<?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>S0185-11012016000200339</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[ROTSE1 J164341.65+251748.1: A new W UMa-type eclipsing binary]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Michel]]></surname>
<given-names><![CDATA[R.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Echevarría]]></surname>
<given-names><![CDATA[J.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Cang]]></surname>
<given-names><![CDATA[T.Q.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Fox-Machado]]></surname>
<given-names><![CDATA[L.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[González-Buitrago]]></surname>
<given-names><![CDATA[D.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Universidad Nacional Autónoma de México Instituto de Astronomía ]]></institution>
<addr-line><![CDATA[Ensenada Baja California]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Universidad Nacional Autónoma de México Instituto de Astronomía ]]></institution>
<addr-line><![CDATA[ Ciudad de México]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="Af3">
<institution><![CDATA[,Beijing Normal University Department of Astronomy ]]></institution>
<addr-line><![CDATA[Beijing ]]></addr-line>
<country>China</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2016</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2016</year>
</pub-date>
<volume>52</volume>
<numero>2</numero>
<fpage>339</fpage>
<lpage>345</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012016000200339&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012016000200339&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012016000200339&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract: ROTSE1 J164341.65+251748.1 was photometrically observed in the V band during three epochs with the 0.84-m telescope of the San Pedro Mártir Observatory in Mexico. Based on additional BVR photometry, we found that the primary star has a spectral type around G0V. The light curve of the system is typical of a W UMa type binary stars and has an orbital period of &#8776; 0.323 days. In an effort to gain a better understanding of the binary system and determine its physical properties, we analyzed the light curve with the Wilson and Devinney method. We found that ROTSE1 J164341.65+251748.1 has a mass ratio of &#8776; 0.34 and that the less massive component is about 230 K hotter than the primary star. The inclination of the system is &#8776; 84.6 degrees, and the degree of over-contact is 11%. The analysis shows the presence of variable bright spots on the primary star.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen: ROTSE1 J164341.65+251748.1 fue observada fotométricamente en la banda V durante tres épocas con el telescopio de 0.84-m del Observatorio de San Pedro Mártir en México. Con base en fotometría BVR adicional, encontramos que la estrella primaria tiene un tipo espectral cercano a G0V. La curva del luz del sistema es característica de los sistemas binarios del tipo W UMa y tiene un periodo orbital de &#8776; 0.323 días. Con el propósito de entender mejor a este sistema binario, hemos analizado su curva de luz con ayuda del método de Wilson y Devinney. Hemos encontrado que ROTSE1 J164341.65+251748.1 tiene una razón de masas de &#8776; 0.34 y que la componente menos masiva es &#8776; 230 K más caliente que la estrella primaria. La inclinación del sistema es &#8776; 84.6 grados y el sobre-contacto es de 11%. El análisis también mostró la presencia de manchas brillantes variables sobre la estrella primaria.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[binaries: eclipsing]]></kwd>
<kwd lng="en"><![CDATA[techniques: photometric]]></kwd>
<kwd lng="en"><![CDATA[stars: individual (ROTSE1 J164341.65+251748.1)]]></kwd>
</kwd-group>
</article-meta>
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