We look at, starting with Shankar’s treatment of the partition function, inserting in the data of the modified Heisenberg uncertainty principle as to give a role to the inflaton in the formation of a partition of the...We look at, starting with Shankar’s treatment of the partition function, inserting in the data of the modified Heisenberg uncertainty principle as to give a role to the inflaton in the formation of a partition of the universe. The end result will be, even with the existence of a multiverse, i.e. simultaneous universes, uniform physical laws throughout the multiple universes.展开更多
We use the work of de Vega, Sanchez, and Comes (1997), to approximate the “particle density” of a “graviton gas”. This “particle density” derivation is compared with Dolgov’s (1997) expression of the Vacuum ene...We use the work of de Vega, Sanchez, and Comes (1997), to approximate the “particle density” of a “graviton gas”. This “particle density” derivation is compared with Dolgov’s (1997) expression of the Vacuum energy in terms of a phase transition. The idea is to have a quartic potential, and then to utilize the Bogomol’nyi inequality to refine what the phase transition states. We utilize Ng, Infinite quantum information procedures to link our work with initial entropy and other issues and close with a variation in the HUP: at the start of the expansion of the universe.展开更多
文摘We look at, starting with Shankar’s treatment of the partition function, inserting in the data of the modified Heisenberg uncertainty principle as to give a role to the inflaton in the formation of a partition of the universe. The end result will be, even with the existence of a multiverse, i.e. simultaneous universes, uniform physical laws throughout the multiple universes.
文摘We use the work of de Vega, Sanchez, and Comes (1997), to approximate the “particle density” of a “graviton gas”. This “particle density” derivation is compared with Dolgov’s (1997) expression of the Vacuum energy in terms of a phase transition. The idea is to have a quartic potential, and then to utilize the Bogomol’nyi inequality to refine what the phase transition states. We utilize Ng, Infinite quantum information procedures to link our work with initial entropy and other issues and close with a variation in the HUP: at the start of the expansion of the universe.
