<?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>0121-7488</journal-id>
<journal-title><![CDATA[Ciencia en Desarrollo]]></journal-title>
<abbrev-journal-title><![CDATA[Ciencia en Desarrollo]]></abbrev-journal-title>
<issn>0121-7488</issn>
<publisher>
<publisher-name><![CDATA[Universidad Pedagógica y Tecnológica de Colombia]]></publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id>S0121-74882019000100041</article-id>
<article-id pub-id-type="doi">10.19053/01217488.v10.n1.2019.8812</article-id>
<title-group>
<article-title xml:lang="es"><![CDATA[Modelo estadístico de la distribución de materia de los discos protoplanetarios]]></article-title>
<article-title xml:lang="en"><![CDATA[Statistical model of the distribution of matter of protoplanetary disks]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Poveda Tejada]]></surname>
<given-names><![CDATA[N.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Rodríguez Cuevas]]></surname>
<given-names><![CDATA[L.M.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Vera Villamizar]]></surname>
<given-names><![CDATA[N.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Universidad Pedagógica y Tecnológica de Colombia  ]]></institution>
<addr-line><![CDATA[ ]]></addr-line>
<country>Colombia</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>06</month>
<year>2019</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>06</month>
<year>2019</year>
</pub-date>
<volume>10</volume>
<numero>1</numero>
<fpage>41</fpage>
<lpage>48</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.co/scielo.php?script=sci_arttext&amp;pid=S0121-74882019000100041&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.co/scielo.php?script=sci_abstract&amp;pid=S0121-74882019000100041&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.co/scielo.php?script=sci_pdf&amp;pid=S0121-74882019000100041&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen En la mayoría de modelos de discos protoplanetarios se tiene una distribución continua de gas y polvo, con una dinámica que da origen a los planetas, los cuales en el proceso de formación, hacen surcos en el disco al capturar gravitacionalmente la materia existente a su alrededor. Los discos de transición son una clase de disco protoplanetario que se caracterizan por tener una gran cavidad libre de gas y polvo en su interior. En este artículo se propone un modelo estadístico basado en los discos de transición, el cual se extiende a los discos protoplanetarios. Con este modelo se pueden realizar simulaciones dinámicas de formación planetaria usando pocos parámetros. Se muestra el proceso seguido para simular el disco de transición DoAr44 y el disco protoplanetario Hl-Tauri. A diferencia de otros modelos, la formación de cuerpos planetarios es más rápida.]]></p></abstract>
<abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract In the majority of models, the protoplanetary disks have a continuous distribution of gas and dust, with a dynamics that gives origin to the planets, which in the process of formation, make grooves on the disk by gravitationally capturing the existing matter around them. Transition disks are a class of protoplanetary disk that has a large cavity free of gas and dust inside. In this paper we propose a statistical model based on transitional disks, which extends to protoplanetary disks. With this model you can perform dynamic simulations of planetary formation using few parameters. The process followed to simulate the transition disk DoAr44 and the protoplanetary disk Hl-Tauri is shown. Unlike other models, the formation of planetary bodies is faster.]]></p></abstract>
<kwd-group>
<kwd lng="es"><![CDATA[Discos de transición]]></kwd>
<kwd lng="es"><![CDATA[disco protoplanetario]]></kwd>
<kwd lng="es"><![CDATA[simulación de discos protoplanetarios]]></kwd>
<kwd lng="en"><![CDATA[Transition disks]]></kwd>
<kwd lng="en"><![CDATA[protoplanetary disk]]></kwd>
<kwd lng="en"><![CDATA[simulation of protoplanetary disks]]></kwd>
</kwd-group>
</article-meta>
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