<?xml version="1.0" encoding="ISO-8859-1"?><article xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance">
<front>
<journal-meta>
<journal-id>0185-1101</journal-id>
<journal-title><![CDATA[Revista mexicana de astronomía y astrofísica]]></journal-title>
<abbrev-journal-title><![CDATA[Rev. mex. astron. astrofis]]></abbrev-journal-title>
<issn>0185-1101</issn>
<publisher>
<publisher-name><![CDATA[Universidad Nacional Autónoma de México, Instituto de Astronomía]]></publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id>S0185-11012024000200205</article-id>
<article-id pub-id-type="doi">10.22201/ia.01851101p.2024.60.02.01</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Light and frequency analysis of detached eccentric binary system DT CAM with pre-main sequence component]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Ozdemir]]></surname>
<given-names><![CDATA[Tuncay]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Gürol]]></surname>
<given-names><![CDATA[Birol]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,&#304;nönü University Faculty of Arts and Sciences Department of Physics]]></institution>
<addr-line><![CDATA[Malatya ]]></addr-line>
<country>Turkey</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Ankara University Department of Astronomy and Space Sciences ]]></institution>
<addr-line><![CDATA[Tando&#287;an Ankara]]></addr-line>
<country>Turkey</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2024</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2024</year>
</pub-date>
<volume>60</volume>
<numero>2</numero>
<fpage>205</fpage>
<lpage>216</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012024000200205&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012024000200205&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012024000200205&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract In this study we analyzed TESS data of detached eccentric binary system DT Cam and we obtained the first physical parameters of the components. We found that the out-of-eclipse variation of the system shows a small amplitude periodic feature. Most of the frequencies obtained are related with the orbital variation except one, for which the period was determined as &#8776;0.605 days. The masses and radii of the primary and secondary components were calculated as M 1 = 1.793M &#8857;, M 2 = 1.414M &#8857;, R 1 = 1.355R &#8857;, and R 2 = 1.522R &#8857;, respectively. Considering the physical properties of the primary component we concluded that it is a rotational variable. We found that the massive component is smaller than the low-mass component. It seems that the secondary component is a pre-main sequence star, which is important for the understanding of stellar structure and evolution.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen Se analizan datos de TESS sobre la binaria excéntrica DT Cam y se obtienen por primera vez los parámetros físicos de las componentes. Encontramos una variación periódica de pequeña amplitud fuera de eclipse. Muchas de las frecuencias obtenidas se relacionan con la variación orbital, excepto una, cuyo período se determinó como &#8776;0.605 días. Se calculan las masas y radios de las componentes primaria y secundaria, y se obtienen como resultados M 1 = 1.793M &#8857;, M 2 = 1.414M &#8857;, R 1 = 1.355R &#8857;, y R 2 = 1.522R &#8857;. Dadas las propiedades físicas de la primaria concluimos que es un variable rotacional. Encontramos que la componente masiva es más pequeña que la compañera de baja masa. Al parecer, la secundaria es una estrella pre-secuencia principal, lo cual es importante para entender la estructura y evolución estelares.]]></p></abstract>
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<kwd lng="en"><![CDATA[binaries: eclipsing]]></kwd>
<kwd lng="en"><![CDATA[stars: fundamental parameters]]></kwd>
<kwd lng="en"><![CDATA[stars: individual: DT Cam - stars: rotation]]></kwd>
<kwd lng="en"><![CDATA[techniques: photometric]]></kwd>
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</article-meta>
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