Prof.
Falk Herwig
(University of Victoria)
07/02/2017, 16:45
Poster [Main Conference]
Both 1D stellar evolution models and 3D hydrodynamic simulations suggest that convective shells in evolved massive stars can interact and sometimes even merge. As a first step towards a 3D simulation of an O-C shell merger, we have investigated the dynamic response of the convective flow in the O shell to the burning of C assumed to be present in the fluid entrained from an overlying stable...
Mr
kuan zhu
(National Superconducting Cyclotron Laboratory)
07/02/2017, 16:45
Poster [Main Conference]
Comparison of neutrons and protons emitted in heavy ion collisions is one of the observables to probe the density dependence of symmetry energy [Cou16], which is related to the properties of neutron star. In general, neutrons are difficult to measure and neutron detectors are not as easy to use or as widely available as charged particle detectors. Two neutron walls (NW) called LANA exist at...
Prof.
Paul Woodward
(University of Minnesota)
07/02/2017, 16:45
Poster [Main Conference]
Our team at the University of Minnesota has a new and enhanced PPMstar simulation code under active development, with assistance from the University of Victoria team, especially with the design for handling nucleosynthesis processing. An interesting new feature will be the ability to automatically perform nucleosynthesis processing as a run progresses as a part of the run itself. The plan is...
Dr
Pierre Morfouace
(NSCL)
07/02/2017, 16:45
Poster [Main Conference]
The momentum-dependent potentials for neutrons and protons at energies well away from the Fermi surface cause both to behave as if their inertial masses are effectively 70% of the vacuum values. This effective mass describes the non-locality both in space and in time of the nuclear effective interactions and the Pauli exchange. This similarity in effective masses (isoscalar effective mass) may...
Rekam Giri
(Ohio University, Athens, OH, USA)
07/02/2017, 16:45
Poster [Main Conference]
The 12C(α,γ)16O reaction is one of the most important nuclear reactions in astrophysics, as it determines the C/O ratio at the end of helium burning and it has a strong influence on the stellar evolution and final fate of red giant stars. We have used the DRAGON recoil separator for the measurements of the 12C(α,γ)16O reaction at the higher energies of E_c.m. = 3.7, 4.0, and 4.2 MeV. The...
Ms
Kristyn Brandenburg
(Ohio University)
07/02/2017, 16:45
Poster [Main Conference]
The origin of the elements from roughly zinc-to-tin (30
Cathleen Fry
(MSU/NSCL)
07/02/2017, 16:45
Poster [Main Conference]
In classical novae, the \ce{^{30}P}($p,\gamma$)\ce{^{31}S} reaction potentially acts as a bottleneck in nucleosynthesis flow to higher masses. Knowledge of this reaction rate is necessary for the modeling of elemental and isotopic ratios in classical novae, which affect proposed nova thermometers and presolar grain identification, respectively. The rate is dominated by resonant capture, and...
Donald Willcox
(Stony Brook University)
07/02/2017, 16:45
Poster [Main Conference]
It has long been understood that pre-supernova white dwarf (WD) stars can possess sufficiently high densities that Na-23 synthesized via C-fusion undergoes electron capture to Ne-23. These Ne-23 nuclei may be carried by convection to regions of lower density where they revert via beta decay to Na-23. Cyclic reactions of this sort constitute the Urca process in WDs, which is theorized to...
Mr
Pranjal Tiwari
(MSU)
07/02/2017, 16:45
Poster [Main Conference]
Calcium is an element that can be produced in astrophysical explosions called classical novae. There are discrepancies between the abundance of Calcium observed astronomically in novae and what we expect to see based on astrophysical models. The present work describes preparations for a nuclear physics experiment designed to measure the energies of the excited states of 39Ca. Unbound states...
Mr
Shree Neupane
(Central Michigan University)
07/02/2017, 16:45
Poster [Main Conference]
The mass of the isotope is an important parameter in Nuclear Astrophysics to model various stellar processes. Among the various methods used to measure mass of isotopes, Time-of-Flight Mass measurement technique is suitable for very unstable isotopes. This technique is based on measuring the time-of-flight and magnetic rigidity of isotopes with high precision in a beam of fast ions. The...
