NATURE OF THE MHD AND KINETIC SCALE TURBULENCE IN THE MAGNETOSHEATH OF SATURN: CASSINI OBSERVATIONS
ABSTRACT Low-frequency turbulence in Saturn's magnetosheath is investigated using in situ measurements of the Cassini spacecraft. Focus is put on the magnetic energy spectra computed in the frequency range of ∼[10−4, 1]Hz. A set of 42 time intervals in the magnetosheath were analyzed, and three...
Gespeichert in:
Veröffentlicht in: | Astrophysical journal. Letters 2015-11, Vol.813 (2), p.1-6 |
---|---|
Hauptverfasser: | , , , , , , , |
Format: | Artikel |
Sprache: | eng |
Schlagworte: | |
Online-Zugang: | Volltext bestellen |
Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
container_end_page | 6 |
---|---|
container_issue | 2 |
container_start_page | 1 |
container_title | Astrophysical journal. Letters |
container_volume | 813 |
creator | Hadid, L. Z. Sahraoui, F. Kiyani, K. H. Retinò, A. Modolo, R. Canu, P. Masters, A. Dougherty, M. K. |
description | ABSTRACT Low-frequency turbulence in Saturn's magnetosheath is investigated using in situ measurements of the Cassini spacecraft. Focus is put on the magnetic energy spectra computed in the frequency range of ∼[10−4, 1]Hz. A set of 42 time intervals in the magnetosheath were analyzed, and three main results that contrast with known features of solar wind turbulence are reported. (1) The magnetic energy spectra showed a ∼f−1 scaling at MHD scales followed by an scaling at sub-ion scales without forming the so-called inertial range. (2) The magnetic compressibility and the cross-correlation between the parallel component of the magnetic field and density fluctuations indicate the dominance of the compressible magnetosonic slow-like modes at MHD scales rather than the Alfvén mode. (3) Higher-order statistics revealed a monofractal (multifractal) behavior of the turbulent flow downstream of a quasi-perpendicular (quasi-parallel) shock at sub-ion scales. Implications of these results on theoretical modeling of space plasma turbulence are discussed. |
doi_str_mv | 10.1088/2041-8205/813/2/L29 |
format | Article |
fullrecord | <record><control><sourceid>proquest_O3W</sourceid><recordid>TN_cdi_proquest_miscellaneous_1793273826</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>1773837146</sourcerecordid><originalsourceid>FETCH-LOGICAL-c435t-fcab06075e0a3d8c848a282a2e1ab66120f89ba3e18233d142236f256c36d3c43</originalsourceid><addsrcrecordid>eNqNkUFPgzAYhonRxDn9BV56NCaT9it0nTfGukFESAbz2nQMIss2Jh0m_ntLWHY0nvqled73a_pY1iPBLwRzbgN2yIgDdm1OqA12BJMra3C-JfT6MmP31rrTeosxYEb4wMpjL1stBUrmKAsEeg9myItn6C2MRRb6KPW9SCBDTFeRiH2BwrjnvIUBkjQQXhZ04bSriV-R76VpGIcomaZi-eFlYRKn99ZNqXa6eDifQ2s1F5kfjKJkEZoFo9yh7mlU5mqNGR67BVZ0w3PucAUcFBRErRkjgEs-WStaEA6UbogDQFkJLssp21DTMbSe-95PtZPHptqr5kfWqpKBF8nqoFuJCYCLmfNNDPzUw8em_moLfZL7SufFbqcORd1qScYTCmPKgf0DNRwdE6dDaY_mTa11U5SXdxAsO1WyEyE7EdKokiCNKpOy-1RVH-W2bpuD-aY_E7-YeomC</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>1773837146</pqid></control><display><type>article</type><title>NATURE OF THE MHD AND KINETIC SCALE TURBULENCE IN THE MAGNETOSHEATH OF SATURN: CASSINI OBSERVATIONS</title><source>IOP Publishing Free Content</source><creator>Hadid, L. Z. ; Sahraoui, F. ; Kiyani, K. H. ; Retinò, A. ; Modolo, R. ; Canu, P. ; Masters, A. ; Dougherty, M. K.</creator><creatorcontrib>Hadid, L. Z. ; Sahraoui, F. ; Kiyani, K. H. ; Retinò, A. ; Modolo, R. ; Canu, P. ; Masters, A. ; Dougherty, M. K.</creatorcontrib><description>ABSTRACT Low-frequency turbulence in Saturn's magnetosheath is investigated using in situ measurements of the Cassini spacecraft. Focus is put on the magnetic energy spectra computed in the frequency range of ∼[10−4, 1]Hz. A set of 42 time intervals in the magnetosheath were analyzed, and three main results that contrast with known features of solar wind turbulence are reported. (1) The magnetic energy spectra showed a ∼f−1 scaling at MHD scales followed by an scaling at sub-ion scales without forming the so-called inertial range. (2) The magnetic compressibility and the cross-correlation between the parallel component of the magnetic field and density fluctuations indicate the dominance of the compressible magnetosonic slow-like modes at MHD scales rather than the Alfvén mode. (3) Higher-order statistics revealed a monofractal (multifractal) behavior of the turbulent flow downstream of a quasi-perpendicular (quasi-parallel) shock at sub-ion scales. Implications of these results on theoretical modeling of space plasma turbulence are discussed.