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		<doi>10.1016/j.jastp.2010.06.007</doi>
		<issn>1364-6826</issn>
		<citationkey>TsurutaniEchVerLakGua:2011:MiInUp</citationkey>
		<title>Mirror instability upstream of the termination shock (TS) and in the heliosheath</title>
		<year>2011</year>
		<month>July</month>
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		<author>Tsurutani, Bruce T.,</author>
		<author>Echer, Ezequiel,</author>
		<author>Verkhoglyadovar, Olga P.,</author>
		<author>Lakhina, Gurbax S.,</author>
		<author>Guarnieri, F. L.,</author>
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		<group>DGE-CEA-INPE-MCT-BR</group>
		<affiliation></affiliation>
		<affiliation>Instituto Nacional de Pesquisas Espaciais (INPE)</affiliation>
		<affiliation></affiliation>
		<affiliation>ndian Institute of Geomagnetism, Navi Mumbai, India</affiliation>
		<affiliation>UNIVAP, Sao Jose dos Campos, SP, Brazil</affiliation>
		<electronicmailaddress>Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA</electronicmailaddress>
		<electronicmailaddress></electronicmailaddress>
		<electronicmailaddress>CSPAR, University of Alabama, Huntsville, AL, USA</electronicmailaddress>
		<e-mailaddress>lise@dpi.inpe.br</e-mailaddress>
		<journal>Journal of Atmospheric and Solar-Terrestrial Physics</journal>
		<volume>73</volume>
		<number>11–12</number>
		<pages>1398–1404</pages>
		<secondarytype>PRE PI</secondarytype>
		<secondarymark>B2_ASTRONOMIA_/_FÍSICA B1_CIÊNCIAS_BIOLÓGICAS_I B1_ECOLOGIA_E_MEIO_AMBIENTE B1_ENGENHARIAS_IV B1_GEOCIÊNCIAS A2_INTERDISCIPLINAR</secondarymark>
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		<keywords>Mirror instability, Pickup ions, Heliosheath, Magnetosheaths.</keywords>
		<abstract>We experimentally identify mirror mode (MM) structures in the Voyager 1 heliosheath data for the first time. This is done using the magnetic field data alone. The heliosheath MM structures are found to have the following characteristics: (1) quasiperiodic spacings with a typical scale size of not, vert, similar57 ñp, (2) little or no angular changes across the structures (not, vert, similar3° longitude and not, vert, similar3° latitude), and (3) a lack of sharp boundaries at the magnetic dip edges. It is demonstrated that the pickup of interstellar neutrals in the upstream region of the termination shock (TS) and quasiperpendicular TS plasma compression are the causes of MM instability during intervals when the IMF is nearly orthogonal to the solar wind flow direction. Concomitant additional injection of pickup ions (PUIs) throughout the heliosheath will lead to further MM amplification. MM structures in planetary magnetosheaths and interplanetary sheaths are discussed for comparative purposes. Multiple sources of free energy are often involved.</abstract>
		<area>CEA</area>
		<language>en</language>
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