Jun 21 – 26, 2015
Dipartimento di Fisica ed Astronomia, Università di Catania
Europe/Rome timezone
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The Trojan Horse Method as a tool for investigating astrophysically relevant fusion reactions

Jun 25, 2015, 4:25 PM
20m
Aula Magna (Dipartimento di Fisica ed Astronomia, Università di Catania)

Aula Magna

Dipartimento di Fisica ed Astronomia, Università di Catania

Oral presentation Nuclear Astrophysics Nuclear Astrophysics

Speaker

Livio Lamia (INFN-LNS, Catania, Italy)

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In the framework of stellar nucleosynthesis and models, the combined study of the light elements (i.e. lithium, beryllium and boron) abundances in stellar atmospheres gives an unique opportunity for understanding stellar structure because of their different fragility against (p,alpha) reactions. This implies different stellar depths at which they are gradually destroyed, thus the residual atmospheric abundances will reflect the effect of plasma mixing. Being these reactions ignited at temperatures of few millions of Kelvin, experimental nuclear astrophysics has to use often extrapolation
procedures to access the relevant Gamow energy peak. Thus, the developments
of indirect techniques allowed the experimentalist to by pass such difficulties and, among them,
the Trojan Horse Method (THM) has been largely applied for measuring the bare nucleus S(E)-factor
for astrophysically relevant reactions, without experiencing both Coulomb penetrability and electron
screening effects. THM allows one to extract the bare-nucleus cross-section of a charged-particle induced
reaction a(x,c)C at astrophysical energies free of Coulomb suppression, by properly selecting
the quasi-free (QF) contribution of an appropriate reaction a(A,cC)s, performed at energies well
above the Coulomb barrier. Here, the nucleus A has a dominant x-s cluster configuration, thus representing the so-called "TH-nucleus".
Here, in view of the recent TH measurements, the main destruction channel for the two lithium (6Li and 7Li) and boron (11B and 10B) will be discussed, giving large emphasis to their impact on astrophysical scenarios and to their measurement for probing electron screening effects.

Primary author

Livio Lamia (INFN-LNS, Catania, Italy)

Co-authors

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