Abstract
Frequencies and damping times due to gravitational radiation are calculated for self-bound quark star models. The results are compared with those for neutron star models, and it is found that they differ markedly in less relativistic cases. The difference derived here even based on a simple model of quark stars may be relevant to future theoretical and observational studies, because the oscillation properties depend essentially on the mass and radius for an equilibrium star.
Full Text 
Sign-in/Register to access full text options
Sign-in/Register to access full text options 
Published version (
Free)
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
