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The analysis reveals that this target is a new detached eclipsing binary system with a <jats:italic>\u03b4<\/jats:italic> Scuti component, rather than a single <jats:italic>\u03b4<\/jats:italic> Scuti star as previously known. The frequency analysis of short-cadence data reveals 95 significant frequencies, most of which lie in a frequency range of 23\u221232 day<jats:sup>\u22121<\/jats:sup>. Among them, seven independent frequencies are detected in the typical frequency range of <jats:italic>\u03b4<\/jats:italic> Scuti stars, and they are identified as pressure modes. In addition, a possible large separation value of \u0394<jats:italic>\u03bd<\/jats:italic> = 36.5 \u00b1 0.1 <jats:italic>\u03bc<\/jats:italic>Hz is also detected with the Fourier transform (FT) and autocorrelation function (AC) analysis. The orbital frequency <jats:italic>f<\/jats:italic>\n                  <jats:sub>orb<\/jats:sub> (= 0.320008 day<jats:sup>\u22121<\/jats:sup>) and its harmonics are also detected directly in the frequency spectrum. The binary modelings derived from PHOEBE indicate that this binary system is in detached configurations with a mass ratio of <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <mml:math xmlns:mml=\"http:\/\/www.w3.org\/1998\/Math\/MathML\" overflow=\"scroll\">\n                        <mml:mi>q<\/mml:mi>\n                        <mml:mo>=<\/mml:mo>\n                        <mml:msubsup>\n                           <mml:mrow>\n                              <mml:mn>0.33<\/mml:mn>\n                           <\/mml:mrow>\n                           <mml:mrow>\n                              <mml:mo>\u2212<\/mml:mo>\n                              <mml:mn>0.04<\/mml:mn>\n                           <\/mml:mrow>\n                           <mml:mrow>\n                              <mml:mo>+<\/mml:mo>\n                              <mml:mn>0.06<\/mml:mn>\n                           <\/mml:mrow>\n                        <\/mml:msubsup>\n                     <\/mml:math>\n                  <\/jats:inline-formula>, an inclination angle of <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <mml:math xmlns:mml=\"http:\/\/www.w3.org\/1998\/Math\/MathML\" overflow=\"scroll\">\n                        <mml:msubsup>\n                           <mml:mrow>\n                              <mml:mn>40.19<\/mml:mn>\n                           <\/mml:mrow>\n                           <mml:mrow>\n                              <mml:mo>\u2212<\/mml:mo>\n                              <mml:mn>2.84<\/mml:mn>\n                           <\/mml:mrow>\n                           <mml:mrow>\n                              <mml:mo>+<\/mml:mo>\n                              <mml:mn>3.96<\/mml:mn>\n                           <\/mml:mrow>\n                        <\/mml:msubsup>\n                     <\/mml:math>\n                  <\/jats:inline-formula>\u200b\u200b\u200b\u200b\u200b\u00b0. The derived parameters and binary evolutionary model suggest that the primary star is an object on the verge of leaving the main sequence with a temperature of \u223c7600 K, while the secondary appears to be a cool component entering the giant branch with a temperature \u223c3100 K lower than the primary. Moreover, this system may have undergone a mass ratio reversal, where the more massive star is the gainer component and the less massive one is the donor star.<\/jats:p>","DOI":"10.3847\/1538-4357\/ad7841","type":"journal-article","created":{"date-parts":[[2024,10,31]],"date-time":"2024-10-31T11:40:07Z","timestamp":1730374807000},"page":"171","update-policy":"https:\/\/doi.org\/10.1088\/crossmark-policy","source":"Crossref","is-referenced-by-count":2,"title":["KIC 8840638: A Newly Discovered Eclipsing Binary with \u03b4 Scuti\u2013Type 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