Entropy analysis for MHD flow over a non-linear stretching inclined transparent plate embedded in a porous medium due to solar radiation/Magnetinio hidrodinaminio tekejimo per netiesiskai itempta pasvirusia permatoma plokste, esancia poringoje aplinkoje priklausomybes nuo saules radiacijos entropijos analize.

Dehsara, M. ; Matin, M. Habibi ; Dalir, N. 等

1. Introduction

In the last three decades, fluid convection in porous medium has been one of the interesting subjects in heat transfer field. The researches show that the presence of porous medium makes the thermal conditions much better. Furthermore, another subject in heat transfer field which has been considerably taken into account by scientists and engineers is the use of nanofluids for the enhancement of conductive heat transfer coefficient and finally increasing the convective heat transfer rate. The convective heat transfer of fluid over an inclined plate which is embedded in a porous medium due to solar radiation has many applications such as petroleum material production, separation processes in chemical engineering, solar collectors, thermal insulation systems, buildings and nuclear reactors. Many works have been done in this field, some which are pointed out here.

Cheng and Minkowycz [1] studied the natural convection over a plate embedded in porous medium with surface temperature variation. Bejan and Polikakos [2] investigated the free convective boundary layer in porous medium for non-Darcian regime. The mixed convective flow boundary layer over a vertical plate in porous medium was analysed by Merkin [3]. Kim and Vafai [4] studied the natural convective flow over a vertical plate embedded in porous medium. Chamkha [5] investigated the free convective flow in porous medium with uniform porosity ratio due to solar radiation flux. The magneto hydrodynamic (MHD) mixed convective flow over a vertical porous plate in porous saturated medium and assuming non-Darcian model was studied by Takhar and Beg [6]. Ranganathan and Viskanta [7] investigated the fluid mixed convective boundary layer over a vertical plate embedded in porous medium. They claimed that the viscous effects are significant and cannot be neglected. Kayhani, Khaje and Sadi [8] studied the natural convection boundary layer along impermeable inclined surfaces embedded in porous medium. Chamkha et al. [9] also presented a nonsimilarity solution for natural convective flow over an inclined plate in porous medium due to solar radiation. Forced convection over a vertical plate in a porous medium was studied by Murthy et al. [10] with a non-Darcian model. They showed that the increase of solar radiation flux and also suction causes the increase of Nusselt number and heat transfer rate. Kayhani, Abbasi and Sadi [11] studied local thermal nonequilibrium in porous media due to temperature sudden change and heat generation.

Entropy generation is related to randomness and thermodynamic irreversibility, which is encountered in all heat transfer processes. There are various sources for entropy generation such as heat transfer and viscous dissipation [12, 13]. The investigation of entropy generation in a liquid film falling along an inclined plate was performed by Saouli and Ai Boud-Saouli [14]. Mahmud et al. [15] studied the case of mixed convection in a channel considering the effect of a magnetic field on the entropy generation. The effects of magnetic field and viscous dissipation on entropy generation in a falling liquid film were studied by Ai boud-Saouli et al. [16, 17].

In this paper, the MHD mixed convection flow and entropy generation have been studied over a nonlinearly stretching inclined transparent plate embedded in a porous medium with uniform porosity due to solar radiation flux. The boundary layer equations have been transformed by similarity transformation to two coupled nonlinear equations. These equations have been reduced to five first order nonlinear equations and then they have been transformed with an implicit method called Keller-Box and finally have been solved.

2. Mathematical analysis

Two-dimensional steady state boundary layer mixed convection MHD flow and entropy analysis has been considered over a smooth nonlinearly stretching inclined transparent plate embedded in a porous medium with constant porosity due to solar radiation and assuming viscous dissipation and variable magnetic field. An incompressible fixed fluid with electrical conductivity in presence of magnetic field B(x) has been considered perpendicular to the plate. Fig. 1 shows the schematics of the physical model and system coordinates.

