<?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>S0185-11012020000200287</article-id>
<article-id pub-id-type="doi">10.22201/ia.01851101p.2020.56.02.10</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Analysis of a short periodic pulsator: SX phoenicis star XX Cyg]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Abdel-Sabour]]></surname>
<given-names><![CDATA[Mohamed]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Shokry]]></surname>
<given-names><![CDATA[Ahmed]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Ibrahim]]></surname>
<given-names><![CDATA[Ahmed]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
<xref ref-type="aff" rid="Aaf"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,National Research Institute of Astronomy and Geophysics  ]]></institution>
<addr-line><![CDATA[Cairo ]]></addr-line>
<country>Egypt</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Al-Azhar University Faculty of Science Dept. of Astronomy and Meteorology]]></institution>
<addr-line><![CDATA[Cairo ]]></addr-line>
<country>Egypt</country>
</aff>
<aff id="Af3">
<institution><![CDATA[,King Saud University Coll. Sci Dept. Phys &amp; Astron]]></institution>
<addr-line><![CDATA[ ]]></addr-line>
<country>Saudi Arabia</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2020</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2020</year>
</pub-date>
<volume>56</volume>
<numero>2</numero>
<fpage>287</fpage>
<lpage>294</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012020000200287&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012020000200287&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012020000200287&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[ABSTRACT Photometric observations were made of the SX Phoenicis star XX Cyg between September and October 2019, using the 1.88-m Kottamia reflector telescope in Egypt. We used 340 CCD observations with blue-visible-red (BVR) filters to derive light curves. In addition, we obtained 9540 visual magnitudes for XX Cyg from the literature to prepare an observed-minus-calculated (O-C) diagram. 85 new times of maximum for XX Cyg are presented. We did not detect a bump in the descending portion of the light curve of maximum light for XX Cyg. However, we did detect a secular bump in the phased light curves, which changes with phase in some SuperWASP observations. We found the change in period of XX Cyg to be dP/dt = 15.5×10&#8722;5 s/yr, with its amplitude decreasing at a rate of 0.7 mmag/year. Stellar parameters of XX Cyg and its position in the instability strip of the Hertzsprung Russell stellar evolution diagram are presented.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[RESUMEN Se realizaron observaciones fotométricas de la estrella tipo SX Phoenicis XX Cyg entre septiembre y octubre de 2019 con el telescopio de 1.88 m Kottamia, en Egipto. Mediante 340 observaciones con CCD en los filtros BVR derivamos curvas de luz. También obtuvimos 9540 magnitudes visuales para XX Cyg de la literatura, para preparar un diagrama O-C. Presentamos 85 nuevos tiempos del máximo para XX Cyg. No detectamos una protuberancia en la parte descendiente del máximo de la curva de luz de XX Cyg. Sin embargo, encontramos una protuberancia secular en las curvas de luz en fase, la cual cambia con la fase en algunas observaciones del SuperWASP. Encontramos que el cambio del período de XX Cyg es dP/dt = 15.5×10&#8722;5 s/yr, y que la amplitud decrece a una tasa de 0.7 mmag/year. Presentamos los parámetros estelares y el estado evolutivo de XX Cyg, que se encuentra en la franja de inestabilidad del diagrama de Hertzsprung Russell.]]></p></abstract>
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