<?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>1909-3667</journal-id>
<journal-title><![CDATA[Tecciencia]]></journal-title>
<abbrev-journal-title><![CDATA[Tecciencia]]></abbrev-journal-title>
<issn>1909-3667</issn>
<publisher>
<publisher-name><![CDATA[Universidad ECCI]]></publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id>S1909-36672018000100053</article-id>
<article-id pub-id-type="doi">10.18180/tecciencia.2018.24.6</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Bifurcation in the Tidal Streams of Sagittarius: Numerical Simulations]]></article-title>
<article-title xml:lang="es"><![CDATA[Bifurcación en las Corrientes de Marea de Sagitario: Simulaciones Numéricas]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Camargo Camargo]]></surname>
<given-names><![CDATA[Yeimy]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
<xref ref-type="aff" rid="Aaf"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Casas-Miranda]]></surname>
<given-names><![CDATA[Rigoberto A.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Universidad de Cundinamarca  ]]></institution>
<addr-line><![CDATA[Facatativá ]]></addr-line>
<country>Colombia</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Universidad Nacional de Colombia  ]]></institution>
<addr-line><![CDATA[Bogotá ]]></addr-line>
<country>Colombia</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>06</month>
<year>2018</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>06</month>
<year>2018</year>
</pub-date>
<volume>13</volume>
<numero>24</numero>
<fpage>53</fpage>
<lpage>62</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.co/scielo.php?script=sci_arttext&amp;pid=S1909-36672018000100053&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.co/scielo.php?script=sci_abstract&amp;pid=S1909-36672018000100053&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.co/scielo.php?script=sci_pdf&amp;pid=S1909-36672018000100053&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract N-body simulations of the interaction between the Sagittarius dwarf galaxy and the Milky Way are performed to study whether it is possible to reproduce both the bifurcations in the tidal streams and the physical properties of Sagittarius. Both galaxies are simulated as sets of particles (live potentials). The initial structures are formed using GALIC and the gravitational interaction between these galaxies is simulated with GADGET-2. Sagittarius initially is simulated as a rotating disk-type galaxy with two components: dark matter halo and stellar disk and the Milky Way is a disk galaxy with three components: dark matter halo, stellar disk and central spheroid. Several numerical simulations of the interaction of this galaxy with the Milky Way with angles between the orbital angular momentum and the disc angular momentum in the range 180° &#8804;&#952; &#8804; 0° were performed, showing that, although the position and physical properties of Sagittarius are not reproduced entirely by the remnant, the bifurcations appear clearly when 180° &#8804;&#952; &lt; 90°.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen Se realizan simulaciones de N-cuerpos de la interacción entre la galaxia enana Sagitario y la Vía Láctea para estudiar si es posible reproducir tanto las bifurcaciones en las corrientes de marea como las propiedades físicas de Sagitario. Ambas galaxias son simuladas como conjuntos de partículas (potencial vivo). Las estructuras iniciales son conformadas en GALIC y la interacción gravitacional entre estas galaxias es simulada con GADGET-2. Sagitario inicialmente es una galaxia de tipo disco rotante con dos componentes: Halo de materia oscura y disco estelar y la Vía Láctea como es usual, es una galaxia de disco con tres componentes: halo de materia oscura, disco estelar y esferoide. Se realizan varias simulaciones de la interacción del progenitor de esta galaxia enana con la Vía Láctea, donde el ángulo entre el momento angular orbital y el momento angular del disco es 180° &#8804; &#952; &#8804; 0° mostrando que aunque no se reproducen en su totalidad la posición y propiedades físicas del remanente de Sagitario, las bifurcaciones aparecen de modo evidente cuando 180° &#8804;&#952; &#8804; 90°.]]></p></abstract>
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<kwd lng="en"><![CDATA[Galaxy: evolution]]></kwd>
<kwd lng="en"><![CDATA[Galaxy: formation]]></kwd>
<kwd lng="en"><![CDATA[Galaxies: individual (Sagittarius dSph)]]></kwd>
<kwd lng="es"><![CDATA[Galaxia: evolución]]></kwd>
<kwd lng="es"><![CDATA[Galaxia: formación]]></kwd>
<kwd lng="es"><![CDATA[Galaxias: individual (enana Sagitario)]]></kwd>
</kwd-group>
</article-meta>
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