<?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>S0185-11012019000200321</article-id>
<article-id pub-id-type="doi">10.22201/ia.01851101p.2019.55.02.17</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Chaos in growing bar models]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Caritá]]></surname>
<given-names><![CDATA[Lucas Antonio]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
<xref ref-type="aff" rid="Aaf"/>
<xref ref-type="aff" rid="A a"/>
<xref ref-type="aff" rid="A3"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Rodrigues]]></surname>
<given-names><![CDATA[Irapuan]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Puerari]]></surname>
<given-names><![CDATA[Ivânio]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Schiavo]]></surname>
<given-names><![CDATA[Luiz Eduardo Camargo Aranha]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
<xref ref-type="aff" rid="Aaf"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Instituto Federal de Educação, Ci&#519;ncia e Tecnologia de São Paulo  ]]></institution>
<addr-line><![CDATA[São José dos Campos ]]></addr-line>
<country>Brazil</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Universidade do Vale do Paraíba  ]]></institution>
<addr-line><![CDATA[São José dos Campos ]]></addr-line>
<country>Brazil</country>
</aff>
<aff id="Af3">
<institution><![CDATA[,Instituto Nacional de Astrofísica, Optica y Electrónicá  ]]></institution>
<addr-line><![CDATA[Puebla ]]></addr-line>
<country>México</country>
</aff>
<aff id="Af4">
<institution><![CDATA[,Universidade Estadual de Campinas  ]]></institution>
<addr-line><![CDATA[Campinas ]]></addr-line>
<country>Brazil</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2019</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2019</year>
</pub-date>
<volume>55</volume>
<numero>2</numero>
<fpage>321</fpage>
<lpage>335</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012019000200321&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012019000200321&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012019000200321&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[ABSTRACT This paper aims to verify the influence of the bar, its pattern speed (&#8486; b ) and its rate of growth on the stability of the orbits in gravitational potentials. We studied the nature of the orbits in potentials representing galaxies with growing bars, where a linear growth was assumed. In order to study the stability of the orbits we applied SALI. We studied six models in which the bar dimensions were fixed, but we varied their pattern speed and time of bar growth. We found that when the bar growth is faster, more chaos is generated and we also noted that the higher the &#8486; b , the greater its influence on the system dynamics. The initial positions of the orbits that became chaotic were located in a well-defined ring-like region, confined between the ILR and CR resonances. There was also an indication that the retrograde orbits, although much scarcer, are more conductive to chaos when they do exist.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[RESUMEN Este trabajo verifica la influencia de la barra, de su velocidad angular (&#8486; b ) y de su tasa de crecimiento en la estabilidad de las órbitas en potenciales gravitacionales. Estudiamos órbitas en potenciales representando galaxias con barras en crecimiento, asumiendo un crecimiento lineal. Para estudiar la estabilidad de las órbitas aplicamos SALI. Estudiamos seis modelos con dimensiones fijas de la barra, pero variamos la velocidad y el tiempo de crecimiento de la misma. Evidenciamos que cuando el crecimiento de la barra es más rápido, se genera más caos y también observamos que cuanto mayor es &#8486; b , mayor será su influencia en la dinámica del sistema. Las posiciones iniciales de las órbitas que se han vuelto caóticas quedan ubicadas en una región anular bien definida, confinada entre ILR y CR. Las órbitas retrógradas, aunque mucho más escasas, parecen ser más propicias al el caos.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[chaos]]></kwd>
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