<?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>S0185-11012018000200317</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Numerical simulation of the HH 30 astrophysical jet near its launch site]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Gardner]]></surname>
<given-names><![CDATA[Carl L.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Jones]]></surname>
<given-names><![CDATA[Jeremiah R.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Vargas]]></surname>
<given-names><![CDATA[Perry B.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Arizona State University School of Mathematical &amp; Statistical Sciences ]]></institution>
<addr-line><![CDATA[Tempe AZ]]></addr-line>
<country>USA</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2018</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2018</year>
</pub-date>
<volume>54</volume>
<numero>2</numero>
<fpage>317</fpage>
<lpage>323</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012018000200317&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012018000200317&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012018000200317&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract We simulate the surface brightness of the HH 30 astrophysical jet near its launch site in the forbidden [O I], [N II], and [S II] doublets by post-processing gas dynamical simulations of densities and temperatures, using spectral line emission data from the astrophysical spectral synthesis package Cloudy. We then compare the simulated surface brightness in each line with Hubble Space Telescope observations of Hartigan and Morse and with multiple-ion magnetohydrodynamic simulations of Tesileanu et al. The general trend of our simulated surface brightness in each doublet using the gas dynamical/Cloudy approach is in excellent agreement with the observational data, verifying our choices of initial jet and ambient densities and jet temperature, as well as the number and sequencing of the jet pulses over the 35 year evolution of the jet near its launch site.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen Simulamos el brillo superficial en los dobletes prohibidos [O I], [N II], y [S II] del chorro astrofísico HH 30 cerca del sitio de su lanzamiento mediante el post proceso de simulaciones de dinámica de gas de las densidades y las temperaturas, usando datos sobre la emisión espectral en líneas del paquete de síntesis espectral astrofísica Cloudy. Comparamos los brillos superficiales simulados en cada línea con las observaciones de Hartigan y Morse usando el Hubble Space Telescope y con las simulaciones magneto hidrodinámicas de iones múltiples de Tesileanu et al. La tendencia general de nuestros brillos superficiales simulados en cada doblete usando el enfoque de dinámica de gases Cloudy concuerda muy bien con los datos observacionales, y confirma los valores que elegimos para las densidades iniciales del chorro y del medio ambiente, así como del número y la secuencia de pulsos del chorro cerca del sitio de su lanzamiento, a lo largo de 35 años de evolución.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[ISM: jets and outflows]]></kwd>
<kwd lng="en"><![CDATA[Herbig-Haro objects]]></kwd>
</kwd-group>
</article-meta>
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