<?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>0187-6236</journal-id>
<journal-title><![CDATA[Atmósfera]]></journal-title>
<abbrev-journal-title><![CDATA[Atmósfera]]></abbrev-journal-title>
<issn>0187-6236</issn>
<publisher>
<publisher-name><![CDATA[Universidad Nacional Autónoma de México, Instituto de Ciencias de la Atmósfera y Cambio Climático]]></publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id>S0187-62362026000100107</article-id>
<article-id pub-id-type="doi">10.20937/atm.53524</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Superrotation of the Venus&#8217; atmosphere computed with a thermodynamic model]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Mendoza]]></surname>
<given-names><![CDATA[Víctor M.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Mendoza]]></surname>
<given-names><![CDATA[Blanca]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Pazos]]></surname>
<given-names><![CDATA[Marni]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Quintanar]]></surname>
<given-names><![CDATA[Arturo I.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Garduño]]></surname>
<given-names><![CDATA[René]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Universidad Nacional Autónoma de México Instituto de Ciencias de la Atmósfera y Cambio Climático ]]></institution>
<addr-line><![CDATA[Ciudad de México ]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Universidad Nacional Autónoma de México Instituto de Geofísica, Unidad Michoacán ]]></institution>
<addr-line><![CDATA[Morelia Michoacán]]></addr-line>
<country>Mexico</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2026</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2026</year>
</pub-date>
<volume>40</volume>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0187-62362026000100107&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0187-62362026000100107&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0187-62362026000100107&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[ABSTRACT A thermodynamic model is developed in which the dynamics of Venusian atmospheric superrotation is subordinated to thermal forcing. The key mechanism is a diurnal thermal tide, generated by simplified heating based on radiative balance between solar insolation and long-wave emission. This heating produces horizontal temperature gradients (day-night and equator-pole), which, through hydrostatic equilibrium, translate into geopotential gradients. These gradients act as the primary force in the equations of motion, increasing specific angular momentum with altitude and generating a superrotating zonal wind in the direction of planetary rotation, but opposed to the slow propagation of the thermal tide. Numerical integration across 24 tropospheric layers, coupled with a regolith thermal conductivity model (down to 19.1 m depth) to compute surface heat flux, demonstrates that thermally induced vertical circulation transports angular momentum from the surface to the cloud level. It is concluded that the diurnal thermal tide, driven by insolation gradients, is the fundamental mechanism generating and maintaining superrotation in Venus&#8217; atmosphere. This novel thermodynamic approach provides a unified framework for understanding this phenomenon on slowly rotating planets.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[RESUMEN Se desarrolló un modelo termodinámico que subordina la dinámica de la superrotación atmosférica de Venus a los forzamientos térmicos. El mecanismo clave es una marea térmica diurna, generada por un calentamiento simplificado basado en el equilibrio radiativo entre la insolación solar y la emisión de onda larga. Este calentamiento produce gradientes horizontales de temperatura (día-noche y ecuador-polo) que, a través del equilibrio hidrostático, se traducen en gradientes de geopotencial. Dichos gradientes actúan como la fuerza principal en las ecuaciones de movimiento, incrementando el momento angular específico con la altitud y generando un viento zonal superrotante en la dirección de la rotación planetaria, pero opuesto a la lenta propagación de la marea térmica. La integración numérica en 24 capas troposféricas, junto con un modelo de conductividad térmica del regolito (hasta 19.1 m de profundidad) para calcular el flujo de calor superficial, muestra que la circulación vertical inducida térmicamente transporta el momento angular desde la superficie hacia el nivel de las nubes. Se concluye que la marea térmica diurna, impulsada por los gradientes de insolación, es el mecanismo fundamental que genera y mantiene la superrotación en la atmósfera de Venus. Este enfoque termodinámico novedoso proporciona un marco unificado para comprender este fenómeno en planetas de rotación lenta.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[Venus&#8217; atmosphere]]></kwd>
<kwd lng="en"><![CDATA[planetary atmospheres]]></kwd>
<kwd lng="en"><![CDATA[Venus&#8217; superrotation]]></kwd>
</kwd-group>
</article-meta>
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