标题： CMB温度红移关系对衰减暗能量密度模型的限制 显示英文标题

标题： Limits on decaying dark energy density models from the CMB temperature-redshift relation

摘要： 暗能量的本质仍然是一个谜，已经提出了几种模型来解释它。 在这里，我们考虑了一个现象学模型，即暗能量衰变为光子和粒子，这是由Lima（J. Lima, Phys. Rev. D 54, 2571 (1996))提出的。 他研究了衰变暗能量模型的热力学方面，特别是在连续光子产生和/或破坏的情况下。 根据他的方法，我们推导出了宇宙微波背景辐射（CMB）的温度红移关系，该关系依赖于有效状态方程$w_{eff}$和“绝热指数”$\gamma$。 将我们的关系与通过Sunyaev-Zel'dovich观测获得的CMB温度随红移的变化数据以及通过类星体吸收线光谱在更高红移处获得的数据进行比较，我们发现$w_{eff}=-0.97 \pm 0.034$，采用绝热指数$\gamma=4/3$，这与当前估计值一致，并且仍然与$w_{eff}=-1$相容，这意味着暗能量含量随时间保持不变。 显示英文摘要

摘要： The nature of the dark energy is still a mystery and several models have been proposed to explain it. Here we consider a phenomenological model for dark energy decay into photons and particles as proposed by Lima (J. Lima, Phys. Rev. D 54, 2571 (1996)). He studied the thermodynamic aspects of decaying dark energy models in particular in the case of a continuous photon creation and/or disruption. Following his approach, we derive a temperature redshift relation for the CMB which depends on the effective equation of state $w_{eff}$ and on the "adiabatic index" $\gamma$. Comparing our relation with the data on the CMB temperature as a function of the redshift obtained from Sunyaev-Zel'dovich observations and at higher redshift from quasar absorption line spectra, we find $w_{eff}=-0.97 \pm 0.034$, adopting for the adiabatic index $\gamma=4/3$, in good agreement with current estimates and still compatible with $w_{eff}=-1$, implying that the dark energy content being constant in time.