<?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>0016-7169</journal-id>
<journal-title><![CDATA[Geofísica internacional]]></journal-title>
<abbrev-journal-title><![CDATA[Geofís. Intl]]></abbrev-journal-title>
<issn>0016-7169</issn>
<publisher>
<publisher-name><![CDATA[Universidad Nacional Autónoma de México, Instituto de Geofísica]]></publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id>S0016-71692016000200155</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Relationship between the minima of the horizontal magnetic component measured in Mexico and the Dst and SYM-H indices for geomagnetic storms with Dst&#8804; -100nT during the descending phase of solar cycle 23]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Martínez-Bretón]]></surname>
<given-names><![CDATA[Julia Lénica]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Mendoza Ortega]]></surname>
<given-names><![CDATA[Blanca]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Hernández-Quintero]]></surname>
<given-names><![CDATA[Esteban]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="A01">
<institution><![CDATA[,Universidad Nacional Autónoma de México Posgrado en Ciencias de la Tierra ]]></institution>
<addr-line><![CDATA[México D.F.]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="A02">
<institution><![CDATA[,Universidad Nacional Autónoma de México Instituto de Geofísica ]]></institution>
<addr-line><![CDATA[México D.F.]]></addr-line>
<country>Mexico</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>06</month>
<year>2016</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>06</month>
<year>2016</year>
</pub-date>
<volume>55</volume>
<numero>2</numero>
<fpage>155</fpage>
<lpage>164</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0016-71692016000200155&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0016-71692016000200155&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0016-71692016000200155&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract In this paper, we analyze the time delay between the occurrence of the minima in the geomagnetic Dst, SYM-H indices and the horizontal magnetic component (H) measured in the Teoloyucan Magnetic Observatory (TEO) of Mexico. This difference was calculated in Universal Time for 15 geomagnetic storms (Dst&#8804;-100nT) occurred during the descending phase of solar cycle 23. We found that, when the TEO was at the dayside, dawn and dusk, the time difference was negative, indicating that the minimum appeared first in the Dst, SYM-H reported by Kyoto, and afterwards in the H reported by TEO. On the other hand, when the TEO was close to midnight the difference was positive, indicating that the minimum occurred first at TEO and afterwards in Dst. We noticed that 14 out of 15 geomagnetic storms followed this behavior, except the most intense one of the sample. For the rest of the storms, it seems that the cause of the delay is not the intensity of the magnetic field at minimum but the intensity of the current systems present during the storm occurrences.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen En este trabajo se analizan las diferencias en aparición de mínimos entre los índices Dst, SYM-H y la componente horizontal H medida en el Observatorio Magnético Teoloyucan (TEO) ubicado en México. Se calculó esta diferencia en tiempo universal para 15 tormentas geomagnéticas (Dst&#8804;-100nT) que ocurrieron durante la fase descendente del ciclo solar 23. Notamos que cuando TEO se encontraba en el lado día, amanecer y atardecer, la diferencia horaria fue negativa, indicado que el mínimo apareció por primera vez en el Dst y SYM-H reportado por Kyoto y después en H medido por TEO. Por otra parte, cuando TEO se encontraba cercano a la medianoche la diferencia es positiva, lo que indica que el mínimo se reportó antes en TEO y después en Dst. Notamos que 14 de las 15 tormentas geomagnéticas siguieron este comportamiento, excepto la más intensa de la muestra. Para las 14 restantes el tiempo de desfasamiento en los mínimos no parece depender de la intensidad de la tormenta geomagnética, sino de la intensidad de los sistemas de corrientes presentes.]]></p></abstract>
<kwd-group>
<kwd lng="es"><![CDATA[corrientes de la Ionosfera]]></kwd>
<kwd lng="es"><![CDATA[DST]]></kwd>
<kwd lng="es"><![CDATA[SYM-H]]></kwd>
<kwd lng="es"><![CDATA[tormentas geomagnéticas intensas]]></kwd>
<kwd lng="es"><![CDATA[relaciones solar-terrestres]]></kwd>
<kwd lng="en"><![CDATA[ionosphere currents]]></kwd>
<kwd lng="en"><![CDATA[Dst]]></kwd>
<kwd lng="en"><![CDATA[SYM-H]]></kwd>
<kwd lng="en"><![CDATA[intense geomagnetic storms]]></kwd>
<kwd lng="en"><![CDATA[solar-terrestrial relations]]></kwd>
</kwd-group>
</article-meta>
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