Contribution of magnetic measurements onboard NetLander to Mars exploration
Identifieur interne : 001F90 ( Istex/Corpus ); précédent : 001F89; suivant : 001F91Contribution of magnetic measurements onboard NetLander to Mars exploration
Auteurs : Michel Menvielle ; Günter Musmann ; Falko Kuhnke ; Jean-Jacques Berthelier ; Karl-Heinz Glassmeier ; Mioara H. Mandea ; Uwe Motschmann ; Kari Pajunpaa ; Jean-Louis Pinçon ; Fritz Primdahl ; Laszlo SzarkaSource :
- Planetary and Space Science [ 0032-0633 ] ; 2000.
Abstract
In the frame of the international cooperation for Mars exploration, a set of 4 NetLanders developed by an European consortium is expected to land on the planet during the forthcoming years. Among other instruments, the geophysical package of each lander will include a magnetometer. The different possible contributions of magnetic measurements onboard the NetLander stations are presented. Intrinsic planetary field and remanent magnetisation investigations by means of magnetometers onboard a network of landers are first considered, and the information that can be thus derived on the Martian core dynamo and surface rocks, soil, and dust is discussed. The contribution of permanent recording of the magnetic transient variations at a network of surface stations is then discussed. The transient variations of the magnetic field at the surface of a planet has a primary external source, the interaction between the environment of the planet and solar radiation, and a secondary source, the electric currents induced in the conductive planet. The continuous recording of the time variations of the magnetic field at the surface of Mars by means of three component magnetometers installed onboard NetLander stations will therefore allow study of both the internal structure of Mars and dynamics of its ionised environment. The expected characteristics of transient magnetic variations, and their relation with plasma flow and current in the Mars ionised environment are discussed. The use of the network magnetic data to probe the internal structure of Mars is also considered. The used techniques are presented, and the information that can be thus obtained on the Mars permafrost, lithosphere and mantle structure illustrated by numerical simulations. Finally, the specifications of the instrument allowing to achieve these objectives are discussed, and the instrument described.
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DOI: 10.1016/S0032-0633(00)00106-9
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<record><TEI wicri:istexFullTextTei="biblStruct"><teiHeader><fileDesc><titleStmt><title>Contribution of magnetic measurements onboard NetLander to Mars exploration</title><author><name sortKey="Menvielle, Michel" sort="Menvielle, Michel" uniqKey="Menvielle M" first="Michel" last="Menvielle">Michel Menvielle</name><affiliation><mods:affiliation>E-mail: michel.menvielle@cetp.ipsl.fr</mods:affiliation></affiliation><affiliation><mods:affiliation>Observatoire de Saint-Maur, CETP UMR CNRS/UVSQ 8639, 4 Avenue de Neptune, F-94107 Saint-Maur-des-Fosses, Cedex France</mods:affiliation></affiliation></author><author><name sortKey="Musmann, Gunter" sort="Musmann, Gunter" uniqKey="Musmann G" first="Günter" last="Musmann">Günter Musmann</name><affiliation><mods:affiliation>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</mods:affiliation></affiliation></author><author><name sortKey="Kuhnke, Falko" sort="Kuhnke, Falko" uniqKey="Kuhnke F" first="Falko" last="Kuhnke">Falko Kuhnke</name><affiliation><mods:affiliation>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</mods:affiliation></affiliation></author><author><name sortKey="Berthelier, Jean Jacques" sort="Berthelier, Jean Jacques" uniqKey="Berthelier J" first="Jean-Jacques" last="Berthelier">Jean-Jacques Berthelier</name><affiliation><mods:affiliation>Observatoire de Saint-Maur, CETP UMR CNRS/UVSQ 8639, 4 Avenue de Neptune, F-94107 Saint-Maur-des-Fosses, Cedex France</mods:affiliation></affiliation></author><author><name sortKey="Glassmeier, Karl Heinz" sort="Glassmeier, Karl Heinz" uniqKey="Glassmeier K" first="Karl-Heinz" last="Glassmeier">Karl-Heinz Glassmeier</name><affiliation><mods:affiliation>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</mods:affiliation></affiliation></author><author><name sortKey="Mandea, Mioara H" sort="Mandea, Mioara H" uniqKey="Mandea M" first="Mioara H." last="Mandea">Mioara H. 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Mandea</name><affiliation><mods:affiliation>I.P.G.P., 4 Place Jussieu, F-75252 Paris Cedex 05, France</mods:affiliation></affiliation></author><author><name sortKey="Motschmann, Uwe" sort="Motschmann, Uwe" uniqKey="Motschmann U" first="Uwe" last="Motschmann">Uwe Motschmann</name><affiliation><mods:affiliation>Inst. für Theoretische Physik, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</mods:affiliation></affiliation></author><author><name sortKey="Pajunpaa, Kari" sort="Pajunpaa, Kari" uniqKey="Pajunpaa K" first="Kari" last="Pajunpaa">Kari Pajunpaa</name><affiliation><mods:affiliation>F.M.I., Box 503, FIN-00101 Helsinki, Finland</mods:affiliation></affiliation></author><author><name sortKey="Pincon, Jean Louis" sort="Pincon, Jean