<?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>S0035-001X2024000300018</article-id>
<article-id pub-id-type="doi">10.31349/revmexfis.70.031501</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Investigating the effects of numerical algorithms on global magnetohydrodynamics simulations of solar wind in the inner heliosphere]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[León Alanís]]></surname>
<given-names><![CDATA[L. A. de]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[González-Avilés]]></surname>
<given-names><![CDATA[J. J.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Riley]]></surname>
<given-names><![CDATA[P.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Ben-Nun]]></surname>
<given-names><![CDATA[M.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Universidad Autónoma de Nuevo León Facultad de Ciencias Físico Matemáticas ]]></institution>
<addr-line><![CDATA[San Nicolás de los Garza Nuevo León]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Universidad Nacional Autónoma de México Escuela Nacional de Estudios Superiores ]]></institution>
<addr-line><![CDATA[Morelia Michoacán]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="Af3">
<institution><![CDATA[,Predictive Science Inc.  ]]></institution>
<addr-line><![CDATA[San Diego CA]]></addr-line>
<country>USA</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>06</month>
<year>2024</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>06</month>
<year>2024</year>
</pub-date>
<volume>70</volume>
<numero>3</numero>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0035-001X2024000300018&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0035-001X2024000300018&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0035-001X2024000300018&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract This paper explores the effects of numerical algorithms on global magnetohydrodynamics simulations of solar wind (SW) in the inner heliosphere. To do so, we use sunRunner3D, a 3-D magnetohydrodynamics model that employs the boundary conditions generated by CORHEL and the PLUTO code to compute the plasma properties of the SW with the ideal magnetohydrodynamics approximation up to 1.1 AU in the inner heliosphere. Mainly, we define three different combinations of numerical algorithms based on their diffusion level. This diffusion level is related to the way of solving the magnetohydrodynamics equations using the finite volume formulation, and, therefore, we set in terms of the divergence-free condition methods, Riemann solvers, variable reconstruction schemes, limiters, and time-steeping algorithms. According to the simulation results, we demonstrate that sunRunner3D reproduces global features of Corotating Interaction Regions observed by Earth-based spacecraft for a set of Carrington rotations that cover a period that lays in the late declining phase of solar cycle 24, independently of the numerical algorithms. Moreover, statistical analyses between models and in-situ measurements show reasonable agreement with the observations, and remarkably, the high diffusive method matches better with in-situ data than low diffusive methods.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[Solar wind]]></kwd>
<kwd lng="en"><![CDATA[magnetohydrodynamics]]></kwd>
<kwd lng="en"><![CDATA[numerical methods]]></kwd>
<kwd lng="en"><![CDATA[heliosphere]]></kwd>
</kwd-group>
</article-meta>
</front><back>
<ref-list>
<ref id="B1">
<label>1</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Riley]]></surname>
<given-names><![CDATA[P.]]></given-names>
</name>
<name>
<surname><![CDATA[Linker]]></surname>
<given-names><![CDATA[J. A.]]></given-names>
</name>
<name>
<surname><![CDATA[Mikic`]]></surname>
<given-names><![CDATA[Z.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[An empirically-driven global MHD model of the solar corona and inner heliosphere]]></article-title>
<source><![CDATA[Journal of Geophysical Research: Space Physics]]></source>
<year>2001</year>
<volume>106</volume>
</nlm-citation>
</ref>
<ref id="B2">
<label>2</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Odstrcil]]></surname>
<given-names><![CDATA[D.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Modeling 3-D solar wind structure]]></article-title>
<source><![CDATA[Advances in Space Research]]></source>
<year>2003</year>
<volume>32</volume>
<page-range>497</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[Tóth]]></surname>
<given-names><![CDATA[G.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Space Weather Modeling Framework: A new tool for the space science community]]></article-title>
<source><![CDATA[Journal of Geophysical Research: Space Physics]]></source>
<year>2005</year>
<volume>110</volume>
</nlm-citation>
</ref>
<ref id="B4">
<label>4</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Feng]]></surname>
<given-names><![CDATA[X.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Three-Dimensional Solar Wind Modeling from The Sun to Earth by a SIP-CESE MHD Model with a Six-Component Grid]]></article-title>