Dr
Juan Carlos Zamora Cardona
(NSCL)
07/02/2017, 16:45
Poster [Main Conference]
Charge-exchange reactions at intermediary energies is a powerful tool to study
spin-isospin excitations in nuclei. In particular, these type of reactions
serve as a direct method for the extraction of the Gamow-Teller (GT) transition
strengths which are of importance for a variety of applications where
weak transition strengths play a role (e.g. electron capture and $\beta$-decay...
Ilka Petermann
(Arizona State University)
07/02/2017, 16:45
Poster [Main Conference]
Massive stars are essential to the evolution of galaxies due to their intense radiation and strong winds as well as their powerful deaths as supernovae. In this study, we aim at understanding the non-monotonic behavior of crucial properties like
the final iron-core masses of massive stars in analyzing stellar models with respect to the influence of underlying numerics such as spatial and...
Mr
Shiv Kumar Subedi
(Ohio University)
07/02/2017, 16:45
Poster [Main Conference]
Recent observational advances have enabled high resolution mapping of 44Ti in core-collapse supernovae (CCSN) remnants. Comparison between observations and 3D models provide stringent constraints on the CCSN mechanism. However, recent work has identified several uncertain nuclear reaction rates that influence 44Ti production in model calculations. We are using MESA as a tool to investigate the...
Neerajan Nepal
(Central Michigan University)
07/02/2017, 16:45
Poster [Main Conference]
The rapid neutron capture process (r-process) is a nucleosynthesis process and is responsible for about half of the abundance of elements heavier than iron in the solar system and for most of those abundances in very metal-poor stars. The probability of β-delayed neutron emission is one of the key feature to understand the nature of the r-process nucleosynthesis model. The β-delayed neutron...
Mr
Chris Seymour
(University of Notre Dame)
07/02/2017, 16:45
Poster [Main Conference]
The St. George recoil separator located in the Nuclear Science Lab at Notre Dame will be used to measure radiative alpha capture reaction cross sections of astrophysical interest. Low reaction rates at energies found in stellar environments inhibit standard measurement techniques due to a relatively high gamma background. Recoil separators aim to eliminate this background problem by directly...
Mr
Jonathan Barney
(NSCL)
07/02/2017, 16:45
Poster [Main Conference]
The newly constructed SπRIT Time Projection Chamber (TPC) [1] has been used in a series of experiments at RIBF in RIKEN, Japan. This detector utilizes a 12,096 channel pad plane to reconstruct 3D images of events that occur inside a detection region. This makes the detector very useful to study nuclear reactions. The main goal of this device is to place constraints on the nuclear symmetry...
Dr
Satyen Baindur
(Affiliation after 1/1/2017 TBD)
07/02/2017, 16:45
Poster [Main Conference]
The detection of inspiral gravitational waves in the black hole binary merger reported by LIGO (2015) has kindled strong interest in the frequency of other possible detections, and their implications for stellar formation models and the black hole mass function, among other long-standing classical problems in astrophysics. However, LIGO is also sensitive to, and is looking for, continuous...
Ryan Connolly
(Michigan State University)
07/02/2017, 16:45
Poster [Main Conference]
The free neutrons in a neutron star are thought to be paired in a superfluid. The critical temperatures and the density at which the neutron pairing gap closes, however, are poorly constrained. Neutron superfluid singlet pairing gap models that close in the core imply that free neutrons are superfluid throughout the entire crust, while gaps that close in the crust allow a layer of normal...
Mr
Tamas Budner
(Michigan State University)
07/02/2017, 16:45
Poster [Main Conference]
Theoretical calculations of the relative isotopic abundances of classical nova ejecta depend heavily on certain radiative proton-capture reaction rates. Perhaps the most important uncertainty is the thermonuclear rate of the 30P(p,γ)31S reaction. Currently, technical challenges make measuring this reaction directly unfeasible. However, the 30P(p,γ)31S reaction is dominated by resonances,...
Mr
Devin Whitten
(University of Notre Dame)
07/02/2017, 16:45
Poster [Main Conference]
We present results for surface temperature, metallicity ([Fe/H]), carbonicity ([C/Fe]) and surface gravity (log g) determinations with preliminary data from the Javalambre Photometric Local Universe Survey (J-PLUS). Spectra with stellar parameters obtained from the SEGUE Stellar Parameter Pipeline (SSPP) were used in conjunction with synthetic magnitudes transformed to the J-PLUS system to...
