4 W = 1 2 ( ρ$_{sc}$ − P$_{sc}$ ) , (27) Ψ$_{a}$ = − 1 2 ( ρ$_{sc}$ + P$_{sc}$ ) H ˜ rdt + 1 2 ( ρ$_{sc}$ + P$_{sc}$ ) adr, (28) δQ = − dE = − A Ψ = A ( ρ$_{sc}$ + P$_{sc}$ ) H ˜ r$_{A}$dt, (29) dS sc A = 8 π 2 1 H $_{3}$( ρ$_{sc}$ + P$_{sc}$ ) dt = 1 8 πG [ 2 π ˙ A S + A $^{2}$H2 2 ˙ S 2 − 1 2 ˙ S A 2 a 2 − 1 − S 2 a 2 HA 2 S ] dt (30) ds 2 = − dt 2 + a 2 ( dr 2 1 − r 2 + r $^{2}$d Ω 2 ) = h$_{ab}$dx $^{a}$dxb + ˜ r $^{2}$d Ω 2 $_{2}$, (21) h $^{ab}$∂$_{a}$ ˜ r∂$_{b}$ ˜ r ≡ f, (22) S sc A = S sc Aa + A$_{eff}$ 4 G + 1 4 G ∫ A$_{eff}$d ln S + 1 8 πG ∫ A 2 $_{eff}$H 2 2 d S − 1 16 πG ∫ A 2 eff a $^{2}$S$_{2}$d S − 1 8 πG (1 − S $^{2}$) S a 2 HA 2 $_{eff}$dt, (31) dE = A Ψ + WdV, (24) W = − 1 2 T $^{ab}$h$_{ab}$ , (25) Ψ$_{a}$ = T b $_{a}$∂$_{b}$ ˜ r + W∂$_{a}$ ˜ r, (26) S$_{bh}$ = S$_{BH}$ + ∞ ∑ n =0 C$_{n}$A − n H , (32) Considering our interested metric (21), we can get the obvious expressions for W, Ψ$_{a}$ [16]: In those equations, we have considered the quantal cor- rection. The energy thrill through the apparent horizon at the interval time dt is given as [16] with the total energy E$_{m}$ = ρV and the work density W$_{m}$ = ( ρ − p ) / 2, the authors of [16] showed that the entropy-area relationship of apparent horizon would be corrected by the modified Friedmann equation in loop quantum cosmology. In this subsection, we will discuss the modified entropy-area relation which is caused by the corrected Friedmann equation (6). Just as [16] stated, the temperature of apparent horizon is just determined by the spacetime metric, so it is convenient to assume the temperature of apparent horizon is T$_{A}$ = 1 / (2 π ˜ r$_{A}$ ), with the radius of the apparent horizon ˜ r$_{A}$ . Noticed that the LQC is just correcting the Hamiltonian, not the La- grangian. And the spacetime metric is described by the Lagrangian, so it is natural to believe that the definition of temperature of the apparent horizon in LQC is as same as in the classical one. Our interested spacetime is the closed Friedmann- Robertson-Walker (FRW) universe which is described by the metric with the area of the apparent horizon A = 4 π ˜ r 2 $_{A}$. If the modified entropy of the apparent horizon is denoted as S sc A , considering δQ = T dS sc A and Eq.(29), one can obtain with h$_{ab}$ = diag( − 1 , a $^{2}$/ (1 − r $^{2}$)) , ˜ r = a ( t ) r , and k denotes the spatial curvature. If we define the Missner-Sharpe mass [24, 31, 32] in which we have used the temperature of the apparent horizon T$_{A}$ = 1 / (2 π ˜ r$_{A}$ ) with the radius of the apparent horizon ˜ r$_{A}$ = 1 / √ H 2 + 1 /a 2 and Eq.(8). Expanding the above equation and integrating it, Eq.(30) can be written as the apparent horizon is determined from f = 0. So, we can get the radius of the apparent horizon ˜ r$_{A}$ = 1 √ H 2 + 1 /a $_{2}$. (23) with the Hubble parameter H described by Eq.(6). In this paper, we consider the dark energy fluid is a perfect fluid satisfies T$_{µν}$ = ( ρ$_{sc}$ + P$_{sc}$ ) U$_{µ}$U$_{ν}$ + P$_{sc}$g$_{µν}$ , where ρ$_{sc}$ and P$_{sc}$ are the modified energy density and pressure in the semiclassical LQC, respectively. And the energy conservation law which is described by Eq.(10) still satisfied. The Einstein equation is written as in which A$_{eff}$ = A/ S denotes the effective area of the ap- parent horizon in the semiclassical LQC. in which S sc Aa is a constant and the value depends on the specific physics. In a short conclusion, considering the Einstein equa- tion (24) and assuming that the apparent horizon has Hawking temperature, we get the expression for the mod- ified entropy-area relation in the semiclassical LQC. The semiclassical theory not only modify the entropy of ap- parent horizon, but also the area of it. And it is worth to notice that this modified entropy-area relation is not as same as the correction of black hole in loop quantum gravity [33] where A = 4 π ˜ r 2 A is the area of the apparent horizon and V = 4 π 3 ˜ r 3 A is the volume of 3-dimensional sphere. E = M is the Misser-Sharp energy which is given by Eq.(22). W is the work density and Ψ is the energy-supply vector, are defined as where T$_{ab}$ is the projection of the (3 + 1)-dimensional energy-momentum tensor T$_{µν}$ of dark energy fluid in the FRW universe in the normal direction of 2-sphere[16]. with some constants C$_{n}$ . And it is different from the modified entropy-area relationship, which has the same