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From IFPA wiki
  1. The 2nd law also applies to multiple black holes. In this case the statement is that the total entropy - ie the sum of the areas of all black holes - must increase. Argue that if two uncharged, non-rotating black holes collide violently to make one bigger black hole, then at most 29% of their initial rest energy can be radiated in gravitational waves. From T. Hartman's page http://www.hartmanhep.net/topics2015/2-bhthermo.pdf
  2. Consider a massless scalar field; i.e., a scalar field [math]\phi(t,x)[/math] with a potential-energy density [math] V(\phi) = 0[/math]. Suppose that this scalar field is initially rolling, so that [math]\dot\phi\neq 0[/math], and that the kinetic-energy density associated with this rolling dominates the energy density of the Universe. Show that this implies that [math]\rho\propto a^{-6}[/math], where [math]a[/math] is the scale factor, in two ways: (1) by recalling how the energy density of matter with an equation of state P = wρ scales with a; and (2) by solving the equation of motion [math]\phi[/math] in an expanding Universe.
  3. Study the evolution of a scalar field (under the slow-roll assumption) if the inflationary potential is [math]\lambda \Phi^4[/math].
  4. Show that [math] d(det(M))=det(M) M^{ik} dM_{ik} [/math], and that [math] T^{\mu\nu}=-\frac{2}{\sqrt{-g}}\frac{\partial(\sqrt{-g}{\mathcal L})}{\partial g_{\mu\nu}}[/math] leads to the usual energy-momentum tensor in the case of a scalar field with a generic potential [math]V(\Phi)[/math] and for a Minkowski space-time [math] g_{\mu\nu}=diag(1,-1,-1,-1)[/math]. Work out [math]T^{00}[/math] and [math] T^{ii}[/math] in the case of a FLRW metric [math] g_{\mu\nu}=diag(1,-a^2(t),-a^2(t),-a^2(t))[/math]



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