Research in Gravitation Theory and Astrophysics

Lindblom教授将继续他在引力和天体物理学方面的理论研究。 他将强调天体物理的情况下，强引力场发挥了重要作用。 这些问题可以分为四个主要领域：a）相对论恒星的脉动和稳定性，B）中子星中的超流流体动力学，c）耗散相对论流体动力学理论，d）相对论恒星结构中的基本数学问题。 将在这些领域中的每一个领域进行具体的研究问题，例如：a）将开发一种新的近似方法来评估快速旋转的完全相对论恒星模型的模式。 这种近似是基于这样一个事实，即引力辐射耦合到中子星的主要物理感兴趣的模式只有微弱的。 B）评价超流体流体动力学对旋转中子星引力辐射不稳定性影响的方案将继续进行。 下一步是完成计算机代码的调试，以评估快速旋转的超流中子星的模式。 （3）研究发散型耗散相对论流体理论与基于拉格朗日的耗散相对论流体理论之间的关系。 人们希望，这套理论属于这两个类可以确定，这些将包含一个强有力的候选人是理论的耗散相对论流体。 d）将进一步研究通过测量中子星的质量和半径来确定核状态方程的可能性。

Professor Lindblom will continue his theoretical research on gravitation and astrophysics. He will emphasize astrophysical situations in which strong gravitational fields play a significant role. These problems can be divided into four major areas: a) the pulsations and stability of relativistic stars, b) superfluid hydrodynamics in neutron stars, c) dissipative relativistic hydrodynamic theories, and d) fundamental mathematical problems in relativistic stellar structure. Specific research problems in each of these areas will be carried out, for example: a) A new approximation method to evaluate the modes of rapidly rotating fully relativistic stellar models will be developed. This approximation is based on the fact that gravitational radiation couples only weakly to the modes of primary physical interest in neutron stars. b) The program to evaluate the effects of superfluid hydrodynamics on the gravitational radiation instability of rotating neutron stars will be continued. The next step is to finish debugging the computer codes that evaluate the modes of rapidly rotating superfluid neutron stars. c) The relationship between the dissipative relativistic fluid theories of divergence type and the Lagrangian based dissipative relativistic fluid theories will be investigated. It is hoped that the set of theories which belong to both classes can be identified and that these will contain a strong candidate to be THE theory of dissipative relativistic fluids. d) Further investigations into the possibility of determining the nuclear equation of state by measuring the masses and radii of neutron stars will be carried out.