NIC-XIV School 2016

Session

Students2

15 Jun 2016, 15:30

Library Hall, Central Library (Niigata University (Ikarashi Campus))

26. Insights on the first stars from CEMP-no stars

Mr Arthur Choplin (Geneva Observatory)

15/06/2016, 15:30

Short Talk

The CEMP-no stars (Carbon-Enhanced Metal-poor stars with no sign or weak signs for the presence of s- or r-elements) are long-lived small mass stars presenting a very low iron content and overabundances of carbon. Their chemically peculiar abundance pattern could be inherited from a previous massive star (the source star) that has lost mass through winds or at the time of the supernova....

30. Single-particle energies of oxygen isotopes in the unitary-model-operator approach

Mr Takayuki Miyagi (Department of Physics, the University of Tokyo)

15/06/2016, 15:40

Short Talk

Owing to the recent computational progress, the medium-mass nuclei have been investigated recently by the ab initio methods such as the coupled-cluster method, in-medium similarity renormalization group approach, and self-consistent Green’s function method. Similarly to these methods, the unitary-model-operator approach (UMOA) can also be applied to the medium-mass nuclei. So far, we...

33. Impact of rotation and convective boundary mixing in low mass AGB stars

Ms Jacqueline Den Hartogh (Keele University)

15/06/2016, 15:50

Short Talk

After the central He burning in exhausted, stars with an initial mass of 1.5-3 solar masses start the AGB phase. In this phase, the s-process takes place, which is producing about half of all elements heavier than iron. Our non-rotating AGB stellar models calculated with MESA (see Battino et al., submitted) include a treatment of convective boundary mixing based on the results of hydrodynamic...

36. Lfitetime measurements to constrain the 30P(p,g)31S rate at classical nova temperatures

Cathleen Fry (MSU/NSCL)

15/06/2016, 16:00

Short Talk

In classical novae, the 30P(p,g)31S 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. While most of the resonance energies are known experimentally, the...

37. Development of high time resolution detector for RI beam using Cherenkov light

Ms Eri Miyata (graduate school of science Niigata University)

15/06/2016, 16:10

Short Talk

In order to improve the resolution of particle identification for radioactive beams, it is important to develop the high time resolution detector to measure TOF. We have developed the high time resolution TOF detector which detects the Cherenkov light emitted when RI beam passes through the high refractive index radiator. Generally, the plastic scintillation counter has been commonly used as a...

47. Overview of the BRIKEN Project

Mr Vi Phong (RIKEN Nishina Center)

15/06/2016, 16:20

Short Talk

Vi Ho Phong1,2, Shunji Nishimura1, Giuseppe Lorusso3,4, Jorge Agramunt5, Alejandro Algora5, Roger Caballero-Folch6, Francisco Calvino7, Guillem Cortes7, Thomas Davinson8, Iris Dillmann6, Alfredo Estrade9, Robert Grzywacz10, Gabor Kiss1, Keishi Matsui1, Fernando Montes12, Cesar Domingo Pardo5, Albert Riego8, Krzysztof Rykaczewski13, Jose Luis Tain5, Ariel Tarifeno Saldivia7, Alvaro Tolosa5,...