Internal Gravity Waves in the Magnetized Solar Atmosphere. II. Energy Transport

Abstract

In this second paper of the series on internal gravity waves (IGWs), we present a study of the generation and propagation of IGWs in a model solar atmosphere with diverse magnetic conditions. A magnetic field free, and three magnetic models that start with an initial, vertical, homogeneous field of 10 G, 50 G, and 100 G magnetic flux density, are simulated using the CO${}^5$BOLD code. We find that the IGWs are generated in similar manner in all four models in spite of the differences in the magnetic environment. The mechanical energy carried by IGWs is significantly larger than that of the acoustic waves in the lower part of the atmosphere, making them an important component of the total wave energy budget. The mechanical energy flux (10${}^6$ - 10${}^3$ W m${}^{-2}$) is few orders of magnitude larger than the Poynting flux (10${}^3$ - 10${}^1$ W m${}^{-2}$). The Poynting fluxes show a downward component in the frequency range corresponding to the IGWs, which confirm that these waves do not propagate upwards in the atmosphere when the fields are predominantly vertical and strong. We conclude that, in the upper photosphere, the propagation properties of IGWs depend on the average magnetic field strength and therefore these waves can be potential candidate for magnetic field diagnostics of these layers. However, their subsequent coupling to Alfvénic waves are unlikely in a magnetic environment permeated with predominantly vertical fields and therefore they may not directly or indirectly contribute to the heating of layers above plasma-$\beta$ less than 1.

To appear in ApJ, 15 pages, 9 figures, 1 video

References in corpus (15)

• The NumPy array: a structure for efficient numerical computation
• A grid of MARCS model atmospheres for late-type stars I. Methods and general properties
• Asymptotic g modes: Evidence for a rapid rotation of the solar core
• On the Chemical Mixing Induced by Internal Gravity Waves (IGW)
• The horizontal internetwork magnetic field: numerical simulations in comparison to observations with Hinode
• Theoretical seismology in 3D : nonlinear simulations of internal gravity waves in solar-like stars
• Can plume-induced internal gravity waves regulate the core rotation of subgiant stars?
• Conversion of Internal Gravity Waves into Magnetic Waves
• Nonlinear Dynamics of Gravity Wave Driven Flows in the Solar Radiative Interior
• Internal Gravity Waves in the Magnetized Solar Atmosphere. I. Magnetic Field Effects
• Magnetoacoustic Waves in a Stratified Atmosphere with a Magnetic Null Point
• Chromospheric and Coronal Wave Generation in a Magnetic Flux Sheath
• First local helioseismic experiments with CO5BOLD
• Three-dimensional hydrodynamical CO5BOLD model atmospheres of red giant stars VI. First chromosphere model of a late-type giant
• The polarization signature of photospheric magnetic fields in 3D MHD simulations and observations at disk center

Cited by in corpus (3)

• Synthetic observations of internal gravity waves in the solar atmosphere
• Multi-Height Observations of Atmospheric Gravity Waves at Solar Disk Center
• On the propagation of gravity waves in the lower solar atmosphere in different magnetic configurations