Pouthier Vincent
Institut UTINAM, Université de Franche-Comté, CNRS UMR 6213, 25030 Besançon Cedex, France.
J Chem Phys. 2022 Apr 21;156(15):155101. doi: 10.1063/5.0087200.
An attractive Bose-Hubbard model is applied for describing quantum self-trapping in an extended star graph. In the strong coupling limit and when two excitons are created on the core of the star, the dynamics is dominated by pair states whose properties are governed by the branch number N. When N = 2, the star reduces to a linear chain so that the energy does not self-localize. Conversely, when N ≥ 3, restructuring of the eigenstates arises and a low-energy state occurs describing a pair localized on the core of the star. Preferentially excited, this localized state gives rise to quantum self-trapping of the energy, a process that intensifies as N increases.
一个引人注目的玻色-哈伯德模型被用于描述扩展星型图中的量子自陷现象。在强耦合极限下，当在星型图的核心产生两个激子时，动力学由对态主导，其性质由分支数N决定。当N = 2时，星型图退化为线性链，因此能量不会自局域化。相反，当N≥3时，本征态会发生重构，出现一个低能态，描述一对局域在星型图核心的粒子。优先被激发后，这个局域态会导致能量的量子自陷，随着N的增加，这个过程会加剧。
