# Subthreshold resonances and resonances in the $R$-matrix method for binary reactions and in the Trojan Horse method

## TL;DR

This paper advances the $R$-matrix method for analyzing subthreshold resonances and resonances in binary reactions, and applies the Trojan Horse method to calculate astrophysical S-factors, with implications for nuclear astrophysics.

## Contribution

It formulates new relations between ANC and observable widths in the $R$-matrix framework and extends the Trojan Horse method to three-body resonant reactions.

## Key findings

- Derived equations relating ANC and resonance widths for wide and narrow resonances.
- Expressed Trojan Horse double differential cross section in terms of on-shell S-factor.
- Reanalyzed TH data for $^{13}{
m C}( ext{α},n)^{16}{
m O}$ considering three-body effects.

## Abstract

In this paper we discuss the $R$-matrix approach to treat the subthreshold resonances for the single-level and one channel, and for the single-level and two channel cases. In particular, the expression relating the ANC with the observable reduced width, when the subthreshold bound state is the only channel or coupled with an open channel, which is a resonance, is formulated. Since the ANC plays a very important role in nuclear astrophysics, these relations significantly enhance the power of the derived equations. We present the relationship between the resonance width and the ANC for the general case and consider two limiting cases: wide and narrow resonances. Different equations for the astrophysical S-factors in the $R$-matrix approach are presented. After that we discuss the Trojan Horse Method (THM) formalism. The developed equations are obtained using the surface-integral formalism and the generalized $R$-matrix approach for the three-body resonant reactions. It is shown how the Trojan Horse (TH) double differential cross section can be expressed in terms of the on-the-energy-shell astrophysical S-factor for the binary sub-reaction. Finally, we demonstrate how the THM can be used to calculate the astrophysical S-factor for the neutron generator $^{13}{\rm C}(\alpha,\,n)^{16}{\rm O}$ in low-mass AGB stars. At astrophysically relevant energies this astrophysical S-factor is controlled by the threshold level $1/2^{+}, E_{x}= 6356$ keV. Here, we reanalyzed recent TH data taking into account more accurately the three-body effects and using both assumptions that the threshold level is a subthreshold bound state or it is a resonance state.