<?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>0035-001X</journal-id>
<journal-title><![CDATA[Revista mexicana de física]]></journal-title>
<abbrev-journal-title><![CDATA[Rev. mex. fis.]]></abbrev-journal-title>
<issn>0035-001X</issn>
<publisher>
<publisher-name><![CDATA[Sociedad Mexicana de Física]]></publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id>S0035-001X2006000900068</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Propagation of linear MHD waves in a hydrogen plasma: the mode crossing problem]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Tremola]]></surname>
<given-names><![CDATA[C]]></given-names>
</name>
<xref ref-type="aff" rid="A01"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Sigalotti]]></surname>
<given-names><![CDATA[L. Di G]]></given-names>
</name>
<xref ref-type="aff" rid="A01"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Sira]]></surname>
<given-names><![CDATA[E]]></given-names>
</name>
<xref ref-type="aff" rid="A01"/>
</contrib>
</contrib-group>
<aff id="A01">
<institution><![CDATA[,Instituto Venezolano de Investigaciones Científicas Centro de Física ]]></institution>
<addr-line><![CDATA[Caracas ]]></addr-line>
<country>Venezuela</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>05</month>
<year>2006</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>05</month>
<year>2006</year>
</pub-date>
<volume>52</volume>
<fpage>233</fpage>
<lpage>235</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0035-001X2006000900068&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0035-001X2006000900068&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0035-001X2006000900068&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Here we use linear analysis to investigate the propagation of small thermal and magnetohydrodynamic (MHD) disturbances in a heat-conducting, ionizing-recombining, hydrogen plasma threaded by an external uniform magnetic field. Linearization of the governing MHD equations for this model leads to a dispersion equation for the wavenumber k as a function of the frequency &#969; which may be either quadratic or cubic in k², depending on the orientation of the magnetic field. In either case, the solution of the dispersion equation is such that crossing of the roots may happen at some frequencies, implying that they may not always correspond to the same particular physical wave. The crossing of modes is merely a mathematical property of the solution and must not be interpreted as an interchange of the thermal and MHD waves' physical nature at the crossing frequency. Here we find that mode crossing is a function of the wave frequency, plasma temperature, magnetic field strength and orientation.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Mediante un análisis lineal se estudia la propagación de perturbaciones térmicas y magnetohidrodinámicas (MHD) en un plasma de hidrógeno sujeto a la acción de un campo magnético externo de intensidad uniforme, incluyendo los efectos de conducción de calor, fotoionización y fotorecombinación. A partir de la linealización de las ecuaciones MHD para este modelo se obtiene una ecuación de dispersión para el número de onda k en funcion de la frecuencia &#969;, que puede ser cuadrática o cúbica en k² dependiendo de la orientación del campo magnético. En ambos casos, la solución de la ecuación de dispersión es tal que las raices pueden cruzarse a determinadas frecuencias. De este modo, las raices no siempre corresponderán a la misma onda para todo el espectro de frecuencias. El cruce de modos es una propiedad matemática de la solución y no debe interpretarse como un intercambio de la naturaleza física de las ondas. Se encuentra que el cruce de modos es una función de la frecuencia, de la temperatura del plasma y de la orientación e intensidad del campo magnético.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[Magnetohydrodynamics and plasmas]]></kwd>
