From Multifragmentation to Supernovae and Neutron Stars
نویسندگان
چکیده
The thermodynamics properties of globally neutral dense stellar matter are analyzed both in terms of mean field instabilities and structures beyond the mean field. The mean field response to finite wavelenght fluctuations is calculated with the realistic Sly230a effective interaction. A Monte Carlo simulation of a schematic lattice Hamiltonian shows the importance of calculations beyond the mean field to calculate the phase diagram of stellar matter. The analogies and differences respect to the thermodynamics of nuclear matter and finite nuclei are stressed.
منابع مشابه
Probing the Coulomb field in relativistic collisions
Two main questions determine the recent directions of the research in nuclear dynamics. One is the role of the Coulomb field in diluted nuclear matter: in cosmological objects (e.g. neutron stars, supernovae) theoretical studies relate it to the formation of crystalline structures by frustration effects [1]. The Coulomb field can be probed experimentally at the nuclear scale, where it rules the...
متن کاملDifferent Magnetic Field Distributions in Deformed Neutron Stars
In this work, we review the formalism which would allow us to model magnetically deformed neutron stars. We study the effect of different magnetic field configurations on the equation of state (EoS) and the structure of such stars. For this aim, the EoS of magnetars is acquired by using the lowest order constraint variational (LOCV) method and employing the AV18 potential....
متن کاملIsospin Observables in Multifragmentation of Relativistic Projectiles
Multifragmentation is a universal phenomenon occurring when a large amount of energy is deposited in a nucleus. It was observed in high energy nuclear reactions induced by hadrons and heavy ions. It is believed to be a manifestation of the nuclear liquid-gas phase transition which is also expected to occur in crusts of neutron stars and in supernova explosions. This reaction offers a unique pos...
متن کاملSpin and Isospin Asymmetry, Equation of State and Neutron Stars
In the present work, we have obtained the equation of state for neutron star matter considering the in uence of the ferromagnetic and antiferromagnetic spin state. We have also investigated the structure of neutron stars. According to our results, the spin asymmetry stiens the equation of state and leads to high mass for the neutron star.
متن کاملNucleosynthesis in early supernova winds III: No significant contribution from neutron-rich pockets
Recent nucleosynthesis calculations of Type II supernovae using advanced neutrino transport determine that the early neutrino winds are proton-rich. However, a fraction of the ejecta emitted at the same time is composed of neutron-rich pockets. In this paper we calculate the nucleosynthesis contribution from the neutron-rich pockets in the hot convective bubbles of a core-collapse supernova and...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
عنوان ژورنال:
دوره شماره
صفحات -
تاریخ انتشار 2004