期刊
ASTROPHYSICAL JOURNAL
卷 746, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/746/2/183
关键词
magnetohydrodynamics (MHD); methods: numerical; Sun: atmosphere; Sun: oscillations; Sun: photosphere
资金
- Science and Technology Facilities Council (STFC)
- Northern Ireland Department of Education and Learning
- CSUN College of Science
- European Office of Aerospace Research and Development
- STFC [ST/I001123/1, ST/K001620/1, ST/G004986/1, ST/H000852/1, ST/I00016X/1, ST/F002270/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K001620/1, ST/I001123/1, ST/I00016X/1, ST/G004986/1, ST/F002270/1, ST/H000852/1] Funding Source: researchfish
We present high-cadence observations and simulations of the solar photosphere, obtained using the Rapid Oscillations in the Solar Atmosphere imaging system and the MuRAM magnetohydrodynamic (MHD) code, respectively. Each data set demonstrates a wealth of magnetoacoustic oscillatory behavior, visible as periodic intensity fluctuations with periods in the range 110-600 s. Almost no propagating waves with periods less than 140 s and 110 s are detected in the observational and simulated data sets, respectively. High concentrations of power are found in highly magnetized regions, such as magnetic bright points and intergranular lanes. Radiative diagnostics of the photospheric simulations replicate our observational results, confirming that the current breed of MHD simulations are able to accurately represent the lower solar atmosphere. All observed oscillations are generated as a result of naturally occurring magnetoconvective processes, with no specific input driver present. Using contribution functions extracted from our numerical simulations, we estimate minimum G-band and 4170 angstrom continuum formation heights of 100 km and 25 km, respectively. Detected magnetoacoustic oscillations exhibit a dominant phase delay of -8 degrees between the G-band and 4170 angstrom continuum observations, suggesting the presence of upwardly propagating waves. More than 73% of MBPs (73% from observations and 96% from simulations) display upwardly propagating wave phenomena, suggesting the abundant nature of oscillatory behavior detected higher in the solar atmosphere may be traced back to magnetoconvective processes occurring in the upper layers of the Sun's convection zone.
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