[FIGURE 1 OMITTED]

It is assumed that the x and y coordinates are the flow directions on the plate and perpendicular to the plate respectively. The plate temperature ([T.sub.w]) is assumed constant and it is considered higher than the ambient temperature ([T.sub.[infinity]]). Assuming incompressible viscous fluid and Boussinesq approximation, the governing equations are as follows

[[partial derivative]u/[partial derivative]x] + [[partial derivative]v/[partial derivative]y] = 0 (1)

[MATHEMATICAL EXPRESSION NOT REPRODUCIBLE IN ASCII] (2)

[MATHEMATICAL EXPRESSION NOT REPRODUCIBLE IN ASCII] (3)

The boundary conditions are

[MATHEMATICAL EXPRESSION NOT REPRODUCIBLE IN ASCII] (4)

where b is the stretching rate which is a constant u and v are the velocity components in x and y directions respectively, [sigma] is the electric conductivity, [gamma] is the plate inclination angle, [mu], [rho] and [beta] are the effective dynamic viscosity, effective density and effective thermal expansion coefficient of fluid respectively.

Also K([epsilon]) and C([epsilon]) are the porous medium permeability and inertia coefficient which have the following relations for uniform porosity [18]

k([epsilon]) = [d.sup.2.sub.p][[epsilon].sup.3]/175[(1 - [epsilon]).sup.2] (5)

C([epsilon]) = 1.75(1 - [epsilon])/[d.sub.p][[epsilon].sup.2] (6)

here [mu] is the dynamic viscosity of the fluid, [beta] is the thermal conductivity of the fluid and [epsilon] is the porosity and also [rho], [C.sub.p] are the fluid density, specific heat of the fluid. [epsilon] is the porosity of porous medium which is constant assuming uniform distribution of solid components and [d.sub.p] is the diameter of porous medium solid particles.

k is the effective thermal conductivity of porous medium and the Pr number is obtained using this effective conductivity and [q.sub.rad] is the solar radiation flux. Assuming that some of the solar radiation energy reaching the plate surface is absorbed by the fluid, the Beer law can be used in radiation absorption and written

q" (y) = q"(0)(1 - exp (-ay)) (7)

where q" (y) is the radiation flux reached to the distance y from the plate, is the incident flux to the plate and a is the extinction coefficient of the fluid. Also here the magnetic field function has been considered as follows [19, 20]

B(x) = [B.sub.0] [square root of [x.sup.m-1]] (8)

The following similarity variable have been used to transform the governing equations to ordinary differential equations

[eta] = [y/x] [square root of ([m + 1]/2)[Re.sub.x]] (9)

where

[Re.sub.x] = [[rho][u.sub.w](x)/[mu]] x (10)

The dimensionless stream and temperature functions are as follows

f([eta]) = [psi](x,y)[([Re.sub.x]).sup.1/2]/[u.sub.w](x) (11)

[theta]([eta]) = T - T[infinity]/[T.sub.w] - [T.sub.[infinity]] (12)

The stream function satisfies continuity equation

u = [partial derivative][PSI]/[partial derivative]y, v = -[partial derivative][PSI]/[partial derivative]x (13)

By the use of similarity parameters and their replacement in momentum and energy equations, the governing equations become

[MATHEMATICAL EXPRESSION NOT REPRODUCIBLE IN ASCII] (14)

[[theta].sub.[eta][eta]] + Pr f[[theta].sub.[eta]] + Ec Pr [f.sup.2.sub.[eta][eta]] + R/Re exp (-[a.sup.e][eta]/[square root of (Re)]) = 0 (15)

And the transformed boundary conditions become

[f.sub.[eta]] (0) = 1, f (0) = 0, [theta](0) = 1, [f.sub.[eta]] ([infinity]) = 0, [theta]([infinity]) = 0 (16)

The dimensionless parameters in the equations, R, [a.sub.e], Mn, [D.sub.p], [Re.sub.x], Pr, Ec, Gr/[Re.sub.x.sup.2], [C.sub.f] and Nu are radiation parameter, extinction parameter, magnetic parameter, porous medium geometric parameter and dimensionless Reynolds, Prandtl, Eckert, Richardson numbers, skin friction coefficient and Nusselt number respectively

