Three-dimensional hydrodynamical simulations unravel the evolution of SN 1987A from the explosion to the supernova remnant (Opens in a new window)
Dr. Masaomi Ono
Abstract: Supernova 1987A (SN 1987A) provides a unique opportunity to unravel the evolution of core-collapse supernovae (CCSNe) from the explosions to their supernova remnants (SNRs) thanks to its proximity and youth. Early observation of iron lines has indicated matter mixing during the explosion to convey innermost 56Ni to outer layers. Since the density structure of the progenitor star affects the matter mixing, it provides a hint on the properties of the progenitor star.
Constraining Tidal deformability from finite nuclei data, Bijay Agrawal (Saha Institute of Nuclear Physics) (Opens in a new window)
*Please note that this seminar will take place at 11:00am ET
Saha Institute of Nuclear Physics
The tidal deformability inferred from the Gravitational Waves, which are emitted by merging neutron stars, are instrumental in determining the equation of state (EoS) of dense matter. The importance of the observed finite nuclei properties in unveiling the correlations of the tidal deformability with the key EoS parameters will be discussed.
PAN-CAKE is a free online masterclass for teachers scheduled on March 13 & 14, 12:30-4:00pm ET. Science teachers (from pre-service to veterans) in the US and Canada will learn about world-class scientific research in nuclear astrophysics at MSU’s Facility for Rare Isotope Beams. This is an opportunity to meet scientists and other educators, take a “virtual tour” of a leading rare isotope laboratory, collect tools and demos for your curriculum, and discover the future of research.
Michigan State University
Are you connected with your “self”? with others? With your past and present?
In this presentation specially dedicated to graduate students and postdocs, we will explore linkages with mental well-being. There will be opportunities for discussion and questions.
University of Regina
Hosted by: Mansi Saxena (Ohio University)
r-process nucleosynthesis and the production of heavy elements: A nuclear physics perspective (Opens in a new window)
(ECT*), Trento, Italy
About half of the chemical elements heavier than iron that found in nature are produced during the rapid neutron-capture process (r process). In August 2017, the observation of the kilonova light curve, an electromagnetic transient produced by the radioactive decay of r-process nuclei synthesized during the merger of two neutron stars, marked the beginning of a new era for r-process studies where nucleosynthesis predictions can be directly confronted with astronomical observations.
Supernovae produce elements across the periodic table and are probes of stellar evolution, explosion physics and compact object formation.
Nuclear-physics and multi-messenger constraints on the neutron-star equation of state (Opens in a new window)
Los Alamos National Laboratory
Neutron stars contain the largest reservoirs of degenerate fermions, reaching the highest densities we can observe in the cosmos, and probe matter under conditions that cannot be recreated in terrestrial experiments. Throughout the Universe, a large number of high-energy, cataclysmic astrophysical collisions of neutron stars are continuously occurring.
JINA-CEE and IReNA will organize “JINA Horizons” on November 30 - December 4, 2020 - a virtual meeting that brings together the international nuclear astrophysics community to discuss open questions and future directions.
Texas A&M University
A small fraction of old, metal-poor stars exhibits large enhancements in elements produced in the rapid neutron capture (r-)process. Their chemical composition, mapped through detailed abundance analysis, is a direct fingerprint of the elements produced in the stellar generation before them. This makes them excellent laboratories for studying the r-process. The first r-process enhanced star was discovered over 30 years ago. Since then, about 30 highly r-process enhances stars have been found in the Milky Way halo.
Nucleosynthesis and observational evidences of magneto rotational driven supernovae (Opens in a new window)
Abstract: About half of the heavy elements in our Universe are synthesized by one process, the rapid neutron capture process (r-process). This process requires extreme and violent environments that achieve the necessary neutron-rich conditions. Neutron star mergers and magneto rotational driven supernovae are promising candidates to host the r-process. We investigate the r-process from an observational as well as a nucleosynthesis point of view.
University of Hertfordshire
Abstract: Galactic chemical evolution (GCE) can provide stringent constraints not only on nuclear astrophysics but also on the formation and evolutionary history of the Milky Way itself, through an approach called Galactic archeology.
Constraining the key input to X-ray burst models and the role of active-targets (Opens in a new window)
University of Notre Dame
Abstract: Type-I X-ray bursts (XRBs) are among the most frequent thermonuclear explosions in the Universe. Detailed models are required to constrain the mass-radius relation and other underlying physics through comparisons between the observations and models.
Core-Collapse Supernovae: From Neutrino-Driven 1D Explosions to Light Curves and Spectra (Opens in a new window)
North Carolina State University
Abstract: The number of observed core-collapse supernova lightcurves is growing every day, providing valuable clues about progenitors, stellar evolution, the explosion mechanism, the nuclear equation of state, nucleosynthesis, and the formation of neutron stars and black holes. However, interpreting electromagnetic observables correctly is a formidable challenge, one that requires detailed and accurate theoretical modeling.
New equations of state constrained by nuclear physics, observations, and high-density QCD calculations (Opens in a new window)
Abstract: We present new equations of state for applications in core-collapse supernova and neutron star merger simulations. We start by introducing an effective mass parametrization that is fit to recent microscopic calculations up to twice saturation density. This is important to capture the predicted thermal effects, which have been shown to determine the proto-neutron star contraction in supernova simulations.
PAN is a free week-long program for current high school students.
Online PAN: Both Michigan State University and the University of Notre Dame have cancelled in-person K-12 summer programs for 2020.
The Importance of Nuclear Astrophysics in the Evolution of the Elements in Galaxies (B. Cote) (Opens in a new window)
The Seminar will begin at 2pm EST Online Seminar featuring Benoit Cote (Konkoly Observatory)
POSTPONED - Taking the Temperature: Statistical Nuclear Physics for Astrophysics and Applications (T3) (Opens in a new window)
Statistical estimates of nuclear reaction rates are essential ingredients for astrophysical model calculations, e.g. r-process nucleosynthesis in neutron star mergers, and nuclear applications, e.g. next generation nuclear reactor performance. Rate calculations require experimental or theoretical constraints for nuclear properties such as level densities (temperature), gamma-strength functions, particle optical potentials, and level spin distributions.