The development of gravitational instabilities - RESCEU

More documents

Recommendations

Info

A self-gravitating expanding dust fluid 6
A self-gravitating expanding dust fluid ‣ Data show that large-scale structure has formed from small density inhomogeneities since time of matter dominated universe with a dominant cold dark matter component The Vlasov equation (collisionless Boltzmann equation) - f(x,p) is the phase space density distribution - are fully nonlinear. The rules of the game: single flow equations Peebles 1980; Fry 1984 FB, Colombi, Gaztañaga, Scoccimarro, Phys. Rep. 2002 df dt = ∂ f(x, p,t)+ p ∂t ma 2 ∂ ∂x ∂ f(x, p,t) − m ∂x Φ(x) ∂ ∂p (∫ ∆Φ(x) = 4πGm a f(x, p,t)=0 ) f(x, p,t)d 3 p − ¯n This is what N-body codes aim at simulating... + expansion with respect to initial density fields δ(x,t)=δ (1) (x,t)+δ (2) (x,t)+. . . 7 GR corrections effects: Yoo et al., PRD, 2009 B, Bonvin, Vernizzi, PRD, 2010 Francis Bernardeau IPhT Saclay
Page 1: Francis Bernardeau IPhT Saclay, Fra
Page 4 and 5: Which observables ? 〈δ x (k 1 )
Page 8 and 9: ‣Motion equations in Fourier spac
Page 10 and 11: ‣ A lot is known at tree order Th
Page 12 and 13: A field theory reformulation Scocci
Page 14 and 15: Not a standard quantum field theory
Page 16: The closure theory Valageas P., A&A
Page 19 and 20: One key ingredient : the propagator
Page 21 and 22: ‣ RPT (Scoccimarro and Crocce) co
Page 23 and 24: Insights into higher order propagat
Page 25 and 26: ‣ This suggests another scheme :
Page 27 and 28: Comparison with numerical simulatio
Page 29 and 30: • Does it speed up the convergenc
Page 31 and 32: Using large-scale structure to test
Page 33 and 34: In presence of a dilaton field Brax
Page 35 and 36: Evolution of structure: from GR to
Page 37 and 38: Bispectra (equilateral configuratio

The development of gravitational instabilities - RESCEU

Create successful ePaper yourself

Delete template?

Save as template?