[MATHEMATICAL EXPRESSION NOT REPRODUCIBLE IN ASCII] (17)

3. Analysis of entropy generation

According to Woods [21], the local volumetric rate of entropy generation in the presence of a magnetic field is given by the following relation

[MATHEMATICAL EXPRESSION NOT REPRODUCIBLE IN ASCII] (18)

Eq. (18) shows that the entropy generation is composed of three sources. The first term on the right-hand side of Eq. (18) is the entropy generation due to heat transfer across a finite temperature difference; the second term is the local entropy generation due to viscous dissipation, while the third term is the local entropy generation due to the effect of the magnetic field. It is appropriate to define dimensionless number for entropy generation rate [N.sub.S]. The entropy generation number is defined by dividing the local volumetric entropy generation rate [S.sub.G] to a characteristic entropy generation rate [([S.sub.G]).sub.0]. For prescribed boundary conditions the characteristic entropy generation rate can be written as

[([S.sub.G]).sub.0] = [k.sub.ef] [([DELTA]T).sup.2]/[x.sup.2][T.sup.2.sub.[infinity]] (19)

Thus the entropy generation number is written as

[N.sub.s] = [S.sub.G]/[([S.sub.G]).sub.0] (20)

Using Eqs. (9)-(11) and (18) entropy generation number is given by the following relation in terms of dimensionless velocity and temperature variables

[N.sub.s] = [Br Re/[OMEGA]] [f.sup.2.sub.[eta][eta]] + [Br[(Ha).sup.2]/[OMEGA]] [f.sup.2.sub.[eta]] + Re[[theta].sup.2.sub.[eta]] (21)

where

Br = [mu][u.sup.2.sub.w] = [OMEGA] = [DELTA]T/[T.sub.[infinity]], Ha = [B.sub.0]x [([sigma]/[mu]).sup.1/2]. (22)

4. Numerical method

Two dimensional equations of flow and energy for a vertical, nonlinear stretching plate have been considered. These equations include the viscous dissipation and variable (nonlinear) MHD. Then, they are transformed into similarity form. From similarity method, two nonlinear coupled equations are derived. The transformed coupled nonlinear ordinary differential Eqs. (14) and (15) subject to boundary conditions (16) are solved numericallyby using Keller-Box method. This method is second order accurate and allows nonuniform grid size.

First, the coupled boundary value problem of (14) and (15) in f and [theta] are reduced to a first order system of five simultaneous ordinary differential equations. Next, after choosing [[eta].sub.[infinity]], the numerical infinity, a grid for the closed interval [0, [[eta].sub.[infinity]] is chosen and the system of first order equations are transformed into a system of finite difference equations (FDEs) by replacing the differential terms by forward difference approximation and the non-differential terms by the average of two adjacent grid points. The numerical method gives approximate values of f, [f.sub.[eta]], [f.sub.[eta][eta]] and [theta], [theta][eta] at all the grid points. By adding the boundary conditions (16) to the system of FDEs, we obtain a nonlinear system of algebraic equations in which the number of equations and unknowns are the same. Subsequently, the linearization of these FDEs was done by Newton's method [22, 23, 24]. The resulting systems of linear equations were solved by a block tri-diagonal solver. The step size [DELTA][eta] in [eta] and the position of the edge of the boundary layer in [[eta].sub.[infinity]] are to be adjusted for different values of the parameters to maintain accuracy. A step size of [[DELTA].sub.[eta]] = 0.005 is selected which satisfies the convergence criterion of [10.sup.-4] in all cases. In this solution, [[eta].sub.[infinity]] = 5 is sufficient to apply the perfect effect of boundary layer.

5. Results and discussions

In this study, the entropy generation for two- dimensional steady-state boundary layer magneto- hydrodynamic mixed convection flow has been considered over a smooth nonlinearly stretching inclined transparent plate embedded in a porous medium due to solar radiation and with viscous dissipation and variable magnetic field.