Louis" uniqKey="Pincon J" first="Jean-Louis" last="Pinçon">Jean-Louis Pinçon</name><affiliation><mods:affiliation>L.P.C.E., 3A Avenue de la Recherche Scientifique, F-45071 Orleans Cedex 2, France</mods:affiliation></affiliation></author><author><name sortKey="Primdahl, Fritz" sort="Primdahl, Fritz" uniqKey="Primdahl F" first="Fritz" last="Primdahl">Fritz Primdahl</name><affiliation><mods:affiliation>Danish Space Research Institute, DK-2800 Lyngby, Denmark</mods:affiliation></affiliation></author><author><name sortKey="Szarka, Laszlo" sort="Szarka, Laszlo" uniqKey="Szarka L" first="Laszlo" last="Szarka">Laszlo Szarka</name><affiliation><mods:affiliation>G.G.K.I., Po.B. 5, H-9400 Sopron, Hungary</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">Planetary and Space Science</title><title level="j" type="abbrev">PSS</title><idno type="ISSN">0032-0633</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="2000">2000</date><biblScope unit="volume">48</biblScope><biblScope unit="issue">12–14</biblScope><biblScope unit="page" from="1231">1231</biblScope><biblScope unit="page" to="1247">1247</biblScope></imprint><idno type="ISSN">0032-0633</idno></series><idno type="istex">384E1306B8E16B1C589F2F428FDBA08FC46B4B3C</idno><idno type="DOI">10.1016/S0032-0633(00)00106-9</idno><idno type="PII">S0032-0633(00)00106-9</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0032-0633</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">In the frame of the international cooperation for Mars exploration, a set of 4 NetLanders developed by an European consortium is expected to land on the planet during the forthcoming years. Among other instruments, the geophysical package of each lander will include a magnetometer. The different possible contributions of magnetic measurements onboard the NetLander stations are presented. Intrinsic planetary field and remanent magnetisation investigations by means of magnetometers onboard a network of landers are first considered, and the information that can be thus derived on the Martian core dynamo and surface rocks, soil, and dust is discussed. The contribution of permanent recording of the magnetic transient variations at a network of surface stations is then discussed. The transient variations of the magnetic field at the surface of a planet has a primary external source, the interaction between the environment of the planet and solar radiation, and a secondary source, the electric currents induced in the conductive planet. The continuous recording of the time variations of the magnetic field at the surface of Mars by means of three component magnetometers installed onboard NetLander stations will therefore allow study of both the internal structure of Mars and dynamics of its ionised environment. The expected characteristics of transient magnetic variations, and their relation with plasma flow and current in the Mars ionised environment are discussed. The use of the network magnetic data to probe the internal structure of Mars is also considered. The used techniques are presented, and the information that can be thus obtained on the Mars permafrost, lithosphere and mantle structure illustrated by numerical simulations. Finally, the specifications of the instrument allowing to achieve these objectives are discussed, and the instrument described.</div></front></TEI><istex><corpusName>elsevier</corpusName><author><json:item><name>Michel Menvielle</name><affiliations><json:string>E-mail: michel.menvielle@cetp.ipsl.fr</json:string><json:string>Observatoire de Saint-Maur, CETP UMR CNRS/UVSQ 8639, 4 Avenue de Neptune, F-94107 Saint-Maur-des-Fosses, Cedex France</json:string></affiliations></json:item><json:item><name>Günter Musmann</name><affiliations><json:string>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</json:string></affiliations></json:item><json:item><name>Falko Kuhnke</name><affiliations><json:string>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</json:string></affiliations></json:item><json:item><name>Jean-Jacques Berthelier</name><affiliations><json:string>Observatoire de Saint-Maur, CETP UMR CNRS/UVSQ 8639, 4 Avenue de Neptune, F-94107 Saint-Maur-des-Fosses, Cedex France</json:string></affiliations></json:item><json:item><name>Karl-Heinz Glassmeier</name><affiliations><json:string>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</json:string></affiliations></json:item><json:item><name>Mioara H. Mandea</name><affiliations><json:string>I.P.G.P., 4 Place Jussieu, F-75252 Paris Cedex 05, France</json:string></affiliations></json:item><json:item><name>Uwe Motschmann</name><affiliations><json:string>Inst. für Theoretische Physik, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</json:string></affiliations></json:item><json:item><name>Kari Pajunpaa</name><affiliations><json:string>F.M.I., Box 503, FIN-00101 Helsinki, Finland</json:string></affiliations></json:item><json:item><name>Jean-Louis Pinçon</name><affiliations><json:string>L.P.C.E., 3A Avenue de la Recherche Scientifique, F-45071 Orleans Cedex 2, France</json:string></affiliations></json:item><json:item><name>Fritz Primdahl</name><affiliations><json:string>Danish Space Research Institute, DK-2800 