergences are incorporated into the model, we find that the simulated corona self-corrects within a few days, so that simulated structures off the west limb more closely match what is observed. Where the model is less successful, we consider how this may be addressed, through model developments or additional observational products. Comment: 26 pages, 11 figures |
| Databáze: | OpenAIRE |
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