Gravitational waves from the axial oscillation of neutron star considering non-Newtonian gravity  

作　　者：WEN Dehua ZHOU Ying 

机构地区：[1]Department of Physics,South China University of Technology

出　　处：《Nuclear Science and Techniques》2013年第5期38-43,共6页核技术（英文）

基　　金：Supported by National Natural Science Foundation of China(Nos.10947023,11275073 and 11205061);Fundamental Research Funds for the Central University,China(No.2012ZZ0079);sponsored by SRF for ROCS,SEM

摘　　要：The eigen-frequencies of the axial w-modes of neutron star described by a super-soft equation of state(EOS) are investigated,by considering the non-Newtonian gravity.The results show that at the same stellar mass,the frequencies of wI and wI2 for our model are lower than that of the typical EOSs(such as APR); and the frequencies increase with the stellar masses,which is contrary to that of the typical EOSs.These characters may provide a probe to testify the super soft symmetry energy and the non-Newtonian gravity in the future.Moreover,our model also has the universal behavior of the mass-scaled eigen-frequencies as a function of the compactness.The eigen-frequencies of the axial w-modes of neutron star described by a super-soft equation of state （EOS） are investigated, by considering the non-Newtonian gravity. The results show that at the same stellar mass, the frequencies of wl and wn for our model are lower than that of the typical EOSs （such as APR）; and the frequencies increase with the stellar masses, which is contrary to that of the typical EOSs. These characters may provide a probe to testify the super soft symmetry energy and the non-Newtonian gravity in the future. Moreover, our model also has the universal behavior of the mass-scaled eigen-frequencies as a fimction of the compactness.

关 键 词：非牛顿引力 中子星 轴向 引力波 摆动 本征频率 恒星质量 EOS 

分 类 号：O571.5[理学—粒子物理与原子核物理]