6 ρ$_{sc}$ ( a ) = ρ$_{0}$ [ T$_{sc}$ ( a ) T$_{0}$ ω$_{0}$ + 1 ω$_{sc}$ ( a ) + 1 ] $^{ω}$sc ( a )+1 $^{ω}$sc ( a ) × exp [ 3 ω$_{sc}$ ( a ) ∫ 1 a daω ′ $_{sc}$( a ) ln a ] , for ω$_{sc}$ ( a ) = 0; ρ$_{sc}$ ( a ) = ρ$_{0}$ [ T$_{sc}$ ( a ) T$_{0}$ ω$_{0}$ + 1 ω$_{sc}$ ( a ) + 1 ] ( 1 a ) 3 , for ω$_{sc}$ ( a ) = 0 . (39) µ$_{sc}$ ( a ) = 1 n [(1 + ω$_{sc}$ ( a )) ρ$_{sc}$ ( a ) − T$_{sc}$ ( a ) s$_{sc}$ ( a )] . (40) µ$_{sc}$ ( a ) = µ$_{0}$ [ ω$_{sc}$ ( a ) + 1 ω$_{0}$ + 1 ] [ 1 a 3 ω$_{sc}$ ( a ) ] × exp [ − 3 ∫ 1 a daω ′ $_{sc}$( a ) ln a ] , (41) µ$_{sc}$ ( a ) = µ$_{0}$ T$_{sc}$ ( a ) T$_{0}$ . (42) S$_{sc}$ ( a ) = s$_{0}$V ( a ) [ T$_{sc}$ ( a ) T$_{0}$ ω$_{0}$ + 1 ω$_{sc}$ ( a ) + 1 ] 1 $^{ω}$sc ( a ) × exp [ 3 ω$_{sc}$ ( a ) ∫ 1 a daω ′ $_{sc}$( a ) ln a ] , (43) IV. CONCLUSION AND DISCUSSION generalized Stefan-Boltzmann law for temperature, chemical potential and entropy. We find that those variables are corrected due to the semiclassical quantum effect, and those corrections are connected with the modified EoS parameters. Our method is following [20], in which the temperature is regular for the vacuum when they discuss the thermodynamics properties in the classical regions but the temperature will be divergent at a = 0. But due to the modification of semiclassical quantum effect, a = 0 doesn’t lie in the regions we inter- ested, so the expression for temperature always holds for a varying classical EoS ω$_{cl}$ . The expressions for chemical potential and entropy are obtain in this subsection. It is worth to notice that the above equations are still valid for ω$_{sc}$ ( a ) = − 1, for T$_{sc}$ ( a ) = 0 in this moment. Now we turn to consider the chemical potential and entropy. Consider the Euler’s relation of T$_{sc}$ ( a ) s$_{sc}$ ( a ) = [1 + ω$_{sc}$ ( a )] ρ$_{sc}$ ( a ) − µ$_{sc}$ ( a ) n , with the chemical potential µ$_{sc}$ ( a ), the chemical potential can be given as [20] In this paper, we have discussed the thermodynamics properties of the dark energy in the semiclassical LQC scenario. The common feature of the all models of dark energy is the EoS parameters ω of dark energy fluid is included by the field evolution. So, at the first, we con- sider the correction of EoS parameters in the regions we interested. We find that the corrected EoS parameters depends on the changing rate of inverse volume factor D$_{l}$ and classical EoS parameters ω$_{cl}$ ( a ). Using the Gibbs law (36) and the modified temperature (38), it is easy to get the modified chemical potential with chemical potential at present µ$_{0}$ = 1 $_{n$_{0}$}$[ ρ$_{0}$ ( ω$_{0}$ + 1) − T$_{0}$s$_{0}$ ]. As before, the above equation is well-defined when ω$_{0}$ = − 1, for T$_{0}$ = 0. But the sign of µ$_{sc}$ ( a ) is indepen- dent on ω$_{sc}$ ( a ), for the sign of µ$_{0}$ can be general. And the chemical potential can be wrote as a function of T$_{sc}$ ( a ), We discussed the area-entropy relation of the appar- ent horizon of universe which is full of dark energy fluid. We found that the effective LQC not only modify the en- tropy of apparent horizon, but also the area of it. And the modified area-entropy relation is different from the one considered by [16], in which the authors considered the holonomy correction. And then, we discussed the ther- modynamical properties of dark energy fluid in the inner side of apparent horizon. The expressions for tempera- ture, chemical potential and entropy are obtained. We find that, if the classical EoS parameter is a function of the scale factor, the thermodynamical variables are func- tions of the modified EoS parameters and well-defined when ω ( a$_{0}$ ) = − 1. The sign of temperature is dependent on the modified EoS ω$_{sc}$ , when ω$_{sc}$ > − 1, T$_{sc}$ > 0, T$_{sc}$ < 0 when ω$_{sc}$ < − 1, and T$_{sc}$ = 0 if ω$_{sc}$ = − 1, but the sign of the modified temperature is independent on the sign of potential, which is determined by the sign of µ$_{0}$ . This is as same as the discussion in the classical region [20]. T$_{sc}$ ( a ) = S$_{sc}$ ( a ) = 0 when ω$_{sc}$ ( a ) = − 1, this is like the be- havior of massless degenerate Fermi gas [37, 38]. Just as we discussed above, when ω$_{sc}$ < − 1, the temperature is negative. But this negative temperature is independent on the sign of potential, for the sign of potential is just dependent on µ$_{0}$ . The negative temperature can only be explain in the quantum framework. The quantum field theory for the field with EoS parameters ω$_{cl}$ < − 1 is still an open question. In the semiclassical regions, the EoS parameters should be modified by the quantum geometry effect, so the negative temperature in the semiclassical regions partial is cased by the quantum geometry effect. In this paper, we just consider the thermodynamics properties of dark energy fluid, it is easy to verify that It is easy to get the entropy of the dark energy fluid by considering the Eq.(40). Remembering S ( a ) = s ( a ) V ( a ) = s ( a ) a $^{3}$, and using Eqs.(35),(39) and (42), we can get the expression for entropy. in which we have considered the present scale factor a$_{0}$ = 1. When ω$_{sc}$ ( a ) = 0, combining Eq.(39) and Eq.(42), we find it is a trivial result. Note that, above equation is regular at ω$_{sc}$ ( a ) = − 1, because if ω$_{sc}$ ( a ) = − 1, T$_{sc}$ = 0. And if ω$_{0}$ = − 1, then T$_{0}$ = 0, so the above equation is still well-defined. It is easy to get s$_{0}$V$_{0}$ = s$_{sc}$ ( a ) V ( a ). In a short conclusion, in this subsection, we has dis- cussed the thermodynamics properties of dark energy in the inside of apparent horizon, and get the expressions