Lyngby, Denmark</json:string></affiliations></json:item><json:item><name>Laszlo Szarka</name><affiliations><json:string>G.G.K.I., Po.B. 5, H-9400 Sopron, Hungary</json:string></affiliations></json:item></author><language><json:string>eng</json:string></language><originalGenre><json:string>Full-length article</json:string></originalGenre><abstract>In the frame of the international cooperation for Mars exploration, a set of 4 NetLanders developed by an European consortium is expected to land on the planet during the forthcoming years. Among other instruments, the geophysical package of each lander will include a magnetometer. The different possible contributions of magnetic measurements onboard the NetLander stations are presented. Intrinsic planetary field and remanent magnetisation investigations by means of magnetometers onboard a network of landers are first considered, and the information that can be thus derived on the Martian core dynamo and surface rocks, soil, and dust is discussed. The contribution of permanent recording of the magnetic transient variations at a network of surface stations is then discussed. The transient variations of the magnetic field at the surface of a planet has a primary external source, the interaction between the environment of the planet and solar radiation, and a secondary source, the electric currents induced in the conductive planet. The continuous recording of the time variations of the magnetic field at the surface of Mars by means of three component magnetometers installed onboard NetLander stations will therefore allow study of both the internal structure of Mars and dynamics of its ionised environment. The expected characteristics of transient magnetic variations, and their relation with plasma flow and current in the Mars ionised environment are discussed. The use of the network magnetic data to probe the internal structure of Mars is also considered. The used techniques are presented, and the information that can be thus obtained on the Mars permafrost, lithosphere and mantle structure illustrated by numerical simulations. Finally, the specifications of the instrument allowing to achieve these objectives are discussed, and the instrument described.</abstract><qualityIndicators><score>8</score><pdfVersion>1.2</pdfVersion><pdfPageSize>596 x 792 pts</pdfPageSize><refBibsNative>true</refBibsNative><keywordCount>0</keywordCount><abstractCharCount>1882</abstractCharCount><pdfWordCount>13077</pdfWordCount><pdfCharCount>76969</pdfCharCount><pdfPageCount>17</pdfPageCount><abstractWordCount>281</abstractWordCount></qualityIndicators><title>Contribution of magnetic measurements onboard NetLander to Mars exploration</title><pii><json:string>S0032-0633(00)00106-9</json:string></pii><refBibs><json:item><author><json:item><name>M.H. Acuña</name></json:item><json:item><name>J.E.P. Connerney</name></json:item><json:item><name>P. Wasilewski</name></json:item><json:item><name>R.P. Lin</name></json:item><json:item><name>K.A. Anderson</name></json:item><json:item><name>C.W. Carlson</name></json:item><json:item><name>J. 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The field observed along the trajectory at 3 s intervals is represented by a scaled vector projection of B originating from the position of the spacecraft at such times. Field vectors are scaled to 400 nT=1Rm. (b) Magnitude of the observed magnetic field as a function of time for the interval of time represented in (a) (from Acuña et al. (1998)).</note><note type="content">Fig. 2: Variation of the resistivity for different types of permafrost with respect to temperature (Bogolyubov, 1978). A — massive texture; B — fine texture.</note><note type="content">Fig. 3: A posteriori distribution of the parameters for two 1-D models of permafrost, corresponding to typical high- (a) and low-latitude (b) situations. The data sets consist of apparent resistivities computed at frequencies evenly distributed on a logarithmic scale (10 points per decade) over three different ranges: 10 – 0.001 Hz(nF=41; left), 1 – 0.001 Hz (nF=31; middle), and 0.1 – 0.001 Hz (nF=21; right). In each case, a 16% Gaussian noise is added. For all the models, the a priori distribution and the marginal a posteriori distributions are digitised over a set of 101 possible resistivities evenly distributed on a logarithmic scale as 20 values per decade over the [1Ωm 100,000 Ωm] interval. The results are presented as images, with the resistivities along the horizontal (x) axis, and the depths along the vertical (y). In the images, the level of grey of the (m,1) pixel corresponds to the value of the marginal a posteriori distribution of the parameter Xl for Xl=ρm: the darker the pixel, the higher the marginal a posteriori probability. On each image, the more likely values (dotted curves) and the expected values (dashed curves) of the resistivities, as well as the resistivity profile of the model used to compute the apparent resistivities (continuous curve) are also plotted. (see text for further explanations).