Internal wave generation by tidal flow over a two-dimensional ridge: energy flux asymmetries induced by a steady surface trapped current

2017 ◽  
Vol 836 ◽  
pp. 192-221 ◽  
Author(s):  
Kevin G. Lamb ◽  
M. Dunphy
Keyword(s):  
Total Energy ◽  
Wave Field ◽  
Energy Flux ◽  
Tidal Flow ◽  
Surface Current ◽  
Equation Model ◽  
Two Dimensional ◽  
Total Energy Flux ◽  
Effects Of Rotation ◽  
Internal Wave Generation

The effects of a surface trapped steady background current on internal waves generated by tidal currents oscillating over a small symmetric ridge are investigated using a two-dimensional primitive equation model. A rigid lid is used with a linearly stratified fluid and the effects of rotation are not considered. We consider uni-directional background currents $\bar{U}(z)\geqslant 0$ confined to a surface layer lying well above the ridge. The current introduces asymmetries in the generated wave field. For sufficiently narrow ridges the upstream energy flux is larger than the downstream flux while the opposite is the case for sufficiently wide ridges. The total energy flux radiating away from the ridge is not significantly affected by the current. Mean second-order currents and pressure fields are shown to make important contributions to the total energy flux. A first-order linear theory, valid for a general stratification and surface current, which accurately predicts the wave field is also developed.

scholarly journals Diagnostics of Non-thermal Particles in Solar Chromospheric Flares

2004 ◽  
Vol 219 ◽  
pp. 171-175
Author(s):  
C. Fang ◽  
Z. Xu ◽  
M. D. Ding
Keyword(s):  
Total Energy ◽  
Energy Flux ◽  
Atmospheric Condition ◽  
Particle Beam ◽  
Profile Measurement ◽  
Solar Chromosphere ◽  
Line Profiles ◽  
Total Energy Flux ◽  
Hydrogen Lines ◽  
Semi Empirical

Particle beam bombardment on the solar chromosphere produces non-thermal ionization and excitation. The effect on hydrogen lines is investigated by using non-LTE theory and semi-empirical flare models. It has been found that in the case of electron bombardment, the Hα line is widely broadened and enhanced. Significant enhancements at the wings of Lyα and Lyβ lines are also predicted. In the case of proton bombardment, less strong broadening and less central reversal are expected. We found that the total energy flux of the particle beam and the atmospheric condition give much influence on the line profiles, which, however, are less sensitive to the power index. Based on the Hα line profile measurement, a method to deduce the total energy flux of the particle beam is proposed.

scholarly journals The Total Energy Flux Leaving the Ocean’s Mixed Layer

2016 ◽  
Vol 46 (6) ◽  
pp. 1885-1900 ◽  
Author(s):  
Antonija Rimac ◽  
Jin-Song von Storch ◽  
Carsten Eden
Keyword(s):  
Total Energy ◽  
Wind Stress ◽  
Energy Flux ◽  
Mixed Layer ◽  
General Circulation ◽  
Circulation Model ◽  
Power Input ◽  
Ocean General Circulation Model ◽  
Wind Stress Curl ◽  
Total Energy Flux

AbstractThe total energy flux leaving the ocean’s spatially and seasonally varying mixed layer is estimated using a global ⅝1/10° ocean general circulation model. From the total wind-power input of 3.33 TW into near-inertial waves (0.35 TW), subinertial fluctuations (0.87 TW), and the time-mean circulation (2.11 TW), 0.92 TW leave the mixed layer, with 0.04 TW (11.4%) due to near-inertial motions, 0.07 TW (8.04%) due to subinertial fluctuations, and 0.81 TW (38.4%) due to time-mean motions. Of the 0.81 TW from the time-mean motions, 0.5 TW result from the projection of the horizontal flux onto the sloped bottom of the mixed layer. This projection is negligible for the transient fluxes. The spatial structure of the vertical flux is determined principally by the wind stress curl. The mean and subinertial fluxes leaving the mixed layer are approximately 40%–50% smaller than the respective fluxes across the Ekman layer according to the method proposed by Stern. The fraction related to transient fluctuations tends to decrease with increasing depth of the mixed layer and with increasing strength of wind stress variability.