<source><![CDATA[The Astrophysical Journal]]></source>
<year>2010</year>
<volume>723</volume>
</nlm-citation>
</ref>
<ref id="B5">
<label>5</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Shiota]]></surname>
<given-names><![CDATA[D.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Inner heliosphere MHD modeling system applicable to space weather forecasting for the other planets]]></article-title>
<source><![CDATA[Space Weather]]></source>
<year>2014</year>
<volume>12</volume>
</nlm-citation>
</ref>
<ref id="B6">
<label>6</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Pomoell]]></surname>
<given-names><![CDATA[J.]]></given-names>
</name>
<name>
<surname><![CDATA[Poedts]]></surname>
<given-names><![CDATA[S.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[EUHFORIA: European heliospheric forecasting information asset]]></article-title>
<source><![CDATA[J. Space Weather Space Clim.]]></source>
<year>2018</year>
<volume>8</volume>
</nlm-citation>
</ref>
<ref id="B7">
<label>7</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Mayank]]></surname>
<given-names><![CDATA[P.]]></given-names>
</name>
<name>
<surname><![CDATA[Vaidya]]></surname>
<given-names><![CDATA[B.]]></given-names>
</name>
<name>
<surname><![CDATA[Chakrabarty]]></surname>
<given-names><![CDATA[D.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[SWASTi-SW: Space Weather Adaptive Simulation Framework for Solar Wind and Its Relevance to the Aditya-L1 Mission]]></article-title>
<source><![CDATA[The Astrophysical Journal]]></source>
<year>2022</year>
<volume>262</volume>
</nlm-citation>
</ref>
<ref id="B8">
<label>8</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Goldstein]]></surname>
<given-names><![CDATA[M. L.]]></given-names>
</name>
<name>
<surname><![CDATA[Roberts]]></surname>
<given-names><![CDATA[D. A.]]></given-names>
</name>
<name>
<surname><![CDATA[Matthaeus]]></surname>
<given-names><![CDATA[W.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Magneto-hydrodynamic turbulence in the solar wind]]></article-title>
<source><![CDATA[Annual review of astronomy and astrophysics]]></source>
<year>1995</year>
<volume>33</volume>
<page-range>283</page-range></nlm-citation>
</ref>
<ref id="B9">
<label>9</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Wang]]></surname>
<given-names><![CDATA[C.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Magnetohydrodynamics (MHD) numerical simulations on the interaction of the solar wind with the magnetosphere: A review]]></article-title>
<source><![CDATA[Science China Earth Sciences]]></source>
<year>2013</year>
<volume>56</volume>
<page-range>1141</page-range></nlm-citation>
</ref>
<ref id="B10">
<label>10</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Ogino]]></surname>
<given-names><![CDATA[T.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[A three-dimensional MHD simulation of the interaction of the solar wind with the Earth&#8217;s magnetosphere: The genera280 tion of field-aligned currents]]></article-title>
<source><![CDATA[Journal of Geophysical Research: Space Physics]]></source>
<year>1986</year>
<volume>91</volume>
<page-range>6791</page-range></nlm-citation>
</ref>
<ref id="B11">
<label>11</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Ip]]></surname>
<given-names><![CDATA[W.-H.]]></given-names>
</name>
<name>
<surname><![CDATA[Kopp]]></surname>
<given-names><![CDATA[A.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[MHD simulations of the solar wind interaction with Mercury]]></article-title>
<source><![CDATA[Journal of Geophysical Research: Space Physics]]></source>
<year>2002</year>
<volume>107</volume>
<page-range>SSH</page-range></nlm-citation>
</ref>
<ref id="B12">
<label>12</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Walker]]></surname>
<given-names><![CDATA[R. J.]]></given-names>
</name>
<name>
<surname><![CDATA[Ogino]]></surname>
<given-names><![CDATA[T.]]></given-names>
</name>
<name>
<surname><![CDATA[Kivelson]]></surname>
<given-names><![CDATA[M. G.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Magnetohydrodynamic simulations of the effects of the solar wind on the Jovian magneto sphere]]></article-title>
<source><![CDATA[Planetary and Space Science]]></source>
<year>2001</year>
<volume>49</volume>
<page-range>237</page-range></nlm-citation>
</ref>
<ref id="B13">
<label>13</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Baratashvili]]></surname>
<given-names><![CDATA[T.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Exploring the effects of numerical methods and slope limiters in heliospheric modeling]]></article-title>
<source><![CDATA[Sun and Geosphere]]></source>
<year>2023</year>
<volume>15</volume>
<page-range>49</page-range></nlm-citation>
</ref>
<ref id="B14">
<label>14</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Zhang]]></surname>
<given-names><![CDATA[M.]]></given-names>
</name>
<name>
<surname><![CDATA[Feng]]></surname>
