Speaker
Description
Atmospheric gravity waves (AGWs) are low-frequency, buoyancy-driven waves generated by turbulent convection in the lower solar atmosphere. In addition to their role as energy agents and coupling atmospheric layers, simulations showcase their sensitivity to the average magnetic field topology. Using multi-height IBIS/DST and HMI/SDO velocity and magnetic field observations, we investigate the characteristics of AGWs throughout the lower solar atmosphere in different magnetic field configurations and disk positions. Employing Fourier analysis and local helioseismology techniques, we detect propagating AGWs carrying energy upward at the expected temporal and spatial scales consistent with independent observations, theory, and COBOLD numerical simulations. Using the data derived from HMI SHARP vector magnetograms and moving away from the traditional k-$\omega$ diagnostic diagram, we disentangle the effects of the magnetic field on their behavior. We show that AGWs are suppressed and/or reflected in regions of vertically inclined intermediate to large magnetic fields (|B| > 30 G) in the upper photosphere. At the same time, they propagate unhindered in quiet-Sun transverse fields, in line with COBOLD numerical simulations. This highlights their potential as novel diagnostics for probing the upper photospheric magnetic field.
| Sessions | Seismology of solar and stellar atmospheres |
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