<kwd lng="en"><![CDATA[magnetohydrodynamic waves]]></kwd>
<kwd lng="en"><![CDATA[sound waves]]></kwd>
<kwd lng="en"><![CDATA[wave propagation]]></kwd>
<kwd lng="es"><![CDATA[Magnetohidrodinámica y plasmas]]></kwd>
<kwd lng="es"><![CDATA[ondas magnetohidrodinámicas]]></kwd>
<kwd lng="es"><![CDATA[ondas acústicas]]></kwd>
<kwd lng="es"><![CDATA[propagación de ondas]]></kwd>
</kwd-group>
</article-meta>
</front><body><![CDATA[ <p align="justify"><font face="verdana" size="4">Plasmas</font></p>     <p align="justify"><font face="verdana" size="2">&nbsp;</font></p>     <p align="center"><font face="verdana" size="4"><b>Propagation of linear MHD waves in a hydrogen plasma: the mode crossing problem</b></font></p>     <p align="justify"><font face="verdana" size="2">&nbsp;</font></p>     <p align="center"><font face="verdana" size="2"><b>C. Tremola, L. Di G. Sigalotti, and E. Sira</b></font></p>     <p align="justify"><font face="verdana" size="2">&nbsp;</font></p>     <p align="justify"><font face="verdana" size="2"><i>Centro de F&iacute;sica, Instituto Venezolano de Investigaciones Cient&iacute;ficas, IVIC, Apartado 21827, Caracas 1020A, Venezuela.</i></font></p>     <p align="justify"><font face="verdana" size="2">&nbsp;</font></p>     <p align="justify"><font face="verdana" size="2">Recibido el 25 de noviembre de 2003    <br> Aceptado el 22 de abril de 2004</font></p>     ]]></body>
<body><![CDATA[<p align="justify"><font face="verdana" size="2">&nbsp;</font></p>     <p align="justify"><font face="verdana" size="2"><b>Abstract</b></font></p>     <p align="justify"><font face="verdana" size="2">Here we use linear analysis to investigate the propagation of small thermal and magnetohydrodynamic (MHD) disturbances in a heat&#150;conducting, ionizing&#150;recombining, hydrogen plasma threaded by an external uniform magnetic field. Linearization of the governing MHD equations for this model leads to a dispersion equation for the wavenumber <i>k </i>as a function of the frequency <i>&omega; </i>which may be either quadratic or cubic in <i>k<sup>2</sup></i>, depending on the orientation of the magnetic field. In either case, the solution of the dispersion equation is such that crossing of the roots may happen at some frequencies, implying that they may not always correspond to the same particular physical wave. The crossing of modes is merely a mathematical property of the solution and must not be interpreted as an interchange of the thermal and MHD waves' physical nature at the crossing frequency. Here we find that mode crossing is a function of the wave frequency, plasma temperature, magnetic field strength and orientation.</font></p>     <p align="justify"><font face="verdana" size="2"><b>Keywords:</b> Magnetohydrodynamics and plasmas; magnetohydrodynamic waves; sound waves; wave propagation.</font></p>     <p align="justify"><font face="verdana" size="2">&nbsp;</font></p>     <p align="justify"><font face="verdana" size="2"><b>Resumen</b></font></p>     <p align="justify"><font face="verdana" size="2">Mediante un an&aacute;lisis lineal se estudia la propagaci&oacute;n de perturbaciones t&eacute;rmicas y magnetohidrodin&aacute;micas (MHD) en un plasma de hidr&oacute;geno sujeto a la acci&oacute;n de un campo magn&eacute;tico externo de intensidad uniforme, incluyendo los efectos de conducci&oacute;n de calor, fotoionizaci&oacute;n y fotorecombinaci&oacute;n. A partir de la linealizaci&oacute;n de las ecuaciones MHD para este modelo se obtiene una ecuaci&oacute;n de dispersi&oacute;n para el n&uacute;mero de onda <i>k </i>en funcion de