Phase transitions in compact stars
نویسندگان
چکیده
منابع مشابه
Single-flavor CSL phase in compact stars
We suggest a scenario where the three light quark flavors are sequentially deconfined under increasing pressure in cold asymmetric nuclear matter as, e.g., in neutron stars. The basis for our analysis is a chiral quark matter model of Nambu–Jona-Lasinio (NJL) type with diquark pairing in the spin-1 single flavor (CSL), spin-0 two flavor (2SC) and three flavor (CFL) channels. We find that nucleo...
متن کاملThe Energy Release–stellar Angular Momentum Independence in Rotating Compact Stars Undergoing First-order Phase Transitions
We present the general relativistic calculation of the energy release associated with a first order phase transition (PT) at the center of a rotating neutron star (NS). The energy release, Erel, is equal to the difference in mass-energies between the initial (normal) phase configuration and the final configuration containing a superdense matter core, assuming constant total baryon number and th...
متن کاملQuark phases in neutron stars and a “ third family ” of compact stars as a signature for phase transitions ∗
Quark phases in neutron stars and a " third family " of compact stars as a signature for phase transitions * Abstract The appearance of quark phases in the dense interior of neutron stars provides one possibility to soften the equation of state (EOS) of neutron star matter at high densities. This softening leads to more compact equilibrium configurations of neutron stars compared to pure hadron...
متن کاملCosmological Gravitational Wave Background from Phase Transitions in Neutron Stars
It has recently been suggested that collapse of neutron stars induced by a phase transition to quark matter can be a considerable source of gravitational waves with kHz frequencies. We demonstrate that if about one percent of all neutron stars undergo this process, the resulting cosmological gravitational wave background would reach about 10 times the critical density. The background would peak...
متن کاملPhase Transitions in Neutron Stars and Maximum Masses.
Using the most recent realistic effective interactions for nuclear matter with a smooth extrapolation to high densities including causality, we constrain the equation of state and calculate maximum masses of rotating neutron stars. First- and second-order phase transitions to, e.g., quark matter at high densities are included. If neutron star masses of approximately 2.3 M middle dot in circle f...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: European Journal of Physics
سال: 2005
ISSN: 0143-0807,1361-6404
DOI: 10.1088/0143-0807/26/3/003