Research in Gravitation Theory and Astrophysics

林德布洛姆教授将继续他对引力和天体物理学的理论研究。他将强调强引力场在其中发挥重要作用的天体物理情况。这些问题可分为四个主要领域：a)相对论恒星的脉动和稳定性，b)中子星的超流体力学，c)耗散相对论流体力学理论，d)相对论恒星结构的基本数学问题。将在每个领域开展具体的研究问题，例如：a)将发展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。这一近似是基于这样一个事实，即引力辐射只与中子星中的初级物理感兴趣的模式弱耦合。B)评估超流流体动力学对旋转中子星引力辐射不稳定性的影响的计划将继续进行。下一步是完成计算机代码的调试，这些代码评估快速旋转的超流中子星的模式。C)研究散度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。人们希望这两类理论都能被识别出来，并且这些理论将包含一个强有力的候选者，即耗散相对论流体理论。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.