</note><note type="content">Fig. 4: A posteriori distribution of the parameters for two 1-D models of mantle, corresponding to a ‘cold’ adiabatic convective mantle, topped by a 200 km thick lithosphere with conductive heat transfer (a), and a ‘hot’ adiabatic mantle, topped by a 300 km thick lithosphere lithosphere (b) (models 1a and 2b from Mocquet and Menvielle (2000)). The data sets consist of apparent resistivities computed at frequencies evenly distributed on a logarithmic scale (10 points per decade) over the range 0.1–0.0001 Hz, plus 1 to 5 cycle per day (cpd) (nF=36). In each case, a 16% Gaussian noise is added. For all the models, the a priori distribution and the marginal a posteriori distributions are digitised over a set of 71 possible resistivities evenly distributed on a logarithmic scale as 10 values per decade over the [0.001Ωm, 10,000Ωm] interval. The results are presented as images, with the resistivities along the horizontal (x) axis, and the depths along the vertical (y). In the images, the level of grey of the (m,l) pixel corresponds to the value of the marginal a posteriori distribution of the parameter Xl for Xl=ρm: the darker the pixel, the higher the marginal a posteriori probability. On each image, the more likely values (dotted curves) and the expected values (dashed curves) of the resistivities, as well as the resistivity profile of the model used to compute the apparent resistivities (continuous curve) are also plotted. (see text for further explanations).</note><note type="content">Fig. 5: (a) Hypothetical hysteresis magnetisation curve for a martian soil material. (b) Material remanence curve for the soil represented by the hysteresis curve in panel a. On the hysteresis loop, the magnetisation follows irreversibly the arrows shown. Within the loop curve, the magnetisation is assumed to be reversible along the dashed lines parallel to the upper and lower branches. (c) Calculated remanence field Brem at the fluxgate position as a function of the previous coil current lpeak. The computations have been made for a horizontal coil, at a distance of 20 mm above the Mars surface, and a magnetometer on the axis of the coil, at a distance of 50 mm above the Mars surface (from Nielsen et al., 1992).</note><note type="content">Table 1: Description of the models used to make the numerical simulations presented in Sections 4.2 and 4.3 L in the number of layers of the model, z, is the thickness of the uppermost layer, and zL the depth to the top of the homogeneous underlying half-space (see text for further explanations)</note><note type="content">Table 2: Magnetic experiment specifications</note></notesStmt><sourceDesc><biblStruct type="inbook"><analytic><title level="a">Contribution of magnetic measurements onboard NetLander to Mars exploration</title><author xml:id="author-1"><persName><forename type="first">Michel</forename><surname>Menvielle</surname></persName><email>michel.menvielle@cetp.ipsl.fr</email><note type="correspondence"><p>Correspondence address: Observatoire de Saint-Maur, CETP-CNRS, 4 Avenue de Neptune, 94107 Saint-Maur-des-Fosses, France. Tel.: 33-1-4511-4234; fax: 33-1-4889-4433</p></note><affiliation>Observatoire de Saint-Maur, CETP UMR CNRS/UVSQ 8639, 4 Avenue de Neptune, F-94107 Saint-Maur-des-Fosses, Cedex France</affiliation></author><author xml:id="author-2"><persName><forename type="first">Günter</forename><surname>Musmann</surname></persName><affiliation>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</affiliation></author><author xml:id="author-3"><persName><forename type="first">Falko</forename><surname>Kuhnke</surname></persName><affiliation>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</affiliation></author><author xml:id="author-4"><persName><forename type="first">Jean-Jacques</forename><surname>Berthelier</surname></persName><affiliation>Observatoire de Saint-Maur, CETP UMR CNRS/UVSQ 8639, 4 Avenue de Neptune, F-94107 Saint-Maur-des-Fosses, Cedex France</affiliation></author><author xml:id="author-5"><persName><forename type="first">Karl-Heinz</forename><surname>Glassmeier</surname></persName><affiliation>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</affiliation></author><author xml:id="author-6"><persName><forename type="first">Mioara H.</forename><surname>Mandea</surname></persName><affiliation>I.P.G.P., 4 Place Jussieu, F-75252 Paris Cedex 05, France</affiliation></author><author xml:id="author-7"><persName><forename type="first">Uwe</forename><surname>Motschmann</surname></persName><affiliation>Inst. für Theoretische Physik, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</affiliation></author><author xml:id="author-8"><persName><forename type="first">Kari</forename><surname>Pajunpaa</surname></persName><affiliation>F.M.I., Box 503, FIN-00101 Helsinki, Finland</affiliation></author><author xml:id="author-9"><persName><forename type="first">Jean-Louis</forename><surname>Pinçon</surname></persName><affiliation>L.P.C.E., 3A Avenue de la Recherche Scientifique, F-45071 Orleans Cedex 2, France</affiliation></author><author xml:id="author-10"><persName><forename type="first">Fritz</forename><surname>Primdahl</surname></persName><affiliation>Danish Space Research Institute, DK-2800 Lyngby, Denmark</affiliation></author><author xml:id="author-11"><persName><forename type="first">Laszlo</forename><surname>Szarka</surname></persName><affiliation>G.G.K.I., Po.B. 