Mr
Sean Sweany
(MSU)
07/02/2017, 16:45
Poster [Main Conference]
The symmetry energy contribution in the nuclear equation of state (EOS) can be used to learn about properties in the interior of neutron stars, like the composition of the star as well as its radius. So far constraints have been made on the EOS in symmetric nuclear matter in a range from 1 to 4.5 times saturation density while constraints on asymmetric nuclear matter above saturation density...
Mr
Carl Fields
(Michigan State University)
07/02/2017, 16:45
Poster [Main Conference]
We investigate properties of core-collapse supernova (CCSN) progenitors with respect to the composite uncertainties in the reaction rates using the stellar evolution toolkit, Modules for Experiments in Stellar Astrophysics (MESA) and the probability density functions in the reaction rate library, STARLIB. In total, 1000 15 solar mass stellar models are evolved from the pre main-sequence to...
Ms
Maria Barrios Sazo
(Stony Brook University)
07/02/2017, 16:45
Poster [Main Conference]
A tight binary system in which a millisecond pulsar is ablating its low mass companion star is known as a Black Widow Pulsar (BWP) system. BWP systems have been observed in pulsar eclipses attributed to a cloud surrounding the evaporating companion star. We will describe the methods we are employing for modeling the interaction between the pulsar winds and the companion star. We are...
SOM PANERU
(Ohio University)
07/02/2017, 16:45
Poster [Main Conference]
Precise measurement of s-wave scattering lengths for 7Be+p system
will improve the uncertainty in astrophysical S-factor (S17). We used
R-matrix code AZURE2 for simultaneous fitting of the available 7Be+p elastic and inelastic scattering data including results from Oak Ridge National Laboratory (ORNL). The best fit R-matrix parameters are used to extract the scattering lengths.
Jacob Davison
(Central Michigan University)
07/02/2017, 16:45
Poster [Main Conference]
Computer simulations are valuable in predicting, verifying, and constraining experimental results. The simulation that this poster describes was a project for a collaboration between Central Michigan University, Michigan State University, and North Carolina State University that is studying the mysterious νp-process and its role in nucleosynthesis within core-collapse supernovae. The reaction...
Dr
Sunghoon (Tony) Ahn
(JINA/NSCL)
07/02/2017, 16:45
Poster [Main Conference]
(α,xn) reactions have been identified as the main production mechanism of Z=38-47 abundances in neutrino driven winds during core-collapse supernovae scenario. Recent sensitivity studies showed that uncertainties in (α,xn) reaction rates directly affect calculated abundances in the neutrinodriven wind models with an impact that is comparable to that from astrophysical uncertainties. Current...
Ms
Kaitlin Rasmussen
(University of Notre Dame)
07/02/2017, 16:45
Poster [Main Conference]
We investigate the distribution of stellar carbon abundances in the early Universe and propose a scenario that includes primary carbon production by the massive first-generation stars, recorded in the atmospheres of CEMP-no stars (which show no over-abundances of neutron-capture elements), and secondary carbon production by subsequent generations of AGB stars, recorded in the subset of...
Mr
Santosh Gaire
(Central Michigan University)
07/02/2017, 16:45
Poster [Main Conference]
The mass of a nucleus and its binding energy is one of the most fundamental nuclear properties. The masses of nuclides far from the valley of stability provide information on decay and reaction energies, as well as the nuclear structure that is preeminent for modeling stellar nucleosynthesis. The Time-Of-Flight mass measurement is one technique, which is well-known by its ability to...
Dr
Rana Ezzeddine
(MIT)
07/02/2017, 16:45
Poster [Main Conference]
Ancient ultra-metal-poor (UMP) stars are rare relics of the early Universe. They provide unique insights into
the first nucleosynthesis events and the formation of the first (Pop III) stars. Detailed comparisons of supernova (SN) nucleosynthesis yields with UMP stellar abundances allow us to constrain the nature and shape of the initial mass function (IMF) of Pop III stars. We present new...