The dimensionless temperature and velocity diagrams are plotted in terms of similarity variable for different values of governing parameters and in x = 0.1 and have been discussed in details. Some tables have also been presented for Nusselt number Nu and skin friction coefficient [C.sub.f].

In Figs. 2 to 7, [f.sub.[eta]] is the nondimensional velocity which is one on the sheet and also is zero in a distance sufficiently far away. Similarly, [theta] is implied as nondimensional temperature with the same limits of the nondimensional velocity.

Fig. 2 shows the dimensionless velocity profile for various values of porosity ratio ([epsilon]) and radiation Nu number ([Nu.sub.r]). It can be seen that the velocity in boundary layer increases with the increase of porosity ratio. The reason is that when porosity ratio increases, the fluid has much more possibility to move freely throughout the porous medium. It can also be seen that the velocity in the boundary layer increases with the increase of radiation Nu number. Because Nur is the amount of radiation flux approached to the surface of transparent sheet, when Nur increases, the energy of fluid particles increases which means the increase of velocity.

[FIGURE 2 OMITTED]

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Fig. 3 shows the dimensionless velocity profile for various values of Pr and Ec numbers. If the Pr number increases, the velocity in the boundary layer decreases. The reason is that, having specified properties and thermal conditions, the fluid viscosity increases with the increase of Pr number, and therefore it prevents the free motions of fluid particles. Also the velocity in the boundary layer increases with the increase of Eckert number.

Fig. 4 shows the dimensionless velocity profile for various values of magnetic parameter (Mn) and Pr number. As it is expected, the velocity in boundary layer reduces with the increase of Mn, and this is due to Lorentz force effect which resists the fluid flow. As it can be observed, this effect is independent of the fluid type.

The effect of the transparent plate inclination angle on fluid velocity is shown in Fig. 5. The plate inclination angles, [gamma], are considered 0[degrees] and 60[degrees] with respect to vertical plate. It can be seen that when the plate is inclined with [gamma] = 60[degrees], the particles motions is lower in porous medium than the case [gamma] = 0[degrees], and this is due to the larger gravitational acceleration component in fluid flow direction in [gamma] = 0[degrees] case which strengthens the buoyancy effect. Again as it can be seen, it is independent of the Pr number.

Fig. 6 shows the effect of geometric parameter of porous medium ([D.sub.p]) and Richardson number on velocity. As it can be observed, the velocity profiles translate above when the geometric parameter of porous medium [D.sub.p] increases. Another point which can be derived from diagram is that in Richardson numbers higher than 1 (Gr/[Re.sup.2] > 1) for which the natural convection is dominant, the velocity diagrams show peaks due to buoyancy effects.

Fig. 7 shows the velocity profiles for various values of effective extinction coefficient of porous medium and Pr numbers. It can be observed that the increase of extinction coefficient does not have much effect on velocity profile except at far points of the plate. The effect of [a.sub.e] on fluid velocity becomes more obvious with the reduction of Pr number. In other words, the effect of extinction coefficient on velocity of fluid particles becomes considerable with the reduction of viscosity.

The effect of porosity and radiation Nu number on dimensionless temperature profiles is shown in Fig. 8. It is seen that the reduction of porosity causes the temperature increase. The reason is that the more the porosity decreases, the lower the possibility of fluid motion will be and in fact the convective heat transfer mechanism weakens and it is only the heat conduction which performs the heat transfer. Also as it is expected, the increase of radiation Nu number increases temperature in fluid bulk.

Fig. 9 shows the dimensionless temperature profiles for various values of Eckert and Pr number. The increase of Pr number causes the reduction of thermal boundary layer thickness in porous medium. Conversely the increase of Ec number causes the increase of temperature in boundary layer, and this is due to friction and viscous effects which produces heat and the temperature increases.

