Nuclear Physics in Astrophysics III

Abstract

The present special issue of Journal of Physics G: Nuclear and Particle Physics contains all peer-reviewed contributions to the proceedings of this conference.NPA3 is the third conference in the Nuclear Physics in Astrophysics series of conferences devoted to the interplay between nuclear physics and astrophysics. The first and second editions of the series were held in 2002 and 2005 in Debrecen, Hungary. NPA3 has been organized under the auspices of the Nuclear Physics Board of the European Physical Society as its XXI Divisional Conference.

A new study of the 22Ne(p, γ)23Na reaction deep underground: Feasibility, setup and first observation of the 186 keV resonance

“…10) clearly confirm the linear behaviour expected from previous work using other target gases and beams [34][35][36]. The target density can therefore be described by the following relation:…”

“…This effect has been studied in detail previously in static gas targets of 14 N gas, using the resonance scan method [34,35], and of 3 He gas, using double elastic scattering [36]. In the present work, again the resonance scan method is used.…”

“…The beam heating parameter α = (0.44 ± 0.05) × 10 −3 determined here for proton beam in neon gas has to be compared to α = 0.5×10 −3 for proton beam in nitrogen gas [34,35], and (0.91 ± 0.19) × 10 −3 for 4 He + beam in helium gas [36], from former studies. The differences may be explained by the different heat transport coefficients in different gases.…”

“…It is known from previous work [34][35][36] that the beam heating effect is proportional to the power dissipated by the beam inside the gas per unit length, which, in turn, is given by:…”

The impact of recent advances in laboratory astrophysics on our understanding of the cosmos

“…Work on this reaction over the past decade has been intense. New measurements have been made with both direct methods (Formicola et al 2004;Imbriani et al 2005;Runkle et al 2005;Bemmerer et al 2006b;Lemut et al 2006;Marta et al 2008) and indirect methods, covering the energy range between 70 and 480 keV (see Wiescher et al 2010 andAdelberger et al 2011 for summaries). After summing all transitions S tot 1 14 (0) = 1.66 ± 0.12 keV barn was obtained (Adelberger et al 2011), a value nearly a factor of two below previously recommended values.…”