scholarly journals Total energy flux in a marine bioluminescent bacterium

1989 ◽  
Vol 57 (2) ◽  
pp. 161-165 ◽  
Author(s):  
John C. Makemson ◽  
Andrew S. Gordon
Keyword(s):  
Total Energy ◽  
Energy Flux ◽  
Bioluminescent Bacterium ◽  
Total Energy Flux

scholarly journals Kinematics and Energetics of A Solar Jet from NOAA Active Region 12297

2019 ◽  
Vol 14 (1) ◽  
Author(s):  
Reetika Joshi ◽  
Ramesh Chandra
Keyword(s):  
Active Region ◽  
Total Energy ◽  
Energy Flux ◽  
Solar Active Region ◽  
Active Region Noaa ◽  
Solar Dynamics Observatory ◽  
Total Energy Flux ◽  
Region Noaa ◽  
Solar Dynamics ◽  
Noaa Active Region

In this article, we have presented the study of a solar jet on March 14, 2015 recorded from the Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) satellite. The jet was observed from the solar active region NOAA AR 12297. We have discussed the dynamics and calculated the various possible energy contents of the observed jet. The estimated total energy flux liberated during the jet ejection was 2.1 x 107 erg cm-2 s-1 .

scholarly journals Helically decomposed turbulence

2017 ◽  
Vol 812 ◽  
pp. 752-770 ◽  
Author(s):  
Alexandros Alexakis
Keyword(s):  
Total Energy ◽  
Numerical Simulations ◽  
Energy Flux ◽  
Large Scale ◽  
Inertial Range ◽  
Inverse Cascade ◽  
New Directions ◽  
Total Energy Flux

A decomposition of the energy and helicity fluxes is used to analyse turbulent hydrodynamic flows. The decomposition is based on the projection of the flow to a helical basis. This allows the roles of interactions among modes of different helicities to be investigated separately. The proposed formalism is applied to large-scale numerical simulations of non-helical and helical flows, where the decomposed fluxes are explicitly calculated. It is shown that the total energy flux can be split into three fluxes that independently remain constant in the inertial range. One of these fluxes which corresponds to the interactions of fields with the same helicity is negative, implying the presence of an inverse cascade that is ‘hidden’ inside the forward cascade. Similarly to the energy flux, it is also shown that the helicity flux can be decomposed into two fluxes that remain constant in the inertial range. Implications of these results as well as possible new directions for investigations are discussed.

scholarly journals Kinematics and Energetics of A Solar Jet from NOAA Active Region 12297

2019 ◽  
Vol 14 (1) ◽  
Author(s):  
Reetika Joshi ◽  
Ramesh Chandra
Keyword(s):  
Active Region ◽  
Total Energy ◽  
Energy Flux ◽  
Solar Active Region ◽  
Active Region Noaa ◽  
Solar Dynamics Observatory ◽  
Total Energy Flux ◽  
Region Noaa ◽  
Solar Dynamics ◽  
Noaa Active Region

In this article, we have presented the study of a solar jet on March 14, 2015 recorded from the Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) satellite. The jet was observed from the solar active region NOAA AR 12297. We have discussed the dynamics and calculated the various possible energy contents of the observed jet. The estimated total energy flux liberated during the jet ejection was 2.1 x 107 erg cm-2 s-1 .

scholarly journals Angular Diameters of Cool Stars Measured by the Method of Lunar Occultations

1978 ◽  
Vol 80 ◽  
pp. 447-450
Author(s):  
Nathaniel M. White
Keyword(s):  
Total Energy ◽  
Energy Flux ◽  
Spectral Type ◽  
Effective Temperature ◽  
Angular Diameter ◽  
Cool Stars ◽  
Total Energy Flux ◽  
Photoelectric Observations ◽  
Angular Diameters

Given the angular diameter and total energy flux of a star, its effective temperature can be determined. Until recently, there were few well-determined angular diameters of cool stars, and effective temperature calibrations rested on angular diameter measurements of several not necessarily “normal” stars. The number of measured angular diameters of stars cooler than about spectral type G is steadily being increased by using the method of photoelectric observations of lunar occultations.

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