π凝聚态中的弱过程对中子星振动的阻尼效应

本文主要讨论了中子星内部发生从正常中子物态到π凝聚物态相变所产生的星体振动的阻尼,由弱作用反应u(p₁)→u(p₂)+e^-+v_e和u(p₁)+e^-→u(p₂)+v_e算出振动阻尼时标,并考虑了中子星内部的热演化。关键词：

DAMPING EFFECTS OF WEAK PROCESSES IN PION CONDENSATE ON NEUTRON STAR VIBRATION

In the core of some massive neutron star there may appear pion condensate. The weak processes such as μ(p₁)→μ(p₂) + e^- + v_e and μ(p₁) + e→μ(p₂) + v_e (i. e. equation (9) and (10) of this paper), in pion condenate,have been proved to be essential in damping the radial vibrations in the neutron star. The time scale of this damping effect is model depen dent and may be several days.Considering processes (9) and (10), the equilibrium condition in the pion condensate is μ_π=μ_e. However, only irreversible processes could damp the vibration, so the key parameter here should be ξ=(μ_π,-μ_e)/kT describing the deviation from equilibrium. In this paper, we have derived the reaction rates of processes (9) and (10), and the related neutrino luminosities, and done numerical calculations. Results obtained are the relations of W-t and T-t, as shown in Fig. 2 and 3, using W_v and T to denote the vibrational energy and the temperature of the neutron star respectively.