5, H-9400 Sopron, Hungary</affiliation></author></analytic><monogr><title level="j">Planetary and Space Science</title><title level="j" type="abbrev">PSS</title><idno type="pISSN">0032-0633</idno><idno type="PII">S0032-0633(00)X0058-X</idno><meeting><addName>Mars Exploration Program</addName><addName>Mars Exploration</addName></meeting><editor><persName>Sotin</persName></editor><imprint><publisher>ELSEVIER</publisher><date type="published" when="2000"></date><biblScope unit="volume">48</biblScope><biblScope unit="issue">12–14</biblScope><biblScope unit="page" from="1231">1231</biblScope><biblScope unit="page" to="1247">1247</biblScope></imprint></monogr><idno type="istex">384E1306B8E16B1C589F2F428FDBA08FC46B4B3C</idno><idno type="DOI">10.1016/S0032-0633(00)00106-9</idno><idno type="PII">S0032-0633(00)00106-9</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>2000</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>In the frame of the international cooperation for Mars exploration, a set of 4 NetLanders developed by an European consortium is expected to land on the planet during the forthcoming years. Among other instruments, the geophysical package of each lander will include a magnetometer. The different possible contributions of magnetic measurements onboard the NetLander stations are presented. Intrinsic planetary field and remanent magnetisation investigations by means of magnetometers onboard a network of landers are first considered, and the information that can be thus derived on the Martian core dynamo and surface rocks, soil, and dust is discussed. The contribution of permanent recording of the magnetic transient variations at a network of surface stations is then discussed. The transient variations of the magnetic field at the surface of a planet has a primary external source, the interaction between the environment of the planet and solar radiation, and a secondary source, the electric currents induced in the conductive planet. The continuous recording of the time variations of the magnetic field at the surface of Mars by means of three component magnetometers installed onboard NetLander stations will therefore allow study of both the internal structure of Mars and dynamics of its ionised environment. The expected characteristics of transient magnetic variations, and their relation with plasma flow and current in the Mars ionised environment are discussed. The use of the network magnetic data to probe the internal structure of Mars is also considered. The used techniques are presented, and the information that can be thus obtained on the Mars permafrost, lithosphere and mantle structure illustrated by numerical simulations. Finally, the specifications of the instrument allowing to achieve these objectives are discussed, and the instrument described.</p></abstract></profileDesc><revisionDesc><change when="2000">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/384E1306B8E16B1C589F2F428FDBA08FC46B4B3C/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Elsevier, elements deleted: ce:floats; body; tail"><istex:xmlDeclaration>version="1.0" encoding="utf-8"</istex:xmlDeclaration><istex:docType PUBLIC="-//ES//DTD journal article DTD version 4.5.2//EN//XML" URI="art452.dtd" name="istex:docType"><istex:entity SYSTEM="gr1" NDATA="IMAGE" name="gr1"></istex:entity><istex:entity SYSTEM="gr2" NDATA="IMAGE" name="gr2"></istex:entity><istex:entity SYSTEM="gr3" NDATA="IMAGE" name="gr3"></istex:entity><istex:entity SYSTEM="gr4" NDATA="IMAGE" name="gr4"></istex:entity><istex:entity SYSTEM="gr5" NDATA="IMAGE" name="gr5"></istex:entity></istex:docType><istex:document><converted-article version="4.5.2" docsubtype="fla"><item-info><jid>PSS</jid><aid>1215</aid><ce:pii>S0032-0633(00)00106-9</ce:pii><ce:doi>10.1016/S0032-0633(00)00106-9</ce:doi><ce:copyright type="full-transfer" year="2000">Elsevier Science Ltd</ce:copyright></item-info><head><ce:title>Contribution of magnetic measurements onboard NetLander to Mars exploration</ce:title><ce:author-group><ce:author><ce:given-name>Michel</ce:given-name><ce:surname>Menvielle</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>a</ce:sup></ce:cross-ref><ce:cross-ref refid="AFF2"><ce:sup>b</ce:sup></ce:cross-ref><ce:cross-ref refid="CORR1">*</ce:cross-ref><ce:e-address>michel.menvielle@cetp.ipsl.fr</ce:e-address></ce:author><ce:author><ce:given-name>Günter</ce:given-name><ce:surname>Musmann</ce:surname><ce:cross-ref refid="AFF3"><ce:sup>c</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Falko</ce:given-name><ce:surname>Kuhnke</ce:surname><ce:cross-ref refid="AFF3"><ce:sup>c</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Jean-Jacques</ce:given-name><ce:surname>Berthelier</ce:surname><ce:cross-ref refid="AFF1"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Karl-Heinz</ce:given-name><ce:surname>Glassmeier</ce:surname><ce:cross-ref refid="AFF3"><ce:sup>c</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Mioara H.