Cattaneo–Christov heat flux model on Blasius–Rayleigh–Stokes flow through a transitive magnetic field and Joule heating

2020 ◽  
Vol 548 ◽  
pp. 123991 ◽  
Author(s):  
M. Gnaneswara Reddy ◽  
M.V. V. N.L. Sudha Rani ◽  
K. Ganesh Kumar ◽  
B.C. Prasannakumar ◽  
Ali J. Chamkha
Keyword(s):  
Magnetic Field ◽  
Heat Flux ◽  
Joule Heating ◽  
Stokes Flow ◽  
Flux Model ◽  
Flow Through ◽  
Heat Flux Model

scholarly journals MHD Slip Flow of CNT-Ethylene Glycol Nanofluid due to a Stretchable Rotating Disk with Cattaneo–Christov Heat Flux Model

2020 ◽  
Vol 2020 ◽  
pp. 1-13 ◽  
Author(s):  
Ayele Tulu ◽  
Wubshet Ibrahim
Keyword(s):  
Magnetic Field ◽  
Boundary Layer ◽  
Heat Flux ◽  
Ethylene Glycol ◽  
Layer Thickness ◽  
Boundary Layer Thickness ◽  
Rotating Disk ◽  
Temperature Fields ◽  
Flux Model ◽  
Heat Flux Model

This article deals with carbon nanoliquid flow due to stretchable rotating disk with the effect of Cattaneo–Christov heat flux model. Both SWCNTs and MWCNTs are considered with ethylene glycol as the base fluid. The effects of nanoparticle volume friction, normally applied magnetic field, stretching factor, velocity, and thermal slip factors are examined. The fundamental flow governing equations are transformed into dimensionless system of coupled nonlinear ordinary differential equations, and they are solved numerically using spectral quasi-linearization method (SQLM). Employing graphs and tables, the results of velocity and temperature fields as well as skin friction coefficient and local heat transfer rate are analyzed and presented via embedded parameters. The results reveal that higher velocity fields and lower temperature fields are noticed in the MWCNT nanofluids than SWCNT nanofluids. The higher incidence of magnetic field improves the thermal boundary layer thickness. A growth in velocity slip factor reduces the momentum boundary layer thickness of the nanoliquid flow. Generally, radial stretching of the disk is helpful in improving the cooling process of the rotating disk in practical applications.

scholarly journals Nonlocal heat flux effects on temperature evolution of the solar atmosphere

2018 ◽  
Vol 615 ◽  
pp. A32
Author(s):  
S. S. A. Silva ◽  
J. C. Santos ◽  
J. Büchner ◽  
M. V. Alves
Keyword(s):  
Magnetic Field ◽  
Heat Flux ◽  
Solar Corona ◽  
Heat Transport ◽  
Transition Region ◽  
Solar Atmosphere ◽  
Energy Transport ◽  
Flux Model ◽  
The Impact ◽  
Heat Flux Model

Context. Heat flux is one of the main energy transport mechanisms in the weakly collisional plasma of the solar corona. There, rare binary collisions let hot electrons travel over long distances and influence other regions along magnetic field lines. Thus, the fully collisional heat flux models might not describe transport well enough since they consider only the local contribution of electrons. The heat flux in weakly collisional plasmas at high temperatures with large mean free paths has to consider the nonlocality of the energy transport in the frame of nonlocal models in order to treat energy balance in the solar atmosphere properly. Aims. We investigate the impact of nonlocal heat flux on the thermal evolution and dynamics of the solar atmosphere by implementing a nonlocal heat flux model in a 3D magnetohydrodynamic simulation of the solar corona. Methods. We simulate the evolution of solar coronal plasma and magnetic fields considering both a local collision dominated and a nonlocal heat flux model. The initial magnetic field is obtained by a potential extrapolation of the observed line-of-sight magnetic field of AR11226. The system is perturbed by moving the plasma at the photosphere. We compared the simulated evolution of the solar atmosphere in its dependence on the heat flux model. Results. The main differences for the average temperature profiles were found in the upper chromosphere/transition region. In the nonlocal heat transport model case, thermal energy is transported more efficiently to the upper chromosphere and lower transition region and leads to an earlier heating of the lower atmosphere. As a consequence, the structure of the solar atmosphere is affected with the nonlocal simulations producing on average a smoother temperature profile and the transition region placed about 500 km higher. Using a nonlocal heat flux also leads to two times higher temperatures in some of the regions in the lower corona. Conclusions. The results of our 3D MHD simulations considering nonlocal heat transport supports the previous results of simpler 1D two-fluid simulations. They demonstrated that it is important to consider a nonlocal formulation for the heat flux when there is a strong energy deposit, like the one observed during flares, in the solar corona.

Hybrid dusty fluid flow through a Cattaneo–Christov heat flux model

2020 ◽  
Vol 551 ◽  
pp. 123975 ◽  
Author(s):  
M. Gnaneswara Reddy ◽  
M.V.V.N.L. Sudha Rani ◽  
K. Ganesh Kumar ◽  
B.C. Prasannakumar ◽  
H.J. Lokesh
Keyword(s):  
Heat Flux ◽  
Fluid Flow ◽  
Dusty Fluid ◽  
Flux Model ◽  
Flow Through ◽  
Heat Flux Model
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