在准粒子描述下，采用自洽的热力学方法，考虑奇异夸克物质（SQM）的介质效应，计算了高温近似下奇异夸克物质的体粘滞系数。发现介质效应对奇异夸克物质的体粘滞系数有很大影响，这使得观测数据不再排除两味色超导相奇异星的存在。

在高密情况下考虑了夸克间弱的耦合，直接应用微扰计算得到的热力学势计算了奇异夸克物质（SQM）的体粘滞系数，发现介质效应使SQM的粘滞性提高2个量级左右。

We study the bulk viscosity of strange quark matter (SQM) in density dependent quark mass model(DDQM) under the background of self-consistent thermodynamics. The correct formulae, with which the viscosity can be evaluated, are derived. We also find that the viscosity in DDQM can be higher by 2 to 3 orders of magnitude than MIT bag model. We calculate the damping time scales due to viscosity coupled to r-modes. The numerical results show the time scale can't be shorter than 10-1s.

The effect of a strong magnetic field on the dominant neutrino emissivity in strange stars is investigated. In an ultra strong magnetic field, there exists an enhanced neutrino emission because the charged particles are confined to the lowest Landau level. The results show that the neutrino emissivity is proportional to T5 instead of conventional T6, which implies more rapid cooling behavior in magnetars than usual strange stars.

We utilize the bulk viscosity of interacting strange quark matter to reevaluate the damping timescale. The presence of a medium effect of bulk viscosity leads to a stronger damping of r-modes, which can be over an order of magnitude for realistic parameters. We find that the r-mode instability window is narrowed because of the medium effect, and hence, when a pulsar reaches the instability window, it will slow down by gravitational wave emission to a period of only 1.78ms instead of the 2.5ms given by early estimates. As a theoretical upper rotation limit of pulsars, the period of 1.78ms is very close to the two most rapidly spinning pulsars known, with periods of about 1.6ms.