发表机构
National Research Institute of Astronomy and Geophysics（国家天文与地球物理研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究探讨瑞士奶酪膜世界宇宙的非平衡热力学，提出内部熵产生修正，应用于物质反弹解，证明膨胀阶段满足广义第二定律并渐近进入暗能量主导阶段。
AI 中文摘要
我们研究了瑞士奶酪（SC）膜世界宇宙的非平衡热力学。通过采用Hayward统一第一定律和表观视界处的Clausius关系，我们首先表明，对有效SC膜世界流体的标准平衡处理，连同通常的Hawking温度，再现了Bekenstein-Hawking面积定律，而无需任何膜世界对熵的修正。这表明，膜二次能量密度修正本身不能在平衡框架内产生修正的熵面积关系。因此，我们构建了一个非平衡热力学描述，其中偏离Bekenstein-Hawking熵伴随着内部熵产生项。对于一般的视界熵泛函，我们推导了相应的熵产生率，然后专门研究了对数形式和逆面积量子修正熵。由此产生的不可逆贡献用哈勃参数及其导数表示。我们将该形式应用于SC膜世界中一个非奇异的物质反弹解。在膨胀阶段，总熵产生保持为正，满足广义第二定律（GSLT）。此外，总熵二阶导数的晚期行为变为负，表明熵增长减速并渐近趋近热力学平衡。远离反弹时，状态方程参数$w \approx -1$，表明暗能量主导的时期。对$w = -1$的显著偏离仅限于反弹附近，其中高能膜世界修正驱动非奇异转变。因此，该模型自然地从高能反弹过渡到晚期膨胀中的渐近暗能量阶段。
英文摘要
We investigate the non-equilibrium thermodynamics of a Swiss-cheese (SC) braneworld universe. By employing Hayward's unified first law and the Clausius relation at the apparent horizon, we first show that the standard equilibrium treatment of the effective SC braneworld fluid, together with the usual Hawking temperature, reproduces the Bekenstein-Hawking area law without any braneworld correction to the entropy. This demonstrates that the brane quadratic energy density corrections cannot, by themselves, generate a modified entropy area relation within the equilibrium framework. We therefore formulate a non-equilibrium thermodynamic description in which deviations from the Bekenstein-Hawking entropy are accompanied by an internal entropy production term. For a general horizon entropy functional, we derive the corresponding entropy production rate and then specialize to a logarithmic and inverse area quantum-corrected entropy. The resulting irreversible contribution is expressed in terms of the Hubble parameter and its derivative. We apply the formalism to a nonsingular matter-bounce solution in the SC braneworld. During the expanding phase, the total entropy production remains positive satisfying the GSLT. Moreover, the late-time behavior of the second derivative of the total entropy becomes negative, indicating a decelerating entropy growth and an asymptotic approach toward thermodynamic equilibrium. Far from the bounce, the equation of state parameter $w \approx -1$, indicating a dark energy-dominated regime. Significant departures from $w = -1$ are confined to the bounce vicinity, where high energy braneworld corrections drive the nonsingular transition. Thus, the model naturally transitions from a high energy bounce into an asymptotic dark energy phase during late-time expansion.
