On the Generation of Flux‐Tube Waves in Stellar Convection Zones. III. Longitudinal Tube Wave‐Energy Spectra and Fluxes for Late‐Type Stars

2000 ◽  
Vol 541 (1) ◽  
pp. 410-417 ◽  
Author(s):  
Z. E. Musielak ◽  
R. Rosner ◽  
P. Ulmschneider
Keyword(s):  
Flux Tube ◽  
Wave Energy ◽  
Energy Spectra ◽  
Late Type ◽  
Stellar Convection ◽  
Tube Wave

On the Generation of Flux‐Tube Waves in Stellar Convection Zones. IV. Longitudinal Wave Energy Spectra and Fluxes for Stars with Nonsolar Metallicities

2002 ◽  
Vol 573 (1) ◽  
pp. 418-424 ◽  
Author(s):  
Z. E. Musielak ◽  
R. Rosner ◽  
P. Ulmschneider
Keyword(s):  
Longitudinal Wave ◽  
Flux Tube ◽  
Wave Energy ◽  
Energy Spectra ◽  
Stellar Convection

On the Generation of Flux-Tube Waves in Stellar Convection Zones. II. Improved Treatment of Longitudinal Tube Wave Generation

1995 ◽  
Vol 448 ◽  
pp. 865 ◽  
Author(s):  
Z. E. Musielak ◽  
R. Rosner ◽  
H. P. Gail ◽  
P. Ulmschneider
Keyword(s):  
Flux Tube ◽  
Wave Generation ◽  
Stellar Convection ◽  
Tube Wave

Approximate non-relativistic s-wave energy spectra with non-polynomial potentials within the framework of the WKB approximation

2021 ◽  
Author(s):  
E. Omugbe ◽  
O. E. Osafile ◽  
E. A. Enaibe ◽  
M. C. Onyeaju ◽  
E. Akpata
Keyword(s):  
Wave Energy ◽  
Wkb Approximation ◽  
Energy Spectra ◽  
S Wave ◽  
Polynomial Potentials

scholarly journals Linking Thin Flux Tube MHD Models to Apparent Stellar Surface Activity

2004 ◽  
Vol 219 ◽  
pp. 546-551
Author(s):  
T. Granzer ◽  
K. G. Strassmeier
Keyword(s):  
Magnetic Flux ◽  
Surface Activity ◽  
Flux Tube ◽  
Convection Zone ◽  
Active Regions ◽  
Similar Model ◽  
Flux Tubes ◽  
Stellar Convection ◽  
Magnetic Flux Tubes ◽  
Spot Formation

We model thin magnetic flux tubes as they rise from the bottom of a stellar convection zone to the photosphere. On emergence they form active regions, i.e. star spots. This model was very successfully applied to the solar case, where the simulations where in agreement with the butterfly diagram, Joy's law, and Hale's law. We propose the use of a similar model to describe stellar activity in the more extreme form found on active stars. A comparison between Doppler-images of well-observed pre-MS stars and a theoretically derived probability of star-spot formation as a function of latitude is presented.

Generation of nonlinear magnetic flux tube wave energies in Procyon A

2019 ◽  
Author(s):  
D E Fawzy ◽  
A T Saygac ◽  
K Stȩpień
Keyword(s):  
Magnetic Flux ◽  
Acoustic Wave ◽  
Flux Tube ◽  
Convection Zone ◽  
Frequency Factor ◽  
Turbulent Energy ◽  
Current Approach ◽  
Magnetic Flux Tube ◽  
Tube Wave ◽  
Wave Modes

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.

On the generation of flux tube waves in stellar convection zones. I - Longitudinal tube waves driven by external turbulence

1989 ◽  
Vol 337 ◽  
pp. 470 ◽  
Author(s):  
Z. E. Musielak ◽  
R. Rosner ◽  
P. Ulmschneider
Keyword(s):  
Flux Tube ◽  
Stellar Convection ◽  
External Turbulence

Wave energy in white dwarf atmospheres. I - Magnetohydrodynamic energy spectra for homogeneous DB and layered DA stars

1987 ◽  
Vol 322 ◽  
pp. 234 ◽  
Author(s):  
Zdzislaw E. Musielak
Keyword(s):  
Wave Energy ◽  
White Dwarf ◽  
Energy Spectra

scholarly journals Wave–structure interactions for the distensible tube wave energy converter

2016 ◽  
Vol 472 (2192) ◽  
pp. 20160160
Author(s):  
Warren R. Smith
Keyword(s):  
Wave Energy ◽  
Sea Water ◽  
Wave Structure ◽  
Complex Interaction ◽  
Wave Energy Converter ◽  
Sea Waves ◽  
Energy Converter ◽  
Distensible Tube ◽  
Tube Wave ◽  
Work Done

A comprehensive linear mathematical model is constructed to address the open problem of the radiated wave for the distensible tube wave energy converter. This device, full of sea water and located just below the surface of the sea, undergoes a complex interaction with the waves running along its length. The result is a bulge wave in the tube which, providing certain criteria are met, grows in amplitude and captures the wave energy through the power take-off mechanism. Successful optimization of the device means capturing the energy from a much larger width of the sea waves (capture width). To achieve this, the complex interaction between the incident gravity waves, radiated waves and bulge waves is investigated. The new results establish the dependence of the capture width on absorption of the incident wave, energy loss owing to work done on the tube, imperfect tuning and the radiated wave. The new results reveal also that the wave–structure interactions govern the amplitude, phase, attenuation and wavenumber of the transient bulge wave. These predictions compare well with experimental observations.

The Effect of Wave Energy Spectra on Wave Run-Up

1969 ◽  
Author(s):  
J. H. van Oorschot ◽  
K. d'Angremond
Keyword(s):  
Wave Energy ◽  
Energy Spectra ◽  
Run Up
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