Abstract
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 Å
continuum formation heights of 100 km and 25 km, respectively. Detected magnetoacoustic oscillations exhibit a
dominant phase delay of −8◦ between the G-band and 4170 Å 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.
Original language | English |
---|---|
Article number | 183 |
Pages (from-to) | 1-12 |
Number of pages | 12 |
Journal | Astrophysical Journal |
Volume | 746 |
DOIs | |
Publication status | Published - 20 Feb 2012 |
ASJC Scopus subject areas
- Space and Planetary Science
- Astronomy and Astrophysics