<?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>S0185-11012024000200361</article-id>
<article-id pub-id-type="doi">10.22201/ia.01851101p.2024.60.02.13</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Alp-photon interaction in the stellar environment]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Chaubey]]></surname>
<given-names><![CDATA[Ankur]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Ganguly]]></surname>
<given-names><![CDATA[Avijit K.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Awdhoot Bhagwan Ram PG. College  ]]></institution>
<addr-line><![CDATA[Anpara Sonebhadra]]></addr-line>
<country>India</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Banaras Hindu University Institute of Science Department of Physics]]></institution>
<addr-line><![CDATA[ ]]></addr-line>
<country>India</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2024</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2024</year>
</pub-date>
<volume>60</volume>
<numero>2</numero>
<fpage>361</fpage>
<lpage>365</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012024000200361&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012024000200361&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012024000200361&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract The spin zero, very light bosons, like the pseudoscalar axion, are collectively grouped into the term axion-like particle (ALP). These elusive particles qualify as candidates for dark matter. ALPs also show their presence in higher dimensional theories, as K.K. particles in Kaluza Klein theory, moduli in string theory and chameleons in cosmology. They can interact with the photon via dimension-five coupling. In this text we provide an alternative method for investigating the signatures of the dark matter candidate particles (i.e., ALP) by estimating the expressions of the probabilities of conversion between di&#64256;erent degrees of freedom of interacting photons into ALP and into each other in presence of a stellar magnetized background. We have also tried to explain the contribution of pseudoscalar ALP-photon mixing to the luminosity function of stars like red giants, supergiants, white dwarfs, etc.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen Los bosones ligeros de espín cero, como el axión seudoescalar, se agrupan con el término &#8220;partículas similares al axión (ALP)&#8221;. Estas partículas son candidatos para explicar la materia oscura. Los ALP muestran su presencia en teorías de muchas dimensiones, como partículas K.K. en la teoría de Kaluza-Klein, como módulos en la teoría de cuerdas o como camaleones en cosmología. Pueden interactuar con los fotones mediante un acoplamiento de dimensión 5. Presentamos un método alternativo para investigar las señales de los ALP como candidatos a materia oscura, estimando las expresiones para la probabilidad de conversión entre varios grados de libertad de un fotón en interacción con un ALP o de fotones entre sí, en presencia de un fondo interestelar magnetizado. Intentamos explicar la contribución de la mezcla seudoescalar ALP-fotón a la función de luminosidad de las gigantes rojas, supergigantes, o enanas blancas.]]></p></abstract>
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<kwd lng="en"><![CDATA[galaxies: photometry]]></kwd>
<kwd lng="en"><![CDATA[methods: numerical]]></kwd>
<kwd lng="en"><![CDATA[white dwarfs]]></kwd>
</kwd-group>
</article-meta>
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