  Understanding the explosion mechanism of a core-collapse supernova (CCSN) is
important to accurately model CCSN scenarios for different progenitor stars
using model-observation comparisons. The uncertainties of various nuclear
reaction rates relevant for CCSN scenarios strongly affect the accuracy of
these stellar models. Out of these reactions, the
$^{13}$N($\alpha$,$p$)$^{16}$O reaction has been found to affect various stages
of a CCSN at varying temperatures. This work presents the first direct
measurement of the $^{13}$N($\alpha$,$p$)$^{16}$O reaction performed using a
34.6 MeV beam of radioactive $^{13}$N ions and the active-target detector MUSIC
(MUlti-Sampling Ionization Chamber) at Argonne National Laboratory. The
resulting total $^{13}$N($\alpha$,$p$)$^{16}$O reaction cross sections from
this measurement in the center-of-mass energy range of 3.26 - 6.02 MeV are
presented and compared with calculations using the Hauser-Feshbach formalism.
Uncertainties in the reaction rate have been dramatically reduced at CCSN
temperatures.
