Transmission of acoustic wave energy across a magnetic flux sheath

Solar Physics ◽  
1977 ◽  
Vol 54 (2) ◽  
pp. 371-375
Author(s):  
P. Venkatakrishnan ◽  
M. H. Gokhale
1976 ◽  
Vol 47 (11) ◽  
pp. 4800-4803
Author(s):  
G. Cambon ◽  
A. Saïssy ◽  
M. Rouzeyre

2017 ◽  
Vol 96 (2) ◽  
Author(s):  
Benjamin A. Jorns ◽  
Christoper Dodson ◽  
Dan M. Goebel ◽  
Richard Wirz

2016 ◽  
Vol 54 (1) ◽  
pp. 56-61 ◽  
Author(s):  
G. R. Izmailova ◽  
L. A. Kovaleva ◽  
N. M. Nasyrov

Author(s):  
D E Fawzy ◽  
A T Saygac ◽  
K Stȩpień

Abstract The aim of the current study is the computation of the magnetic flux tube wave energies and fluxes generated in the convection zone of Procyon A. This is a subgiant of spectral type F5 IV-V showing chromospheric and coronal activities. The mechanisms responsible for the generation of different wave modes include the interaction of the thin and vertically oriented magnetic flux tube embedded in magnetic-free regions with turbulence in the convection zone of Procyon A. We are considering longitudinal, transverse and acoustic wave modes. Turbulence in the convection zone is modeled by the extended Kolmogorov turbulent energy spectrum and the modified Gaussian frequency factor. Different magnetic flux tube models with different degrees of magnetic activities were considered. The current approach takes the nonlinear effects into consideration. The results show that there is enough wave energy in the three different forms to heat the outer layers of the star. The obtained acoustic wave energies are larger than those of the longitudinal tube wave energies compared to the solar case. This can be explained by the relatively low magnetic field strength. On the other side, our computations show the importance of the transverse wave energies compared to the energies carried by the longitudinal waves. The former waves carry energy several (between 2 and 14) times higher than the latter. The obtained wave energies are essential for constructing time-dependent model chromospheres and for the predictions of atmospheric oscillations to be compared e.g. with the data collected by the CoRoT and Kepler missions.


2015 ◽  
Vol 29 (4) ◽  
pp. 611-621 ◽  
Author(s):  
Chao-feng Lan ◽  
Feng-chen Li ◽  
Huan Chen ◽  
Di Lu ◽  
De-sen Yang ◽  
...  

1987 ◽  
Vol 122 ◽  
pp. 325-326 ◽  
Author(s):  
M. Cuntz ◽  
L. Hartmann ◽  
P. Ulmschneider

Mass loss generated by radiatively damped acoustic waves is investigated. We find that a persistent wave energy flux leads to extended chromospheres. Mass loss is quite likely produced if the wave field retains a transient character and if large wave periods are used.


1987 ◽  
Vol 65 (4) ◽  
pp. 357-358
Author(s):  
Bhimsen K. Shivamoggi

A new mechanism for the resonant absorption of a shear Alfvén wave is proposed that involves a direct mode conversion of the latter to an ion-acoustic wave without bringing in the intermediary — the kinetic Alfvén wave. The fraction of the incident Alfvén-wave energy that is mode-converted to an ion-acoustic wave is calculated. This mechanism likely operates in the solar wind, where it might lead to heating of the plasma.


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