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Numerical simulations of gravitational singularities

Numerical simulations of gravitational singularities. Gravitational collapse Singularity theorems BKL conjecture Gowdy spacetimes General spacetimes. Star in equilibrium between gravity and pressure. Gravity can win and the star can collapse. Singularity theorems.

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Numerical simulations of gravitational singularities

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  1. Numerical simulations of gravitational singularities

  2. Gravitational collapse • Singularity theorems • BKL conjecture • Gowdy spacetimes • General spacetimes

  3. Star in equilibrium between gravity and pressure. Gravity can win and the star can collapse

  4. Singularity theorems Once a trapped surface forms (given energy and causality conditions) Some observer or light ray ends in a Finite amount of time Very general circumstances for Singularity formation Very little information about The nature of singularities

  5. Approach to the singularity As the singularity is approached, some terms in the equations are blowing up Other terms might be negligible in comparison Therefore the approach to the singularity might be simple

  6. BKL Conjecture As the singularity is approached time derivatives become more important than spatial derivatives. At each spatial point the dynamics approaches that of a homogeneous solution. Is the BKL conjecture correct? Perform numerical simulations and see

  7. Gowdy spacetimes ds2 = e(l+t)/2 (- e-2t dt2 + dx2) + e-t [eP (dy+Qdz)2 +e-P dz2] P, Q and l depend only on t and x The singularity is approached as t goes to infinity

  8. Einstein field equations Ptt – e2P Qt2 – e-2t Pxx + e2(P-t)Qx2=0 Qtt + 2 Pt Qt – e-2t (Qxx + 2 Px Qx) = 0 (subscript means coordinate derivative) Note that spatial derivatives are multiplied by decaying exponentials

  9. As t goes to infinity P = P0(x)+tv0(x) Q = Q0(x) But there are spikes

  10. P

  11. Q

  12. General case Variables are scale invariant commutators of tetrad e0 = N-1 dt ea = eai di [e0,ea]= ua e0 – (Hdab + sab) eb [ea,eb]=(2 a[adb]g + eabd ndg) eg

  13. Scale invariant variables {dt , Eai di} = {e0,ea}/H {Sab,Aa,Nab}={sab,aa,nab}/H

  14. The vacuum Einstein equations become evolution equations and constraint equations for the scale invariant variables.

  15. Results of simulations Spatial derivatives become negligible At each spatial point the dynamics of the scale invariant variables becomes a sequence of “epochs” where the variables are constant, punctuated by short “bounces” where the variables change rapidly

  16. S

  17. N

  18. u

  19. Conclusion BKL conjecture appears to be correct What remains to be done • Matter (2) Small scale structure

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