Dependence of sunspot photospheric waves on the depth of the source of solar $p-$modes

Abstract

Photospheric waves in sunspots moving radially outwards at speeds faster than the characteristic wave velocities have been recently detected. It has been suggested that they are the visual pattern of $p-$modes excited around 5 Mm beneath the sunspot. Using numerical simulations, we have performed a parametric study of the waves observed at the photosphere and higher layers produced by sources located at different depths. The observational measurements are consistent with waves driven between approximately 1 Mm and 5 Mm below the sunspot surface.

Accepted for publication in A&A

References in corpus (6)

• Helioseismology of Sunspots: Confronting Observations with Three-Dimensional MHD Simulations of Wave Propagation
• MHS sunspot model from deep sub-photospheric to chromospheric layers
• MHD wave propagation from the sub-photosphere to the corona in an arcade-shaped magnetic field with a null point
• Influence of Non-Uniform Distribution of Acoustic Wavefield Strength on Time-Distance Helioseismology Measurements
• Modified p-modes in penumbral filaments?
• Helioseismic holography of simulated sunspots: magnetic and thermal contributions to travel times

Cited by in corpus (6)

• The Physical Nature of Spiral Wave Patterns in Sunspots
• Source Depth of Three-minute Umbral Oscillations
• Oscillations In The Line-of-Sight Magnetic Field Strength In A Pore Observed By The GREGOR Infrared Spectrograph (GRIS)
• A theoretic analysis of magnetoactive GES-based turbulent solar plasma instability
• Investigation of the subsurface structure of a sunspot based on the spatial distribution of oscillation centers inferred from umbral flashes
• Origin of the Chromospheric Umbral Waves in Sunspots