Neutron captures and delayed decays of reaction products are common sources of backgrounds in ultra-rare event searches. In this work, we studied $^{13}$C($\alpha,n)^{16}$O reactions induced by $\alpha$-particles emitted within the calibration sources of the \textsc{Majorana Demonstrator}. These sources are thorium-based calibration standards enclosed in carbon-rich materials. The reaction rate was estimated by using the 6129-keV $\gamma$-rays emitted from the excited $^{16}$O states that are populated when the incoming $\alpha$-particles exceed the reaction Q-value. Thanks to the excellent energy performance of the \textsc{Demonstrator}'s germanium detectors, these characteristic photons can be clearly observed in the calibration data. Fac...
Low-mass asymptotic giant branch stars are among the most important polluters of the interstellar me...
Cross sections for the reaction 12C(α,γ)16O have been measured for a range of center-of-mass alpha p...
The beta-delayed neutron emission probability, P-n, of very neutron-rich nuclei allows us to achieve...
Neutron captures and delayed decays of reaction products are common sources of backgrounds in ultrar...
The 13C (α ,n )16O reaction is the main neutron source for the slow-neutron-capture process in asymp...
The $^{13}$C($\alpha$,$n$)$^{16}$O reaction is the main neutron source for the slow-neutron-capture ...
It has been recently suggested that hydrogen ingestion into the helium shell of massive stars could ...
The C-12(alpha,gamma)O-16 reaction plays a central role in astrophysics, but its cross section at en...
Background: The. process in core-collapse supernova explosions is thought to explain the origin of p...
Described in this thesis are measurements made of the thick-target neutron yield from the reaction 1...
Background: It has been recently suggested that hydrogen ingestion into the helium shell of massive ...
The C-12(alpha,gamma)O-16 reaction plays a central role in astrophysics, but its cross section at en...
13C(α,n)16O是渐进巨星支(AGB)星中慢速中子俘获(s)过程的主中子源反应,而17O 6.356 MeV 1/2+阈下共振对13 C(α,n)16 O反应影响很大。本文使用 HI-13串列加...
The 13 C(α, n)16 O reaction determines the dominant neutron source of the sprocess in thermally puls...
The 13 C(α,n)16 O reaction is the prevalent neutron source for the main s-process. The direct measur...
Low-mass asymptotic giant branch stars are among the most important polluters of the interstellar me...
Cross sections for the reaction 12C(α,γ)16O have been measured for a range of center-of-mass alpha p...
The beta-delayed neutron emission probability, P-n, of very neutron-rich nuclei allows us to achieve...
Neutron captures and delayed decays of reaction products are common sources of backgrounds in ultrar...
The 13C (α ,n )16O reaction is the main neutron source for the slow-neutron-capture process in asymp...
The $^{13}$C($\alpha$,$n$)$^{16}$O reaction is the main neutron source for the slow-neutron-capture ...
It has been recently suggested that hydrogen ingestion into the helium shell of massive stars could ...
The C-12(alpha,gamma)O-16 reaction plays a central role in astrophysics, but its cross section at en...
Background: The. process in core-collapse supernova explosions is thought to explain the origin of p...
Described in this thesis are measurements made of the thick-target neutron yield from the reaction 1...
Background: It has been recently suggested that hydrogen ingestion into the helium shell of massive ...
The C-12(alpha,gamma)O-16 reaction plays a central role in astrophysics, but its cross section at en...
13C(α,n)16O是渐进巨星支(AGB)星中慢速中子俘获(s)过程的主中子源反应,而17O 6.356 MeV 1/2+阈下共振对13 C(α,n)16 O反应影响很大。本文使用 HI-13串列加...
The 13 C(α, n)16 O reaction determines the dominant neutron source of the sprocess in thermally puls...
The 13 C(α,n)16 O reaction is the prevalent neutron source for the main s-process. The direct measur...
Low-mass asymptotic giant branch stars are among the most important polluters of the interstellar me...
Cross sections for the reaction 12C(α,γ)16O have been measured for a range of center-of-mass alpha p...
The beta-delayed neutron emission probability, P-n, of very neutron-rich nuclei allows us to achieve...