[FIGURE 8 OMITTED]

[FIGURE 9 OMITTED]

[FIGURE 10 OMITTED]

[FIGURE 11 OMITTED]

Table presents the numerical values of the Nu number and skin friction coefficient, [C.sub.f], for various values of [epsilon], [D.sub.p], [Nu.sub.r], [gamma] and [a.sub.e]. An increase in [D.sub.p], in a specified [epsilon] and [Nu.sub.r], lead to an increase in [C.sub.f] and a decrease in Nu number. When [Nu.sub.r] or [epsilon] increases, [C.sub.f] increases and Nu decreases. Also an increase in [a.sub.e] or [gamma] leads to an increase in [C.sub.f] and a decrease in Nu number.

[FIGURE 12 OMITTED]

[FIGURE 13 OMITTED]

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[FIGURE 19 OMITTED]

Figs. 10 and 11 show the magnetic parameter effect and plate inclination angle effect on temperature profile for various Pr numbers respectively. It can be seen that the magnetic parameter and plate angle of inclination have almost no influence on temperature, and only in high Pr numbers, the increase of magnetic parameter causes the increase of temperature and the increase of plate inclination angle causes the slight temperature reduction.

The influence of geometric parameter of porous medium ([D.sub.p]) and Richardson number on dimensionless temperature profile is shown in Fig. 12. As it can be seen, in Richardson numbers higher than 1 (Gr/[Re.sup.2] > 1) for which the natural convection is dominant, the temperature profiles shift above when the geometric parameter of porous medium, [D.sub.p], increases. This is because when [D.sub.p] increases, motions of fluid particles in porous medium become restricted and this makes the contact of fluid with porous medium stronger and therefore the friction and fluid temperature increases. The interesting point is that this behavior is reverse for Richardson numbers equal to and smaller than 1 (Gr/[Re.sup.2] [less than or equal to] 1). As we know, in Richardson numbers smaller than 1, the forced convection is dominant, and in forced convection case, the external force causes the fluid motion and supplies energy of the fluid. Thus when Gr/[Re.sup.2] [less than or equal to] 1, the increase of [D.sub.p] does not have much effect on fluid temperature because the external force supplies the fluid particles energy which is lost due to the friction increase and therefore fluid temperature decrease. This can be a reason of inconsiderable effect of geometric parameter of porous medium on fluid temperature in Gr/[Re.sup.2] [less than or equal to] 1.

Fig. 13 shows the influence of effective extinction coefficient of porous medium on dimensionless temperature profile for various values of Pr number. It can be seen that the temperature profile shifts above with the increase of effective extinction coefficient. This is because when ae increases, the amount of heat absorption of the fluid increases. The black color of solid particles present in porous medium can also cause the increase of effective extinction coefficient and finally the fluid temperature.

Fig. 14 shows the influence of Eckert number on entropy generation number, [N.sub.s]. The decrease of Eckert number causes the increase of entropy generation number. Considering specified conditions for the fluid, when the Eckert number decreases, the temperature difference of the plate surface and fluid increases. This causes heat transfer enhancement and therefore increase of fluid particles motion and energy on the plate which means that the molecular randomness or in other words the entropy of the fluid passed over the plate has increased. On the other hand, the description of Fig. 9 clarifies that the increase of Eckert number causes the increase of temperature in boundary layer. But according to Fig. 14, this temperature increase, due to increase of Eckert number, shows its influence in a very small distance from sheet surface directly as the entropy generation of the fluid.

It can be seen from Fig. 14 that at [eta] = 0 when the Eckert number increases from 0.5 to 1.0, the entropy generation number [N.sub.s] decreases from 1256.5 to 1223.7. This means that when the Eckert number increases 100% (becomes 2 times larger), then the entropy generation number [N.sub.s] decreases 2.6%.

Fig. 15 shows the influence of magnetic parameter on entropy generation number. Entropy generation number is higher for higher magnetic parameter. In fact, the motion of fluid molecules increases in presence of magnetic force. Consequently the presence of magnetic field in the fluid causes the entropy generation. Furthermore, entropy generation number has the highest value near the surface, where the temperature and velocity have maximum values in forced convection case. It means that the surface acts as the strong source of irreversibility and randomness generation. Also as it can be seen, when the magnetic parameter increases, the effect of this parameter on entropy generation increase of porous medium fluid decreases and becomes almost negligible.

