arXiv1996
We study the classical dynamics of a bosonic string in the $D$--dimensional flat Friedmann--Robertson--Walker and Schwarzschild backgrounds. We make a perturbative development in the string coordinates around a {\it null} string configuration; the background geometry is taken into account exactly. In the cosmological case we uncouple and solve the first order fluctuations; the string time evolution with the conformal gauge world-sheet $τ$--coordinate is given by $X^0(σ, τ)=q(σ)τ^{1\over1+2β}+c^2B^0(σ, τ)+\cdots$, $B^0(σ,τ)=\sum_k b_k(σ)τ^k$ where $b_k(σ)$ are given by Eqs.\ (3.15), and $β$ is the exponent of the conformal factor in the Friedmann--Robertson--Walker metric, i.e. $R\simη^β$. The string proper size, at first order in the fluctuations, grows like the conformal factor $R(η)$ and the string energy--momentum tensor corresponds to that of a null fluid. For a string in the black hole background, we study the planar case, but keep the dimensionality of the spacetime $D$ generic. In the null string expansion, the radial, azimuthal, and time coordinates $(r,ϕ,t)$ are $r=\sum_n A^1_{n}(σ)(-τ)^{2n/(D+1)}~,$ $ϕ=\sum_n A^3_{n}(σ)(-τ)^{(D-5+2n)/(D+1)}~,$ and $t=\sum_n A^0_{n} (σ)(-τ)^{1+2n(D-3)/(D+1)}~.$ The first terms of the series represent a {\it generic} approach to the Schwarzschild singularity at $r=0$. First and higher order string perturbations contribute with higher powers of $τ$. The integrated string energy-momentum tensor corresponds to that of a null fluid in $D-1$ dimensions. As the string approaches the $r=0$ singularity its proper size grows indefinitely like $\sim(-τ)^{-(D-3)/(D+1)}$. We end the paper giving three particular exact string solutions inside the black hole.