First measurement of ^4_ΛHe yields in 3 GeV Au+Au collisions shows consistency with ^4_ΛH yields and JAM coalescence model while thermal model overpredicts absolute yields.
Hypernuclear Physics for Neutron Stars
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abstract
The role of hypernuclear physics for the physics of neutron stars is delineated. Hypernuclear potentials in dense matter control the hyperon composition of dense neutron star matter. The three-body interactions of nucleons and hyperons determine the stiffness of the neutron star equation of state and thereby the maximum neutron star mass. Two-body hyperon-nucleon and hyperon-hyperon interactions give rise to hyperon pairing which exponentially suppresses cooling of neutron stars via the direct hyperon URCA processes. Non-mesonic weak reactions with hyperons in dense neutron star matter govern the gravitational wave emissions due to the r-mode instability of rotating neutron stars.
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Hyper-Nuclei $^4_{\Lambda}\hbox{He}$ Production in $\sqrt{s_{\rm{NN}}}$ = 3 GeV Au+Au collisions at RHIC
First measurement of ^4_ΛHe yields in 3 GeV Au+Au collisions shows consistency with ^4_ΛH yields and JAM coalescence model while thermal model overpredicts absolute yields.