It can be seen from Fig. 15 that at [eta] = 0 when the magnetic parameter increases from 0.2 to 0.4, then the entropy generation number [N.sub.s] increases from 1425.6 to 1530.6 which means that 100% increase in magnetic parameter is equivalent to 7.4% increase in [N.sub.s].

The influence of dimensionless Hartman number (Ha) on entropy generation number is shown in Fig. 16. Considering the specified properties of fluid, the increase of Hartman number means the increase of magnetic field on the plate and porous medium, for which this increase of the resultant force from magnetic field causes the increase of fluid temperature (see Fig. 10) particularly in low Pr numbers and therefore the increase of the fluid entropy and randomness.

It can be seen in Fig. 16 that at [eta] = 0 the increase of the Hartman number from 20 to 40 causes the increase of the entropy generation number [N.sub.s] from 1622.7 to 2822.7. This means that by 100% increase of the Hartman number, [N.sub.s] increase 74%.

Figs. 17 and 18 show the influences of dimensionless group parameter Br[[OMEGA].sup.-1] and Reynolds number on entropy generation number respectively. The increase of dimensionless group parameter and Reynolds number causes the increase of entropy generation number. It can be said that by the increase of dimensionless group parameter and Reynolds number, the fluid velocity increases which causes the fluid particles randomness level to increase. It can be seen in Figs. 16, 17 and 18 that the entropy generation number is maximized near the plate surface. In these cases the surface acts as the strong source of irreversibility and randomness generation.

It is seen in Fig. 17 that at [eta] = 0 the increase of the dimensionless group parameter Br[[OMEGA].sup.-1] from 0.4 to 0.8 causes the increase of the entropy generation number [N.sub.s] from 529.3 to 1058.3, which means that when Br[[OMEGA].sup.-1] increases 100% (becomes 2 times larger), then the entropy generation number [N.sub.s] increases 100%. Also as it can be seen from Fig. 8, at [eta] = 0 when the Reynolds number increases from 200 to 400, then the entropy generation number Ns increases from 590.8 to 1080.6. This means that 100% increase in the Reynolds number is equivalent to 83% increase in [N.sub.s].

Fig. 19 presents the effect of effective extinction coefficient of porous medium on dimensionless entropy generation profile. It can be seen that the entropy generation increases on the plate with the increase of effective extinction coefficient. This is because when [a.sub.e] increases, the amount of heat absorption by the fluid in the porous medium increases (see Fig. 13) which strengthens the fluid particle motions in porous medium and therefore the fluid randomness. However it can be said that the effective extinction coefficient has small effect on the entropy generation number.

It is seen from Fig. 19 that at [eta] = 0 the increase of the effective extinction coefficient [a.sub.e] from 1.0 to 2.0 causes the increase of the entropy generation number [N.sub.s] from 3791 to 3822.4. This means that 100% increase in [a.sub.e] increases [N.sub.s] approximately 0.8%.

[FIGURE 20 OMITTED]

Fig. 20 shows the dimensionless entropy generation profile for various values of porosity ([epsilon]). It can be seen that the entropy generation on the plate increases with the increase of porosity. It is because when porosity increases, the possibility of free motion of the fluid particles inside porous medium increases. On the other hand, as it was mentioned in Fig. 8 description, the fluid temperature increases and this is another reason for the increase of fluid particles motions and consequently the randomness and irreversibility of the fluid.

It can be seen from Fig. 20 that at [eta] = 0 when the porosity [epsilon] increases from 0.5 to 1.0, the entropy generation number [N.sub.s] increases from 4358.4 to 5121.6, which means 100% increase in porosity [epsilon] causes 17.5% increase in [N.sub.s].

Here in investigating the effects of various parameters on the entropy generation number [N.sub.s], the values of [N.sub.s] on the (plate) surface i.e., at [eta] = 0 have been considered because [N.sub.s] has the highest values on the surface.

