Qualitative properties of solutions to semilinear elliptic equations from the gravitational Maxwell Gauged O(3) Sigma model

Abstract

This article is devoted to the study of the following semilinear equation with measure data which originates in the gravitational Maxwell gauged $O(3)$ sigma model, $$-\Delta u + A_0(\prod^k_{j=1}|x-p_j|^{2n_j} )^{-a} \frac{e^u}{(1+e^u)^{1+a}} = 4\pi\sum_{j=1}^k n_j\delta_{p_j} - 4\pi\sum^l_{j=1}m_j\delta_{q_j} \quad{\rm in}\;\; \mathbb{R}^2.\qquad(E)$$ In this equation the $\{\delta_{p_j}\}_{j=1}^k$ (resp. $\{\delta_{q_j}\}_{j=1}^l$ ) are Dirac masses concentrated at the points $\{p_j\}_{j=1}^k$, (resp. $\{q_j\}_{j=1}^l$), $n_j$ and $m_j$ are positive integers, and $a$ is a nonnegative real number. We set $ N=\sum^k_{j=1}n_j $ and $M= \sum^l_{j=1}m_j$. In previous works \cite{C,Y2}, some qualitative properties of solutions of $(E)$ with $a=0$ have been established. Our aim in this article is to study the more general case where $a>0$. The additional difficulties of this case come from the fact that the nonlinearity is no longer monotone and the data are signed measures. As a consequence we cannot anymore construct directly the solutions by the monotonicity method combined with the supersolutions and subsolutions technique. Instead we develop a new and self-contained approach which enables us to emphasize the role played by the gravitation in the gauged $O(3)$ sigma model. Without the gravitational term, i.e. if $a=0$, problem $(E)$ has a layer's structure of solutions $\{u_\beta\}_{\beta\in(-2(N-M),\, -2]}$, where $u_\beta$ is the unique non-topological solution such that $u_{\beta}=\beta\ln |x|+O(1)$ for $-2(N-M)<\beta<-2$ and $u_{-2}=-2\ln |x|-2\ln\ln |x|+O(1)$ at infinity respectively. On the contrary, when $a>0$, the set of solutions to problem $(E)$ has a much richer structure: besides the topological solutions, there exists a sequence of non-topological solutions in type I, i.e. such that $u $ tends to $-\infty$ at infinity, and of non-topological solutions of type II, which tend to $\infty$ at infinity. The existence of these types of solutions depends on the values of the parameters $N,\, M,\, \beta$ and on the gravitational interaction associated to $a$.