LOG#145. Basic QFT in curved ST(V): the Hawking effect.

Idea: Black Holes (BH) are “not” truly black. BH emit thermal radiation at the Hawking temperature and it is proportional to the surface gravity () of the BH. Mathematically, we have as the Bekenstein-Hawking temperature. In the case of a … Continue reading

LOG#144. Basic QFT in curved ST(IV): the Unruh effect.

What is the Unruh effect? Description: any accelerated observer in the traditional Minkovski state OBSERVE a thermal spectrum of particles. When we refer to the accelerated observer, usually it is called the Rindler observer in the literature as well. In … Continue reading

LOG#143. Basic QFT in curved ST(III).

We are now ready to go back to curved spacetime in the IN/OUT formalism! We have Indeed, where when we get particles from gravity! The particle density reads For instance, in a Friedmann-Robertson-Walker metric (FRW universe) we obtain where is … Continue reading

LOG#050. Why riemannium?

TABLE OF CONTENTS DEDICATORY 1. THE RIEMANN ZETA FUNCTION ζ(s) 2. THE RIEMANN HYPOTHESIS 3. THE HILBERT-POLYA CONJECTURE 4. RANDOM MATRIX THEORY 5. QUANTUM CHAOS AND RIEMANN DYNAMICS 6. THE SPECTRUM OF RIEMANNIUM 7. ζ(s) AND RENORMALIZATION 8. ζ(s) AND … Continue reading