<?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>S0185-11012024000200373</article-id>
<article-id pub-id-type="doi">10.22201/ia.01851101p.2024.60.02.15</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Recent update of gas-phase chemical reactions and molecular lines of TiO in cloudy]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Shaw]]></surname>
<given-names><![CDATA[Gargi]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Ferland]]></surname>
<given-names><![CDATA[Gary J.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Stancil]]></surname>
<given-names><![CDATA[Phillip]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Porter]]></surname>
<given-names><![CDATA[Ryan]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Tata Institute of Fundamental Research Department of Astronomy and Astrophysics ]]></institution>
<addr-line><![CDATA[ ]]></addr-line>
<country>India</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,University of Kentucky Physics &amp; Astronomy ]]></institution>
<addr-line><![CDATA[Lexington Kentucky]]></addr-line>
<country>USA</country>
</aff>
<aff id="Af3">
<institution><![CDATA[,University of Georgia Department of Physics and Astronomy and Center for Simulational Physics ]]></institution>
<addr-line><![CDATA[ Georgia]]></addr-line>
<country>USA</country>
</aff>
<aff id="Af4">
<institution><![CDATA[,Stellar Science  ]]></institution>
<addr-line><![CDATA[Albuquerque NM]]></addr-line>
<country>USA</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>373</fpage>
<lpage>379</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012024000200373&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012024000200373&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012024000200373&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract We present our current update on the gas-phase chemical reactions and spectral lines of TiO in the spectral synthesis code CLOUDY. For this purpose, we have added 229 Ti-related reactions in the chemical network. In addition, we consider 230 fine-structure energy levels, the corresponding 223 radiative transitions, and 444 collisional transitions with ortho and para H2, and predict 66 TiO lines. We perform spectroscopic simulations of TiO emission from the circumstellar region of the oxygen-rich red supergiant VY Canis Majoris to validate our update. Our model reproduces the observed TiO column density. This update is helpful in modeling dust-free astrophysical environments where Ti is in the gas phase and TiO can form.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen Presentamos nuestra actualización de las reacciones químicas en fase gaseosa y líneas espectrales de TiO en el código de síntesis espectral CLOUDY. Para ello, hemos añadido 229 reacciones relacionadas con el Ti en la red química. Además, consideramos 230 niveles de energía de estructura fina, las correspondientes 223 transiciones radiativas, y 444 transiciones colisionales con orto- y para- H2 y predecimos 66 líneas de TiO. Realizamos simulaciones espectroscópicas de la emisión de TiO de la región circunestelar de la supergigante roja rica en oxígeno VY Canis Majoris para validar nuestra actualización. Nuestro modelo reproduce la densidad de la columna de TiO observada. Esta actualización es útil para modelar entornos astrofísicos libres de polvo donde el Ti está en fase gaseosa y se puede formar TiO.]]></p></abstract>
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<kwd lng="en"><![CDATA[astrochemistry]]></kwd>
<kwd lng="en"><![CDATA[methods: numerical]]></kwd>
<kwd lng="en"><![CDATA[molecular data]]></kwd>
<kwd lng="en"><![CDATA[software: simulations]]></kwd>
</kwd-group>
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