<given-names><![CDATA[X.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[A comparative study of divergence cleaning methods of magnetic field in the solar coronal numerical simulation]]></article-title>
<source><![CDATA[Frontiers in Astronomy and Space Sciences]]></source>
<year>2016</year>
<volume>3</volume>
<page-range>6</page-range></nlm-citation>
</ref>
<ref id="B15">
<label>15</label><nlm-citation citation-type="">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Riley]]></surname>
<given-names><![CDATA[P.]]></given-names>
</name>
</person-group>
<source><![CDATA[Understanding the large-scale, three-dimensional structure of the 5th of September 2022 interplanetary coronal mass ejection through a new global MHD model]]></source>
<year>2023</year>
</nlm-citation>
</ref>
<ref id="B16">
<label>16</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Riley]]></surname>
<given-names><![CDATA[P.]]></given-names>
</name>
<name>
<surname><![CDATA[Ben-Nun]]></surname>
<given-names><![CDATA[M.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[sunRunner1D: A Tool for Exploring ICME Evolution through the Inner Heliosphere]]></article-title>
<source><![CDATA[Universe]]></source>
<year>2022</year>
<volume>8</volume>
</nlm-citation>
</ref>
<ref id="B17">
<label>17</label><nlm-citation citation-type="">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Gonález-Avilés]]></surname>
<given-names><![CDATA[J. J.]]></given-names>
</name>
</person-group>
<source><![CDATA[Using SunRunner3D to interpret the global structure of the heliosphere from in situ measurements]]></source>
<year>2023</year>
</nlm-citation>
</ref>
<ref id="B18">
<label>18</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Aguilar-Rodriguez]]></surname>
<given-names><![CDATA[E.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Numerical MHD models of Stream Interaction Regions (SIRs) and Corotating Interaction Regions (CIRs) using sunRunner3D: Comparison with observations]]></article-title>
<source><![CDATA[Monthly Notices of the Royal Astronomical Society]]></source>
<year>2023</year>
<volume>529</volume>
<page-range>1250</page-range></nlm-citation>
</ref>
<ref id="B19">
<label>19</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Linker]]></surname>
<given-names><![CDATA[J. A.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[CORHEL: AModeling Suite for Describing the Solar Corona and Inner Heliosphere]]></article-title>
<source><![CDATA[AGU FallMeeting Abstracts]]></source>
<year>2009</year>
<volume>2009</volume>
<page-range>SA43A-1612</page-range></nlm-citation>
</ref>
<ref id="B20">
<label>20</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Mignone]]></surname>
<given-names><![CDATA[A.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[PLUTO: A Numerical Code for Computational Astrophysics]]></article-title>
<source><![CDATA[The Astrophysical Journal]]></source>
<year>2007</year>
<volume>170</volume>
<page-range>228</page-range></nlm-citation>
</ref>
<ref id="B21">
<label>21</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Linker]]></surname>
<given-names><![CDATA[J. A.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[An Empirically Driven Time-Dependent Model of the SolarWind]]></article-title>
<source><![CDATA[Journal of Physics: Conference Series]]></source>
<year>2016</year>
<volume>719</volume>
</nlm-citation>
</ref>
<ref id="B22">
<label>22</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Riley]]></surname>
<given-names><![CDATA[P.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Corotating interaction regions during the recent solar minimum: The power and limitations of global MHD modeling]]></article-title>
<source><![CDATA[Journal of Atmospheric and Solar-Terrestrial Physics]]></source>
<year>2012</year>
<volume>83</volume>
</nlm-citation>
</ref>
<ref id="B23">
<label>23</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Mikic]]></surname>
<given-names><![CDATA[Z.]]></given-names>
</name>
<name>
<surname><![CDATA[Linker]]></surname>
<given-names><![CDATA[J. A.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[The large-scale structure of the solar corona and inner heliosphere]]></article-title>
<person-group person-group-type="editor">
<name>
<surname><![CDATA[Winterhalter]]></surname>
<given-names><![CDATA[D.]]></given-names>
</name>
</person-group>
<source><![CDATA[Proceedings of the eigth International solar wind Conference: Solar wind eight]]></source>
<year>1996</year>
<volume>382</volume>
</nlm-citation>
</ref>
<ref id="B24">
<label>24</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Mikic`]]></surname>
<given-names><![CDATA[Z.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Magnetohydrodynamic modeling of the global solar corona]]></article-title>
<source><![CDATA[Physics of Plasmas]]></source>
<year>1999</year>
<volume>6</volume>
</nlm-citation>
</ref>
<ref id="B25">
<label>25</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Kley]]></surname>
