前两天在家分别计算了Vaidya黑洞的apparent horizon和event horizon的熵，得到了结果。但是吴老师建议凑一下热点，将Massive Gravity加入到Vaidya中试试，于是今天（10月3日）在arXiv上看到两篇文章，有点意思。
第一篇和我正在算的Vaidya黑洞熵有关。最近Massive gravity很火，可以将它与Vaidya结合起来进行计算。
这篇文章名是 Vaidya Spacetime in Massive Gravity’s Rainbow，其中得到了Vaidya的度规，但我感觉有些繁琐。
于是看到了Holographic Thermalization and Generalized Vaidya-AdS Solutions in Massive Gravity 这篇文章，它给出了清晰的解和度规，计算起来很方便了。
第二篇与我所做的工作无直接关系，不过它是Carlo Rovelli 写的 Black holes have more states than those giving the Bekenstein-Hawking entropy: a simple argument.
摘要如下：
It is often assumed that the maximum number of independent states a black hole may contain is \( N_{BH}=e^{BH} \), where \( S_{BH} = A/4 \) is the Bekenstein-Hawking entropy and \( A \) the horizon area in Planck units. I present a simple and straightforward argument showing that the number of states that can be distinguished by local observers inside the hole must be greater than this number.
这一篇将黑洞熵的地位提高了，黑洞熵的价值将因此被发掘。
