Sorry, assume I've read standard textbooks and Ellis-Maartens-Mccallum, and explain to me how inflation controls the spatially flat FLRW chart density of low-en

Sorry, assume I've read standard textbooks and Ellis-Maartens-Mccallum, and explain to me how inflation controls the spatially flat FLRW chart density of low-entropy fluctuations in the quasi de Sitter +CC phase (ideally beginning with the "dark era", or even the earlier black hole era if you want to deal in nonequilibrium entropy explicitly, rather than just assuming heat death). (I don't know where you got "14b.y." from; we still have the local group (including Milkdromeda) making new stars that soon from now; it's a cosmological eyeblink). > This is barely anything beyond inflation, it just sets the proper measure/odds among the details to match observations "Barely anything" seems to be doing a lot of heavy lifting there, but perhaps I'm missing something simple. See at the end below. > For BBs, yes the "tiny" ones will be exponentially more likely. Well, yes, statmech. The problem is that if you allow non-"tiny" low entropy states you get them even during the matter-dominated era, so our sky should be sufficiently full of Boltzmann-russell-teapots to show up in studies of high-redshift quasars (and H II). I do not understand the rest of that paragraph. > That's all I was saying. If that was all you were saying, I'd agree. I used the word "diagnostic" in the comment you replied to. But you also write: > Inflation might be so pervasive it makes BBs infinitesimal ??? > ... Susskind ... Are you trying to summarize stochastic eternal inflation? Or is this something out of his recent investigations of Sachdev-Ye-Kitaev? I haven't looked at his DSSYK stuff because AdS results aren't interesting to me. ETA (just for me, i had to put this somewhere to find it later): Brandenberger et al 1992 "The Entropy of the Gravitational Field", https://arxiv.org/abs/gr-qc/9208009v1 https://arxiv.org/abs/gr-qc/9208009v1