</ce:given-name><ce:surname>Mandea</ce:surname><ce:cross-ref refid="AFF4"><ce:sup>d</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Uwe</ce:given-name><ce:surname>Motschmann</ce:surname><ce:cross-ref refid="AFF5"><ce:sup>e</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Kari</ce:given-name><ce:surname>Pajunpaa</ce:surname><ce:cross-ref refid="AFF6"><ce:sup>f</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Jean-Louis</ce:given-name><ce:surname>Pinçon</ce:surname><ce:cross-ref refid="AFF7"><ce:sup>g</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Fritz</ce:given-name><ce:surname>Primdahl</ce:surname><ce:cross-ref refid="AFF8"><ce:sup>h</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Laszlo</ce:given-name><ce:surname>Szarka</ce:surname><ce:cross-ref refid="AFF9"><ce:sup>i</ce:sup></ce:cross-ref></ce:author><ce:affiliation id="AFF1"><ce:label>a</ce:label><ce:textfn>Observatoire de Saint-Maur, CETP UMR CNRS/UVSQ 8639, 4 Avenue de Neptune, F-94107 Saint-Maur-des-Fosses, Cedex France</ce:textfn></ce:affiliation><ce:affiliation id="AFF2"><ce:label>b</ce:label><ce:textfn>Département des Sciences de la Terre, Université Paris Sud, Orsay, France</ce:textfn></ce:affiliation><ce:affiliation id="AFF3"><ce:label>c</ce:label><ce:textfn>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</ce:textfn></ce:affiliation><ce:affiliation id="AFF4"><ce:label>d</ce:label><ce:textfn>I.P.G.P., 4 Place Jussieu, F-75252 Paris Cedex 05, France</ce:textfn></ce:affiliation><ce:affiliation id="AFF5"><ce:label>e</ce:label><ce:textfn>Inst. für Theoretische Physik, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</ce:textfn></ce:affiliation><ce:affiliation id="AFF6"><ce:label>f</ce:label><ce:textfn>F.M.I., Box 503, FIN-00101 Helsinki, Finland</ce:textfn></ce:affiliation><ce:affiliation id="AFF7"><ce:label>g</ce:label><ce:textfn>L.P.C.E., 3A Avenue de la Recherche Scientifique, F-45071 Orleans Cedex 2, France</ce:textfn></ce:affiliation><ce:affiliation id="AFF8"><ce:label>h</ce:label><ce:textfn>Danish Space Research Institute, DK-2800 Lyngby, Denmark</ce:textfn></ce:affiliation><ce:affiliation id="AFF9"><ce:label>i</ce:label><ce:textfn>G.G.K.I., Po.B. 5, H-9400 Sopron, Hungary</ce:textfn></ce:affiliation><ce:correspondence id="CORR1"><ce:label>*</ce:label><ce:text>Correspondence address: Observatoire de Saint-Maur, CETP-CNRS, 4 Avenue de Neptune, 94107 Saint-Maur-des-Fosses, France. Tel.: 33-1-4511-4234; fax: 33-1-4889-4433</ce:text></ce:correspondence></ce:author-group><ce:date-received day="28" month="5" year="1999"></ce:date-received><ce:date-accepted day="15" month="11" year="1999"></ce:date-accepted><ce:abstract><ce:section-title>Abstract</ce:section-title><ce:abstract-sec><ce:simple-para>In the frame of the international cooperation for Mars exploration, a set of 4 NetLanders developed by an European consortium is expected to land on the planet during the forthcoming years. Among other instruments, the geophysical package of each lander will include a magnetometer. The different possible contributions of magnetic measurements onboard the NetLander stations are presented. Intrinsic planetary field and remanent magnetisation investigations by means of magnetometers onboard a network of landers are first considered, and the information that can be thus derived on the Martian core dynamo and surface rocks, soil, and dust is discussed. The contribution of permanent recording of the magnetic transient variations at a network of surface stations is then discussed. The transient variations of the magnetic field at the surface of a planet has a primary external source, the interaction between the environment of the planet and solar radiation, and a secondary source, the electric currents induced in the conductive planet. The continuous recording of the time variations of the magnetic field at the surface of Mars by means of three component magnetometers installed onboard NetLander stations will therefore allow study of both the internal structure of Mars and dynamics of its ionised environment. The expected characteristics of transient magnetic variations, and their relation with plasma flow and current in the Mars ionised environment are discussed. The use of the network magnetic data to probe the internal structure of Mars is also considered. The used techniques are presented, and the information that can be thus obtained on the Mars permafrost, lithosphere and mantle structure illustrated by numerical simulations. Finally, the specifications of the instrument allowing to achieve these objectives are discussed, and the instrument described.</ce:simple-para></ce:abstract-sec></ce:abstract></head></converted-article></istex:document></istex:metadataXml><mods version="3.6"><titleInfo><title>Contribution of magnetic measurements onboard NetLander to Mars exploration</title></titleInfo><titleInfo type="alternative" contentType="CDATA"><title>Contribution of magnetic measurements onboard NetLander to Mars exploration</title></titleInfo><name type="personal"><namePart type="given">Michel</namePart><namePart type="family">Menvielle</namePart><affiliation>E-mail: michel.menvielle@cetp.ipsl.fr</affiliation><affiliation>Observatoire de Saint-Maur, CETP UMR CNRS/UVSQ 8639, 4 Avenue de Neptune, F-94107 Saint-Maur-des-Fosses, Cedex France</affiliation><description>Correspondence address: Observatoire de Saint-Maur, CETP-CNRS, 4 Avenue de Neptune, 94107 Saint-Maur-des-Fosses, France. Tel.: 33-1-4511-4234; fax: 33-1-4889-4433</description><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Günter</namePart><namePart type="family">Musmann</namePart><affiliation>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Falko</namePart><namePart type="family">Kuhnke</namePart><affiliation>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Jean-Jacques</namePart><namePart type="family">Berthelier</namePart><affiliation>Observatoire de Saint-Maur, CETP UMR CNRS/UVSQ 8639, 4 Avenue de Neptune, F-94107 Saint-Maur-des-Fosses, Cedex France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Karl-Heinz</namePart><namePart type="family">Glassmeier</namePart><affiliation>I.G.M./TU-BS, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Mioara H.