By evaluating the effects of various parameters including Eckert number, magnetic parameter, Hartman number, dimensionless group parameter Br[[OMEGA].sup.-1], Reynolds number, effective extinction coefficient [a.sub.e] and porosity [epsilon] on the entropy generation number [N.sub.s], it is seen that the dimensionless group parameter Br[[OMEGA].sup.-1] has the largest effect on [N.sub.s]. After the dimensionless group parameter Br[[OMEGA].sup.-1], the Reynolds number and then the Hartman number have the largest effects on [N.sub.s]. Next parameters in aspect of having effect on [N.sub.s] are the porosity [epsilon], the magnetic parameter and the Eckert number. It is seen that the effective extinction coefficient [a.sub.e] has the smallest effect on [N.sub.s].

6. Conclusions

The MHD mixed convection flow over a nonlinear stretching inclined transparent plate embedded in a porous medium due to solar radiation has been investigated analytically and numerically. The steady two-dimensional governing equations are obtained considering Boussinesq approximation and uniform porosity in presence of the effects of viscous dissipation and variable magnetic field. These equations are transformed by the similarity method to two coupled nonlinear ordinary differential equations (ODEs). These two nonlinear ODEs are converted into five first order ODEs and then the system of first-order equations is solved numerically using an implicit finite-difference scheme known as the Keller-Box method. The nonlinear discretized system of equations is linearized using the Newton's method. The system of obtained equations is a block-tri-diagonal which is solved using the block-tri-diagonal-elimination technique.

The effects of various parameters such as magnetic parameter, porosity, effective extinction coefficient of porous medium, solar radiation flux, plate inclination angle, diameter of porous medium solid particles and dimensionless Eckert, Richardson, Prandtl, Hartman, Brinkman, Reynolds and entropy generation numbers have been studied on the dimensionless temperature and velocity profiles. The results obtained are as follows:

1. The dark colour of solid particles of porous medium can increase the effective absorption coefficient and finally the temperature in the thermal boundary layer.

2. The entropy generation number is higher near the surface which means that the surface acts as a strong source of irreversibility.

3. The higher the Eckert number, the lower the entropy generation number. The increase of Eckert number causes the increase of temperature in boundary layer, but this temperature increase shows its influence directly as the entropy generation of the fluid in a very small distance from the sheet surface.

4. The dimensionless group parameter Br[[OMEGA].sup.-1], Reynolds number and Hartman number have very large effects on the entropy generation number while the magnetic parameter have small effect on the entropy generation number.

5. The effective extinction coefficient has very small effect on the entropy generation number.

Nomenclature

a--absorption or extinction coefficient of fluid, [m.sup.-1]; B--magnetic field, tesla; [B.sub.0]--magnetic rate, positive constant; Br--Brinkman number (= [mu][u.sub.w][(x).sup.2]/[DELTA]Tk); C([epsilon])--porous medium inertia coefficient, [m.sup.-1]; [C.sub.f]--Skin friction coefficient (= -[(2(m + 1)/[Re.sub.x]).sup.0.5][f.sub.[eta][eta]](0)); [C.sub.p]-specific heat at constant pressure, J/(kgK); [d.sub.p]--particle diameter, m; [D.sub.p]--geometric parameter of porous medium; Ec-Eckert number (= [u.sub.w][(x).sup.2]/[C.sub.p]([T.sub.w] - [T.sub.[infinity]])); f--dimensionless velocity variable (= [PSI](x,y)[([Re.sub.x]).sup.0.5]/[u.sub.w](x)); g--gravitational acceleration, m/[s.sup.2]; [Gr.sub.x]-Grashof number (= g([T.sub.w] - [T.sub.[infinity]])[beta]/[v.sup.2]); Ha-Hartman number (= [B.sub.0]x[([sigma]/[mu]).sup.0.5]); K([epsilon])-porous medium permeability, [m.sup.2]; k-thermal conductivity, W/(mK); m-index of power law velocity, positive constant; M-magnetic parameter (= 2[sigma][B.sub.0.sup.2]/[[rho].sub.[infinity]]b(m + 1)); Nu--Nusselt number (= -[(0.5(m + 1)[Re.sub.x]).sup.0.5][[theta].sub.[eta]](0)); [N.sub.s]--Entropy generation number; Pr-Prandtl number (= [mu][C.sub.p]/k); [q.sub.rad]-radiation flux distribution, W/[m.sup.2]; R-Radiation parameter; [Re.sub.x]-local Reynolds number (= [[rho]u.sub.w](x)x/[mu]); T--temperature, K; u-velocity in x--direction, m/s; v--velocity in y--direction, m/s; x-horizontal coordinate, m; x-vertical coordinate, m; [gamma]--plate inclination angle, degrees; [alpha]--thermal diffusivity, [m.sup.2]/s;[theta]--dimensionless temperature variable (= (T-[T.sub.[infinity]])/([T.sub.w] - [T.sub.[infinity]));] [mu]-dynamic viscosity, kg/(ms); v-kinematic viscosity, [m.sup.2]/s; [rho]-density, kg/[m.sup.3]; [sigma]-electrical conductivity, mho/s; [OMEGA]--dimensionless temperature difference (= [DELTA]T/[T.sub.[infinity]] = (T - [T.sub.w])/[T.sub.[infinity]]); [PSI]--stream function, [m.sup.2]/s; [beta] similarity variable (= (y/x)[(0.5[Re.sub.x](m + 1)).sup.0.5]); [beta]--thermal expansion coefficient, 1/K.