la frecuencia &omega;, que puede ser cuadr&aacute;tica o c&uacute;bica en <i>k<sup>2</sup> </i>dependiendo de la orientaci&oacute;n del campo magn&eacute;tico. En ambos casos, la soluci&oacute;n de la ecuaci&oacute;n de dispersi&oacute;n es tal que las raices pueden cruzarse a determinadas frecuencias. De este modo, las raices no siempre corresponder&aacute;n a la misma onda para todo el espectro de frecuencias. El cruce de modos es una propiedad matem&aacute;tica de la soluci&oacute;n y no debe interpretarse como un intercambio de la naturaleza f&iacute;sica de las ondas. Se encuentra que el cruce de modos es una funci&oacute;n de la frecuencia, de la temperatura del plasma y de la orientaci&oacute;n e intensidad del campo magn&eacute;tico.</font></p>     <p align="justify"><font face="verdana" size="2"><b>Descriptores:</b> Magnetohidrodin&aacute;mica y plasmas; ondas magnetohidrodin&aacute;micas; ondas ac&uacute;sticas; propagaci&oacute;n de ondas.</font></p>     <p align="justify"><font face="verdana" size="2">&nbsp;</font></p>     <p align="justify"><font face="verdana" size="2">PACS: 95.30.Qd; 52.35.Bj; 52.35.Dm; 94.20.Bb</font></p>     ]]></body>
<body><![CDATA[<p align="justify"><font face="verdana" size="2">&nbsp;</font></p>     <p align="justify"><font face="verdana" size="2"><a href="/pdf/rmf/v52s3/v52s3a68.pdf">DESCARGAR ART&Iacute;CULO EN FORMATO PDF</a></font></p>     <p align="justify"><font face="verdana" size="2">&nbsp;</font></p>     <p align="justify"><font face="verdana" size="2"><b>References</b></font></p>     <!-- ref --><p align="justify"><font face="verdana" size="2">1. M.H. Ib&aacute;&ntilde;ez S. and C.A. Mendoza, <i>Astrophys. Space Sci. </i><b>137 </b>(1987) 1.</font>&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;[&#160;<a href="javascript:void(0);" onclick="javascript: window.open('/scielo.php?script=sci_nlinks&ref=8328717&pid=S0035-001X200600090006800001&lng=','','width=640,height=500,resizable=yes,scrollbars=1,menubar=yes,');">Links</a>&#160;]<!-- end-ref --><!-- ref --><p align="justify"><font face="verdana" size="2">2. L. Di G. Sigalotti, E. Sira, and C. Tremola, <i>Phys. Plasmas </i><b>9</b> (2002) 4726.</font>&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;[&#160;<a href="javascript:void(0);" onclick="javascript: window.open('/scielo.php?script=sci_nlinks&ref=8328718&pid=S0035-001X200600090006800002&lng=','','width=640,height=500,resizable=yes,scrollbars=1,menubar=yes,');">Links</a>&#160;]<!-- end-ref --><!-- ref --><p align="justify"><font face="verdana" size="2">3. L. Di G. Sigalotti, E. Sira, O. Rend&oacute;n, C. Tremola, and C.A. Mendoza&#150;Brice&ntilde;o, <i>Phys. Plasmas </i><b>11 </b>(2003), submitted 1631.</font>&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;[&#160;<a href="javascript:void(0);" onclick="javascript: window.open('/scielo.php?script=sci_nlinks&ref=8328719&pid=S0035-001X200600090006800003&lng=','','width=640,height=500,resizable=yes,scrollbars=1,menubar=yes,');">Links</a>&#160;]<!-- end-ref --><!-- ref --><p align="justify"><font face="verdana" size="2">4. M.H. Ib&aacute;&ntilde;ez S. and A. Parravano, <i>Astrophys. J. </i><b>275 </b>(1983) 181.</font>&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;[&#160;<a href="javascript:void(0);" onclick="javascript: window.open('/scielo.php?script=sci_nlinks&ref=8328720&pid=S0035-001X200600090006800004&lng=','','width=640,height=500,resizable=yes,scrollbars=1,menubar=yes,');">Links</a>&#160;]<!-- end-ref --><!-- ref --><p align="justify"><font face="verdana" size="2">5. S.R. Pottasch, P.R. Wesselius, and R.J. Duinen, <i>Astron. Astrophys. Lett. </i><b>74</b> (1979) L15.