Results 331 to 340 of about 781,895 (361)
Constraining the equation of state in neutron-star cores via the long-ringdown signal. [PDF]
Ecker C, Gorda T, Kurkela A, Rezzolla L.
europepmc +1 more source
Collinear Jahn-Teller Ordering Induces Monoclinic Distortion in "Defect-Free" LiNiO<sub>2</sub>. [PDF]
Phillips GS +12 more
europepmc +1 more source
Enhanced production of 60Fe in massive stars. [PDF]
Spyrou A +25 more
europepmc +1 more source
Kilonova simulations: connecting observations with the underlying physics. [PDF]
Collins C, Shingles L, Vijayan V.
europepmc +1 more source
Some of the next articles are maybe not open access.
Related searches:
Related searches:
, 2022
Neutron stars are highly compact astrophysical objects and therefore of utmost relevance to learn about theories of gravity. Whereas the proper equation of state of the nuclear matter inside neutron stars is not yet known, and a wide range of equations ...
J. Kunz
semanticscholar +2 more sources
Neutron stars are highly compact astrophysical objects and therefore of utmost relevance to learn about theories of gravity. Whereas the proper equation of state of the nuclear matter inside neutron stars is not yet known, and a wide range of equations ...
J. Kunz
semanticscholar +2 more sources
Physical Review Letters, 1993
We calculate properties of neutron star matter at subnuclear densities using an improved nuclear Hamiltonian. Nuclei disappear and the matter becomes uniform at a density of about 0.6n(s), where n(s) of about 0.16/cu fm is the saturation density of nuclear matter. As a consequence, the mass of matter in the crusts of neutron stars is only about half as
, Lorenz, , Ravenhall, , Pethick
openaire +2 more sources
We calculate properties of neutron star matter at subnuclear densities using an improved nuclear Hamiltonian. Nuclei disappear and the matter becomes uniform at a density of about 0.6n(s), where n(s) of about 0.16/cu fm is the saturation density of nuclear matter. As a consequence, the mass of matter in the crusts of neutron stars is only about half as
, Lorenz, , Ravenhall, , Pethick
openaire +2 more sources
Nuclear Physics A, 1971
Abstract The matter in neutron stars is essentially in its ground state and ranges in density up to and beyond 3 × 10 14 g/cm 3 , the density of nuclear matter. Here we determine the constitution of the ground state of matter and its equation of state in the regime from 4.3 × 10 11 g/cm 3 where free neutrons begin to “drip” out of the nuclei, up ...
GORDON BAYM +2 more
openaire +1 more source
Abstract The matter in neutron stars is essentially in its ground state and ranges in density up to and beyond 3 × 10 14 g/cm 3 , the density of nuclear matter. Here we determine the constitution of the ground state of matter and its equation of state in the regime from 4.3 × 10 11 g/cm 3 where free neutrons begin to “drip” out of the nuclei, up ...
GORDON BAYM +2 more
openaire +1 more source
Identification of strontium in the merger of two neutron stars
Nature, 2019Half of all of the elements in the Universe that are heavier than iron were created by rapid neutron capture. The theory underlying this astrophysical r-process was worked out six decades ago, and requires an enormous neutron flux to make the bulk of the
D. Watson +17 more
semanticscholar +1 more source