</namePart><namePart type="family">Mandea</namePart><affiliation>I.P.G.P., 4 Place Jussieu, F-75252 Paris Cedex 05, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Uwe</namePart><namePart type="family">Motschmann</namePart><affiliation>Inst. für Theoretische Physik, Mendelssohnstrasse 3, D-38106 Braunschweig, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Kari</namePart><namePart type="family">Pajunpaa</namePart><affiliation>F.M.I., Box 503, FIN-00101 Helsinki, Finland</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Jean-Louis</namePart><namePart type="family">Pinçon</namePart><affiliation>L.P.C.E., 3A Avenue de la Recherche Scientifique, F-45071 Orleans Cedex 2, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Fritz</namePart><namePart type="family">Primdahl</namePart><affiliation>Danish Space Research Institute, DK-2800 Lyngby, Denmark</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Laszlo</namePart><namePart type="family">Szarka</namePart><affiliation>G.G.K.I., Po.B. 5, H-9400 Sopron, Hungary</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="research-article" displayLabel="Full-length article"></genre><originInfo><publisher>ELSEVIER</publisher><dateIssued encoding="w3cdtf">2000</dateIssued><copyrightDate encoding="w3cdtf">2000</copyrightDate></originInfo><language><languageTerm type="code" authority="iso639-2b">eng</languageTerm><languageTerm type="code" authority="rfc3066">en</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType></physicalDescription><abstract lang="en">In the frame of the international cooperation for Mars exploration, a set of 4 NetLanders developed by an European consortium is expected to land on the planet during the forthcoming years. Among other instruments, the geophysical package of each lander will include a magnetometer. The different possible contributions of magnetic measurements onboard the NetLander stations are presented. Intrinsic planetary field and remanent magnetisation investigations by means of magnetometers onboard a network of landers are first considered, and the information that can be thus derived on the Martian core dynamo and surface rocks, soil, and dust is discussed. The contribution of permanent recording of the magnetic transient variations at a network of surface stations is then discussed. The transient variations of the magnetic field at the surface of a planet has a primary external source, the interaction between the environment of the planet and solar radiation, and a secondary source, the electric currents induced in the conductive planet. The continuous recording of the time variations of the magnetic field at the surface of Mars by means of three component magnetometers installed onboard NetLander stations will therefore allow study of both the internal structure of Mars and dynamics of its ionised environment. The expected characteristics of transient magnetic variations, and their relation with plasma flow and current in the Mars ionised environment are discussed. The use of the network magnetic data to probe the internal structure of Mars is also considered. The used techniques are presented, and the information that can be thus obtained on the Mars permafrost, lithosphere and mantle structure illustrated by numerical simulations. Finally, the specifications of the instrument allowing to achieve these objectives are discussed, and the instrument described.</abstract><note type="content">Fig. 1: Projection of the MGS spacecraft trajectory and observed magnetic field onto a plane perpendicular to the Mars orbit plane and the Mars–Sun line for periapsis pass # 6 on day 264. The field observed along the trajectory at 3 s intervals is represented by a scaled vector projection of B originating from the position of the spacecraft at such times. Field vectors are scaled to 400 nT=1Rm. (b) Magnitude of the observed magnetic field as a function of time for the interval of time represented in (a) (from Acuña et al. (1998)).</note><note type="content">Fig. 2: Variation of the resistivity for different types of permafrost with respect to temperature (Bogolyubov, 1978). A — massive texture; B — fine texture.