<given-names><![CDATA[W.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[On the treatment of the Coriolis force in computational astrophysics]]></article-title>
<source><![CDATA[A&amp; A]]></source>
<year>1998</year>
<volume>338</volume>
<page-range>L37</page-range></nlm-citation>
</ref>
<ref id="B26">
<label>26</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Mignone]]></surname>
<given-names><![CDATA[A.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[A conservative orbital advection scheme for simulations of magnetized shear flows with the PLUTO code]]></article-title>
<source><![CDATA[A&amp; A]]></source>
<year>2012</year>
<volume>545</volume>
<page-range>A152</page-range></nlm-citation>
</ref>
<ref id="B27">
<label>27</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Roe]]></surname>
<given-names><![CDATA[P.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Approximate Riemann solvers, parameter vectors, and difference schemes]]></article-title>
<source><![CDATA[Journal of Computational Physics]]></source>
<year>1981</year>
<volume>43</volume>
<page-range>357</page-range></nlm-citation>
</ref>
<ref id="B28">
<label>28</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Cada]]></surname>
<given-names><![CDATA[M.]]></given-names>
</name>
<name>
<surname><![CDATA[Torrilhon]]></surname>
<given-names><![CDATA[M.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Compact third-order limiter functions for finite volume methods]]></article-title>
<source><![CDATA[Journal of Computational Physics]]></source>
<year>2009</year>
<volume>228</volume>
<page-range>4118</page-range></nlm-citation>
</ref>
<ref id="B29">
<label>29</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Li]]></surname>
<given-names><![CDATA[S.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[An HLLC Riemann solver for magneto-hydrodynamics]]></article-title>
<source><![CDATA[Journal of Computational Physics]]></source>
<year>2005</year>
<volume>203</volume>
</nlm-citation>
</ref>
<ref id="B30">
<label>30</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Yamaleev]]></surname>
<given-names><![CDATA[N. K.]]></given-names>
</name>
<name>
<surname><![CDATA[Carpenter]]></surname>
<given-names><![CDATA[M. H.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[A systematic methodology for constructing high-order energy stable WENO schemes]]></article-title>
<source><![CDATA[Journal of Computational Physics]]></source>
<year>2009</year>
<volume>228</volume>
<page-range>4248</page-range></nlm-citation>
</ref>
<ref id="B31">
<label>31</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Yee]]></surname>
<given-names><![CDATA[H.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Construction of explicit and implicit symmetric TVD schemes and their applications]]></article-title>
<source><![CDATA[Journal of Computational Physics]]></source>
<year>1987</year>
<volume>68</volume>
<page-range>151</page-range></nlm-citation>
</ref>
<ref id="B32">
<label>32</label><nlm-citation citation-type="">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Powell]]></surname>
<given-names><![CDATA[K. G.]]></given-names>
</name>
</person-group>
<source><![CDATA[Approximate Riemann solver for magnetohydrodynamics (that works in more than one dimension)]]></source>
<year>1994</year>
</nlm-citation>
</ref>
<ref id="B33">
<label>33</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Dedner]]></surname>
<given-names><![CDATA[A.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Hyperbolic Divergence Cleaning for the MHD Equations]]></article-title>
<source><![CDATA[Journal of Computational Physics]]></source>
<year>2002</year>
<volume>175</volume>
<page-range>645</page-range></nlm-citation>
</ref>
<ref id="B34">
<label>34</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Miyoshi]]></surname>
<given-names><![CDATA[T.]]></given-names>
</name>
<name>
<surname><![CDATA[Kusano]]></surname>
<given-names><![CDATA[K.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[A multi-state HLL approximate Riemann solver for ideal magnetohydrodynamics]]></article-title>
<source><![CDATA[Journal of Computational Physics]]></source>
<year>2005</year>
<volume>208</volume>
<page-range>315</page-range></nlm-citation>
</ref>
<ref id="B35">
<label>35</label><nlm-citation citation-type="">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Stansby]]></surname>
<given-names><![CDATA[D.]]></given-names>
</name>
<name>
<surname><![CDATA[Riley]]></surname>
<given-names><![CDATA[P.]]></given-names>
</name>
</person-group>
<source><![CDATA[PsiPy]]></source>
<year>2022</year>
</nlm-citation>
</ref>
<ref id="B36">
<label>36</label><nlm-citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname><![CDATA[Reiss]]></surname>
<given-names><![CDATA[M. A.]]></given-names>
</name>
</person-group>
<article-title xml:lang=""><![CDATA[Unifying the validation of ambient solar wind models]]></article-title>
<source><![CDATA[Advances in Space Research]]></source>
<year>2022</year>
</nlm-citation>
</ref>
</ref-list>
</back>
</article>