Subscripts:

e--effective; ef--effective for porous medium; f--friction; p--constant pressure, particle; r--radiation heat flux; rad--radiation; s--entropy; x--local x-coordinate; w--plate or sheet; [infinity]--far away from the plate.

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M. Dehsara, School of Mechanical Engineering, Amirkabir University of Technology (Tehran Polytechnic), 424 Hafez Avenue, P.O. Box, 15875-4413 Tehran, Iran, E-mail: [email protected]

M. Habibi Matin, School of Mechanical Engineering, Amirkabir University of Technology (Tehran Polytechnic), 424 Hafez Avenue, P.O. Box, 15875-4413 Tehran, Iran, E-mail: [email protected]

N. Dalir, School of Mechanical Engineering, Amirkabir University of Technology (Tehran Polytechnic), 424 Hafez Avenue, P.O. Box, 15875-4413 Tehran, Iran, E-mail: [email protected]

http://dx.doi.org/10.5755/j01.mech.18.5.2694

Received March 18, 2011

Accepted September 21, 2012

Table
Skin friction and wall temperature gradient for different
values of the physical parameters Ec = 0.10, Mn = 0.10, m
= 1.0, Pr = 1.0, x = 0.10, Re = 500

[a.sub.e] [gamma] [Nu.sub.r] [D.sub.p] [epsilon]
 = 0.3

 [C.sub.f]

0.10 0.0 10 10 -0.22794
 15 -0.26549
 20 -0.28899
0.10 0.0 50 10 -0.22981
 15 -0.26774
 20 -0.29153

[D.sub.p] [Nu.sub.r] [gamma] [a.sub.e] [C.sub.f]

5.0 10 0.0 0.0 -0.15054
 0.5 -0.15216
 1 -0.1536
5.0 10 60 0.0 -0.02462
 0.5 -0.02578
 1 -0.02681

[a.sub.e] [epsilon] [epsilon]
 = 0.3 = 0.4

 Nu [C.sub.f] Nu

0.10 17.99588 -0.29151 17.74096
 17.91314 -0.31996 17.43015
 17.76332 -0.33711 17.17524
0.10 17.71413 -0.2941 17.45251
 17.6314 -0.323 17.13052
 17.47487 -0.34045 16.86442

[D.sub.p] Nu [C.sub.f] Nu

5.0 17.72307 -0.23029 18.06072
 17.36978 -0.23259 17.72084
 17.04331 -0.23462 17.40332
5.0 16.47982 -0.08451 17.60233
 16.10193 -0.08617 17.24903
 15.75086 -0.08763 16.92033