Back to Search
Start Over
Forward Modeling of SDO /AIA and X-Ray Emission from a Simulated Flux Rope Ejection
- Source :
- The Astrophysical Journal
- Publication Year :
- 2019
-
Abstract
- We conduct forward-modeling analysis based on our 2.5 dimensional magnetohydrodynamics (MHD) simulation of magnetic flux rope (MFR) formation and eruption driven by photospheric converging motion. The current sheet (CS) evolution during the MFR formation and eruption process in our MHD simulation can be divided into four stages. The current sheet (CS) evolution during the MFR formation and eruption process in our MHD simulation can be divided into four stages. The first stage shows the CS forming and gradually lengthening. Resistive instabilities that disrupt the CS mark the beginning of the second stage. Magnetic islands disappear in the third stage and reappear in the fourth stage. Synthetic images and light curves of the seven Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA) channels, i.e., 9.4 nm, 13.1 nm, 17.1 nm, 19.3 nm, 21.1 nm, 30.4 nm, and 33.5 nm, and the 3-25 keV thermal X-ray are obtained with forward-modeling analysis. The loop-top source and the coronal sources of the soft X-ray are reproduced in forward modeling. The light curves of the seven SDO/AIA channels start to rise once resistive instabilities develop. The light curve of the 3-25 keV thermal X-ray starts to go up when the reconnection rate reaches one of its peaks. Quasiperiodic pulsations (QPPs) appear twice in the SDO/AIA 17.1 nm, 21.1 nm, and 30.4 nm channels, corresponding to the period of chaotic (re)appearance and CS-guided displacements of the magnetic islands. QPPs appear once in the SDO/AIA 9.4 nm and 33.5 nm channels after the disruption of the CS by resistive instabilities and in the 19.3 nm channel when the chaotic motion of the magnetic islands reappears.<br />The content of the paper has been published on ApJ. This version on arXiv is an improved version of the published one in ApJ, and some typos in the published one have been corrected
- Subjects :
- DYNAMICS
010504 meteorology & atmospheric sciences
PHASE
FOS: Physical sciences
Flux
Astrophysics
Astronomy & Astrophysics
01 natural sciences
magnetohydrodynamics (MHD)
Current sheet
SOLAR-FLARE
0103 physical sciences
RECONNECTION
Astrophysics::Solar and Stellar Astrophysics
010303 astronomy & astrophysics
Solar and Stellar Astrophysics (astro-ph.SR)
0105 earth and related environmental sciences
High Energy Astrophysical Phenomena (astro-ph.HE)
Physics
PULSATIONS
Resistive touchscreen
Science & Technology
Solar flare
Astronomy and Astrophysics
Magnetic reconnection
numerical [methods]
Light curve
Magnetic flux
coronal mass ejections (CMEs) [Sun]
flares [Sun]
Astrophysics - Solar and Stellar Astrophysics
13. Climate action
Space and Planetary Science
magnetic reconnection
thermal [radiation mechanisms]
Physics::Space Physics
Physical Sciences
Magnetohydrodynamics
CURRENT SHEET
Astrophysics - High Energy Astrophysical Phenomena
Subjects
Details
- ISSN :
- 15384357, 0004637X, and 00670049
- Database :
- OpenAIRE
- Journal :
- The Astrophysical Journal
- Accession number :
- edsair.doi.dedup.....f52b19e5a2d7ddbaef7ace2ff0ed3dca
- Full Text :
- https://doi.org/10.3847/1538-4357/ab0284