<?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>2222-145X</journal-id>
<journal-title><![CDATA[Reportes científicos de la FACEN]]></journal-title>
<abbrev-journal-title><![CDATA[Rep. cient. FACEN]]></abbrev-journal-title>
<issn>2222-145X</issn>
<publisher>
<publisher-name><![CDATA[Facultad de Ciencias Exactas y Naturales]]></publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id>S2222-145X2025000200015</article-id>
<article-id pub-id-type="doi">10.18004/rcfacen.2025.16.2.015</article-id>
<title-group>
<article-title xml:lang="es"><![CDATA[Observación de la rotación diferencial del sol alrededor del mínimo del ciclo solar 24.]]></article-title>
<article-title xml:lang="en"><![CDATA[Observation of the differential rotation around the minimum of solar cycle 24.]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Gómez]]></surname>
<given-names><![CDATA[José María]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[González]]></surname>
<given-names><![CDATA[Carlos Daniel]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Universidad Nacional de Asunción Facultad Politécnica ]]></institution>
<addr-line><![CDATA[San Lorenzo ]]></addr-line>
<country>Paraguay</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Universidad Nacional de Asunción Facultad de Ciencias Exactas y Naturales ]]></institution>
<addr-line><![CDATA[San Lorenzo ]]></addr-line>
<country>Paraguay</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>12</month>
<year>2025</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>12</month>
<year>2025</year>
</pub-date>
<volume>16</volume>
<numero>2</numero>
<fpage>15</fpage>
<lpage>24</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://scielo.iics.una.py/scielo.php?script=sci_arttext&amp;pid=S2222-145X2025000200015&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://scielo.iics.una.py/scielo.php?script=sci_abstract&amp;pid=S2222-145X2025000200015&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://scielo.iics.una.py/scielo.php?script=sci_pdf&amp;pid=S2222-145X2025000200015&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen: El estudio de las manchas solares es de interés para la predicción de la actividad solar, esto permite la planificación de misiones espaciales, además, la rotación diferencial está conectada a fenómenos magnéticos y de convección, es decir, con el comportamiento del interior del sol. Mediante la utilización del registro de manchas solares del observatorio astronómico Prof. Alexis Troche Boggino de la FP-UNA en el periodo 2005- 2010, se ha obtenido la curva de rotación diferencial del sol mediante el método de mínimos cuadrados. Los parámetros de ajuste al modelo de rotación diferencial arrojaron una velocidad de rotación ecuatorial de A = 14,01 ± 0,09º/día y un gradiente latitudinal de B = -0,30 ± 1,10º/día. Se ha observado una disminución de la velocidad de rotación ecuatorial y del gradiente latitudinal alrededor del mínimo del ciclo solar 24 en relación al comportamiento alrededor del mínimo de los tres ciclos solares precedentes.]]></p></abstract>
<abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract: The study of sunspots is of interest for the prediction of solar activity, allowing the planning of space missions. In addition, the differential rotation is connected to magnetic and convection phenomena, that is, the behavior of the Sun's interior. Through the use of the sunspot record of the astronomical observatory Prof. Alexis Troche Boggino of the FP-UNA in the period 2005-2010, the Sun's differential rotation curve was obtained using the least squares method. The parameters fitting the differential rotation model yielded an equatorial rotation rate of A = 14,01 ± 0,09º/day and a latitudinal gradient of B = -0,30 ± 1,10º/day. A decrease in the equatorial rotation rate and the latitudinal gradient has been observed around the minimum of solar cycle 24 in relation to the behavior around the minima of the three preceding solar cycles.]]></p></abstract>
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<kwd lng="es"><![CDATA[Física Solar]]></kwd>
<kwd lng="es"><![CDATA[Rotación Diferencial del Sol]]></kwd>
<kwd lng="es"><![CDATA[Manchas Solares]]></kwd>
<kwd lng="en"><![CDATA[Solar Physics]]></kwd>
<kwd lng="en"><![CDATA[Solar Differential Rotation]]></kwd>
<kwd lng="en"><![CDATA[Sunspots]]></kwd>
</kwd-group>
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