Response function for supernova and neutron star crust with chiral effective theory
ORAL
Abstract
We have been studied dynamic response function in an environment of supernova and static response function for neutron star crust. We use different cutoff energies (414, 450, and 500 MeV) at dynamic response function in chiral effective theory. We use nuclear potential from chiral effective theory with 2N and 3N interaction to describe microscopic nucleon-nucleon interaction in static response function. We check the effect of 2N and 3N force in a variety of densities and transferred momentum from neutrinos to pure neutron matter. We checked 2N interaction is opposite to 3N interaction at low momentum. The effect of 2N and 3N disappeared in high momentum. While q is zero, the effect of 3N force in ChEFT is negligible at low densities. 3N force canceled out by 2N at higher densities. Similar phenomena are detected in the equation of state. The equation of state is repulsive for 3N and attractive for 2N. The response is sensitive to choose the nuclear potential. Therefore, I emphasize the importance of nuclear potential.
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Presenters
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Eunkyoung Shin
Cyclotron Institute and Department of Physics and Astronomy, Texas A&M University, College Station, Texas 77843, USA
Authors
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Eunkyoung Shin
Cyclotron Institute and Department of Physics and Astronomy, Texas A&M University, College Station, Texas 77843, USA
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Jeremy W Holt
Cyclotron Institute and Department of Physics and Astronomy, Texas A&M University, College Station, Texas 77843, USA
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Ermal Rrapaj
1 Department of Physics, University of California, Berkeley, California 94720, USA. 2 School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455,
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Sanjay K Reddy
Institute for Nuclear Theory and Department of Physics, University of Washington, Seattle, Washington 98195, USA