Propagating wave phenomena detected in observations and simulations of the lower solar atmosphere

Jess, DB, Shelyag, Sergiy, Mathioudakis, M, Keys, PH, Christian, DJ and Keenan, FP 2012, Propagating wave phenomena detected in observations and simulations of the lower solar atmosphere, Astrophysical journal, vol. 746, no. 2, pp. 1-12, doi: 10.1088/0004-637X/746/2/183.

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Title Propagating wave phenomena detected in observations and simulations of the lower solar atmosphere
Author(s) Jess, DB
Shelyag, SergiyORCID iD for Shelyag, Sergiy orcid.org/0000-0002-6436-9347
Mathioudakis, M
Keys, PH
Christian, DJ
Keenan, FP
Journal name Astrophysical journal
Volume number 746
Issue number 2
Article ID 183
Start page 1
End page 12
Total pages 12
Publisher IOP Publishing
Place of publication Bristol, Eng.
Publication date 2012-02-20
ISSN 0004-637X
1538-4357
Keyword(s) magnetohydrodynamics (MHD)
methods: numerical
Sun: atmosphere
Sun: oscillations
Sun: photosphere
Science & Technology
Physical Sciences
Astronomy & Astrophysics
Summary 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 100km and 25km, 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.
Language eng
DOI 10.1088/0004-637X/746/2/183
Field of Research 0201 Astronomical And Space Sciences
0305 Organic Chemistry
0306 Physical Chemistry (Incl. Structural)
HERDC Research category C1.1 Refereed article in a scholarly journal
Copyright notice ©2012, The American Astronomical Society
Persistent URL http://hdl.handle.net/10536/DRO/DU:30114960

Document type: Journal Article
Collection: School of Information Technology
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