<?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>S0185-11012025000100087</article-id>
<article-id pub-id-type="doi">10.22201/ia.01851101p.2025.61.01.06</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[The Effect of Opacity on Neutron Star Type I X-ray Burst Quenching]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Nava-Callejas]]></surname>
<given-names><![CDATA[Martín]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Cavecchi]]></surname>
<given-names><![CDATA[Yuri]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Page]]></surname>
<given-names><![CDATA[Dany]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Universidad Nacional Autónoma de México Instituto de Astronomia ]]></institution>
<addr-line><![CDATA[CDMX ]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Universitat Politècnica de Catalunya EEBE Departament de Fisíca]]></institution>
<addr-line><![CDATA[Barcelona ]]></addr-line>
<country>Spain</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2025</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2025</year>
</pub-date>
<volume>61</volume>
<numero>1</numero>
<fpage>87</fpage>
<lpage>97</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012025000100087&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012025000100087&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012025000100087&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract One long standing tension between theory and observations of Type I X-ray bursts is the accretion rate at which the bursts disappear due to stabilization of the nuclear burning that powers them. This is observed to happen at roughly one third of the theoretical expectations. Various solutions have been proposed, the most notable of which is the addition of a yet unknown source of heat in the upper layers of the crust, below the burning envelope. In this paper we ran several simulations using the 1D code MESA to explore the impact of opacity on the threshold mass accretion rate after which the bursts disappear, finding that a higher than expected opacity in the less dense layers near the surface has a stabilizing effect.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen Una tensión largamente persistente entre teoría y observaciones de estallidos de rayos-X Tipo I es la tasa de acreción a la cual los estallidos desaparecen debido a la estabilización del quemado nuclear que los origina. Se ha observado que esto ocurre aproximadamente a un tercio de las expectativas teóricas. Varias soluciones se han propuesto; la más notable ha sido la adición de una fuente de calor de origen desconocido en las capas más altas de la corteza, debajo de la envolvente en quemado. En este art culo corrimos varias simulaciones empleando el código 1D MESA para explorar el impacto de la opacidad en la tasa de acreción l mite arriba de la cual los estallidos desaparecen; encontramos que una opacidad más alta de lo esperado en las zonas menos densas cerca de la superficie tiene un efecto estabilizador.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[accretion, accretion discs]]></kwd>
<kwd lng="en"><![CDATA[stars: neutron]]></kwd>
<kwd lng="en"><![CDATA[X-rays: binaries]]></kwd>
<kwd lng="en"><![CDATA[X-rays: bursts]]></kwd>
</kwd-group>
</article-meta>
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