</font>&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;[&#160;<a href="javascript:void(0);" onclick="javascript: window.open('/scielo.php?script=sci_nlinks&ref=8328721&pid=S0035-001X200600090006800005&lng=','','width=640,height=500,resizable=yes,scrollbars=1,menubar=yes,');">Links</a>&#160;]<!-- end-ref --><!-- ref --><p align="justify"><font face="verdana" size="2">6. L.  Spitzer, <i>Physical Processes in  the Interstellar Medium </i>(Wiley&#150;Interscience, New York, 1998) p. 18.</font>&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;[&#160;<a href="javascript:void(0);" onclick="javascript: window.open('/scielo.php?script=sci_nlinks&ref=8328722&pid=S0035-001X200600090006800006&lng=','','width=640,height=500,resizable=yes,scrollbars=1,menubar=yes,');">Links</a>&#160;]<!-- end-ref --> ]]></body><back>
<ref-list>
<ref id="B1">
<label>1</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Ibáñez S]]></surname>
<given-names><![CDATA[M.H]]></given-names>
</name>
<name>
<surname><![CDATA[Mendoza]]></surname>
<given-names><![CDATA[C.A]]></given-names>
</name>
</person-group>
<source><![CDATA[Astrophys. Space Sci]]></source>
<year>1987</year>
<numero>137</numero>
<issue>137</issue>
<page-range>1</page-range></nlm-citation>
</ref>
<ref id="B2">
<label>2</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Di G. Sigalotti]]></surname>
<given-names><![CDATA[L]]></given-names>
</name>
<name>
<surname><![CDATA[Sira]]></surname>
<given-names><![CDATA[E]]></given-names>
</name>
<name>
<surname><![CDATA[Tremola]]></surname>
<given-names><![CDATA[C]]></given-names>
</name>
</person-group>
<source><![CDATA[Phys. Plasmas]]></source>
<year>2002</year>
<numero>9</numero>
<issue>9</issue>
<page-range>4726</page-range></nlm-citation>
</ref>
<ref id="B3">
<label>3</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Di G. Sigalotti]]></surname>
<given-names><![CDATA[L]]></given-names>
</name>
<name>
<surname><![CDATA[Sira]]></surname>
<given-names><![CDATA[E]]></given-names>
</name>
<name>
<surname><![CDATA[Rendón]]></surname>
<given-names><![CDATA[O]]></given-names>
</name>
<name>
<surname><![CDATA[Tremola]]></surname>
<given-names><![CDATA[C]]></given-names>
</name>
<name>
<surname><![CDATA[Mendoza-Briceño]]></surname>
<given-names><![CDATA[C.A]]></given-names>
</name>
</person-group>
<source><![CDATA[Plasmas]]></source>
<year>2003</year>
<numero>11</numero>
<issue>11</issue>
<page-range>1631</page-range></nlm-citation>
</ref>
<ref id="B4">
<label>4</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Ibáñez S]]></surname>
<given-names><![CDATA[M.H]]></given-names>
</name>
<name>
<surname><![CDATA[Parravano]]></surname>
<given-names><![CDATA[A]]></given-names>
</name>
</person-group>
<source><![CDATA[Astrophys. J.]]></source>
<year>1983</year>
<numero>275</numero>
<issue>275</issue>
<page-range>181</page-range></nlm-citation>
</ref>
<ref id="B5">
<label>5</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Pottasch]]></surname>
<given-names><![CDATA[S.R]]></given-names>
</name>
<name>
<surname><![CDATA[Wesselius]]></surname>
<given-names><![CDATA[P.R]]></given-names>
</name>
<name>
<surname><![CDATA[Duinen]]></surname>
<given-names><![CDATA[R.J]]></given-names>
</name>
</person-group>
<source><![CDATA[Astron. Astrophys. Lett.]]></source>
<year>1979</year>
<numero>74</numero>
<issue>74</issue>
<page-range>L15</page-range></nlm-citation>
</ref>
<ref id="B6">
<label>6</label><nlm-citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Spitzer]]></surname>
<given-names><![CDATA[L]]></given-names>
</name>
</person-group>
<source><![CDATA[Physical Processes in the Interstellar Medium]]></source>
<year>1998</year>
<page-range>18</page-range><publisher-loc><![CDATA[New York ]]></publisher-loc>
<publisher-name><![CDATA[Wiley-Interscience]]></publisher-name>
</nlm-citation>
</ref>
</ref-list>
</back>
</article>
