Conveners
Session M3
- alfredo estrade (CMU)
Dr
Alex Zylstra
(LANL)
23/05/2018, 14:00
invited talk
The $^3$He+$^3$He, T+$^3$He, and p+D reactions directly relevant to either Stellar or Big-Bang Nucleosynthesis (BBN) have been studied at the OMEGA laser facility using inertially-confined plasmas. These high-temperature plasmas are created using shock-driven `exploding pusher' implosions. The advantage of using these plasmas is that they better mimic astrophysical systems than cold-target...
Ms
Gwenaelle Gilardy
(Notre dame University)
23/05/2018, 14:30
contributed talk
At the end of its life, a massive star can collapse into a proto-neutron star leading to a supernovae explosion. The neutrino flux released during the collapse and the explosion is so significant that the probability of a neutrino interacting with a nucleus can actually influence the nucleosynthesis, the so-called ν-process.
The ν-process is believed to explain the origins of light...
Dr
Gen Chiaki
(Gergia Tech)
23/05/2018, 14:45
contributed talk
Metal-poor stars are living fossils with records of the nucleosyntheses in the early Universe. In particular, extremely metal-poor (EMP) stars are considered to be born in gas clouds having enriched by a single or several supernovae (SNe) of first metal-free (Pop III) stars, and thus we can indirectly constrain the properties of Pop III SNe from the metal content and elemental abundance ratio...
Ms
Kaitlin Rasmussen
(University of Notre Dame)
23/05/2018, 15:00
contributed talk
We present an analysis of the elemental abundances for a sample of 34
relatively bright carbon-enhanced metal-poor (CEMP) stars with [Fe/H] <
-2 and [C/Fe] > +0.7, identified from among candidate very metal-poor
stars observed by the RAVE survey. Although RAVE does not obtain carbon
abundance estimates, medium-resolution (R ~ 1,800) spectroscopic
follow-up of some 1700 RAVE stars...
Qian Liu
(University of Notre Dame)
23/05/2018, 15:15
contributed talk
The main neutron source reactions for the s-process are $^{\mathrm{13}}$C($\alpha $,$n )^{\mathrm{16}}$O and $^{\mathrm{22}}$Ne($\alpha $,$n )^{\mathrm{25}}$Mg. The previous cross section measurements were confined to $\alpha$-energies higher than the Gamow windows[1]. The $^{\mathrm{10}}$B($\alpha $,$n )^{\mathrm{13}}$N reaction has been sugguested as a possible background neutron source for...