</note><note type="content">Fig. 3: A posteriori distribution of the parameters for two 1-D models of permafrost, corresponding to typical high- (a) and low-latitude (b) situations. The data sets consist of apparent resistivities computed at frequencies evenly distributed on a logarithmic scale (10 points per decade) over three different ranges: 10 – 0.001 Hz(nF=41; left), 1 – 0.001 Hz (nF=31; middle), and 0.1 – 0.001 Hz (nF=21; right). In each case, a 16% Gaussian noise is added. For all the models, the a priori distribution and the marginal a posteriori distributions are digitised over a set of 101 possible resistivities evenly distributed on a logarithmic scale as 20 values per decade over the [1Ωm 100,000 Ωm] interval. The results are presented as images, with the resistivities along the horizontal (x) axis, and the depths along the vertical (y). In the images, the level of grey of the (m,1) pixel corresponds to the value of the marginal a posteriori distribution of the parameter Xl for Xl=ρm: the darker the pixel, the higher the marginal a posteriori probability. On each image, the more likely values (dotted curves) and the expected values (dashed curves) of the resistivities, as well as the resistivity profile of the model used to compute the apparent resistivities (continuous curve) are also plotted. (see text for further explanations).</note><note type="content">Fig. 4: A posteriori distribution of the parameters for two 1-D models of mantle, corresponding to a ‘cold’ adiabatic convective mantle, topped by a 200 km thick lithosphere with conductive heat transfer (a), and a ‘hot’ adiabatic mantle, topped by a 300 km thick lithosphere lithosphere (b) (models 1a and 2b from Mocquet and Menvielle (2000)). The data sets consist of apparent resistivities computed at frequencies evenly distributed on a logarithmic scale (10 points per decade) over the range 0.1–0.0001 Hz, plus 1 to 5 cycle per day (cpd) (nF=36). In each case, a 16% Gaussian noise is added. For all the models, the a priori distribution and the marginal a posteriori distributions are digitised over a set of 71 possible resistivities evenly distributed on a logarithmic scale as 10 values per decade over the [0.001Ωm, 10,000Ωm] interval. The results are presented as images, with the resistivities along the horizontal (x) axis, and the depths along the vertical (y). In the images, the level of grey of the (m,l) pixel corresponds to the value of the marginal a posteriori distribution of the parameter Xl for Xl=ρm: the darker the pixel, the higher the marginal a posteriori probability. On each image, the more likely values (dotted curves) and the expected values (dashed curves) of the resistivities, as well as the resistivity profile of the model used to compute the apparent resistivities (continuous curve) are also plotted. (see text for further explanations).</note><note type="content">Fig. 5: (a) Hypothetical hysteresis magnetisation curve for a martian soil material. (b) Material remanence curve for the soil represented by the hysteresis curve in panel a. On the hysteresis loop, the magnetisation follows irreversibly the arrows shown. Within the loop curve, the magnetisation is assumed to be reversible along the dashed lines parallel to the upper and lower branches. (c) Calculated remanence field Brem at the fluxgate position as a function of the previous coil current lpeak. The computations have been made for a horizontal coil, at a distance of 20 mm above the Mars surface, and a magnetometer on the axis of the coil, at a distance of 50 mm above the Mars surface (from Nielsen et al., 1992).</note><note type="content">Table 1: Description of the models used to make the numerical simulations presented in Sections 4.2 and 4.3 L in the number of layers of the model, z, is the thickness of the uppermost layer, and zL the depth to the top of the homogeneous underlying half-space (see text for further explanations)</note><note type="content">Table 2: Magnetic experiment specifications</note><relatedItem type="host"><titleInfo><title>Planetary and Space Science</title></titleInfo><titleInfo type="abbreviated"><title>PSS</title></titleInfo><name type="conference"><namePart>Mars Exploration Program</namePart><namePart>Mars Exploration</namePart></name><name type="personal"><namePart>Sotin</namePart><role><roleTerm type="text">editor</roleTerm></role></name><genre type="journal">journal</genre><originInfo><dateIssued encoding="w3cdtf">200010</dateIssued></originInfo><identifier type="ISSN">0032-0633</identifier><identifier type="PII">S0032-0633(00)X0058-X</identifier><part><date>200010</date><detail type="issue"><title>Mars Exploration Program</title></detail><detail type="volume"><number>48</number><caption>vol.</caption></detail><detail type="issue"><number>12–14</number><caption>no.</caption></detail><extent unit="issue pages"><start>1143</start><end>1422</end></extent><extent unit="pages"><start>1231</start><end>1247</end></extent></part></relatedItem><identifier type="istex">384E1306B8E16B1C589F2F428FDBA08FC46B4B3C</identifier><identifier type="DOI">10.1016/S0032-0633(00)00106-9</identifier><identifier type="PII">S0032-0633(00)00106-9</identifier><accessCondition type="use and reproduction" contentType="copyright">©2000 Elsevier Science Ltd</accessCondition><recordInfo><recordContentSource>ELSEVIER</recordContentSource><recordOrigin>Elsevier Science Ltd, ©2000</recordOrigin></recordInfo></mods></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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