</description><identifier>ISSN: 2041-8205</identifier><identifier>ISSN: 2041-8213</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.1088/2041-8205/813/2/L29</identifier><language>eng</language><publisher>The American Astronomical Society</publisher><subject>Astrophysics ; Cassini mission ; Compressibility ; Computational fluid dynamics ; Earth and Planetary Astrophysics ; Fluid flow ; magnetic fields ; Magnetohydrodynamic turbulence ; Magnetosheath ; planets and satellites: individual (Saturn) ; plasmas ; Sciences of the Universe ; Solar and Stellar Astrophysics ; Turbulence ; Turbulent flow ; waves</subject><ispartof>Astrophysical journal. Letters, 2015-11, Vol.813 (2), p.1-6</ispartof><rights>2015. The American Astronomical Society. All rights reserved.</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c435t-fcab06075e0a3d8c848a282a2e1ab66120f89ba3e18233d142236f256c36d3c43</citedby><cites>FETCH-LOGICAL-c435t-fcab06075e0a3d8c848a282a2e1ab66120f89ba3e18233d142236f256c36d3c43</cites><orcidid>0000-0001-5437-9923 ; 0000-0002-2517-4846 ; 0000-0002-5973-8339 ; 0000-0001-5824-2852 ; 0000-0002-8587-0202 ; 0000-0002-7209-7732</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.1088/2041-8205/813/2/L29/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,780,784,885,27924,27925,38868,38890,53840,53867</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.1088/2041-8205/813/2/L29$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://insu.hal.science/insu-01225064$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Hadid, L. Z.</creatorcontrib><creatorcontrib>Sahraoui, F.</creatorcontrib><creatorcontrib>Kiyani, K. H.</creatorcontrib><creatorcontrib>Retinò, A.</creatorcontrib><creatorcontrib>Modolo, R.</creatorcontrib><creatorcontrib>Canu, P.</creatorcontrib><creatorcontrib>Masters, A.</creatorcontrib><creatorcontrib>Dougherty, M. K.</creatorcontrib><title>NATURE OF THE MHD AND KINETIC SCALE TURBULENCE IN THE MAGNETOSHEATH OF SATURN: CASSINI OBSERVATIONS</title><title>Astrophysical journal. Letters</title><addtitle>APJL</addtitle><addtitle>Astrophys. J. Lett</addtitle><description>ABSTRACT Low-frequency turbulence in Saturn's magnetosheath is investigated using in situ measurements of the Cassini spacecraft. Focus is put on the magnetic energy spectra computed in the frequency range of ∼[10−4, 1]Hz. A set of 42 time intervals in the magnetosheath were analyzed, and three main results that contrast with known features of solar wind turbulence are reported. (1) The magnetic energy spectra showed a ∼f−1 scaling at MHD scales followed by an scaling at sub-ion scales without forming the so-called inertial range. (2) The magnetic compressibility and the cross-correlation between the parallel component of the magnetic field and density fluctuations indicate the dominance of the compressible magnetosonic slow-like modes at MHD scales rather than the Alfvén mode. (3) Higher-order statistics revealed a monofractal (multifractal) behavior of the turbulent flow downstream of a quasi-perpendicular (quasi-parallel) shock at sub-ion scales. Implications of these results on theoretical modeling of space plasma turbulence are discussed.</description><subject>Astrophysics</subject><subject>Cassini mission</subject><subject>Compressibility</subject><subject>Computational fluid dynamics</subject><subject>Earth and Planetary Astrophysics</subject><subject>Fluid flow</subject><subject>magnetic fields</subject><subject>Magnetohydrodynamic turbulence</subject><subject>Magnetosheath</subject><subject>planets and satellites: individual (Saturn)</subject><subject>plasmas</subject><subject>Sciences of the Universe</subject><subject>Solar and Stellar Astrophysics</subject><subject>Turbulence</subject><subject>Turbulent flow</subject><subject>waves</subject><issn>2041-8205</issn><issn>2041-8213</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2015</creationdate><recordtype>article</recordtype><recordid>eNqNkUFPgzAYhonRxDn9BV56NCaT9it0nTfGukFESAbz2nQMIss2Jh0m_ntLWHY0nvqled73a_pY1iPBLwRzbgN2yIgDdm1OqA12BJMra3C-JfT6MmP31rrTeosxYEb4wMpjL1stBUrmKAsEeg9myItn6C2MRRb6KPW9SCBDTFeRiH2BwrjnvIUBkjQQXhZ04bSriV-R76VpGIcomaZi-eFlYRKn99ZNqXa6eDifQ2s1F5kfjKJkEZoFo9yh7mlU5mqNGR67BVZ0w3PucAUcFBRErRkjgEs-WStaEA6UbogDQFkJLssp21DTMbSe-95PtZPHptqr5kfWqpKBF8nqoFuJCYCLmfNNDPzUw8em_moLfZL7SufFbqcORd1qScYTCmPKgf0DNRwdE6dDaY_mTa11U5SXdxAsO1WyEyE7EdKokiCNKpOy-1RVH-W2bpuD-aY_E7-YeomC</recordid><startdate>20151110</startdate><enddate>20151110</enddate><creator>Hadid, L. Z.</creator><creator>Sahraoui, F.</creator><creator>Kiyani, K. H.</creator><creator>Retinò, A.</creator><creator>Modolo, R.</creator><creator>Canu, P.</creator><creator>Masters, A.</creator><creator>Dougherty, M. K.</creator><general>The American Astronomical Society</general><general>Bristol : IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0001-5437-9923</orcidid><orcidid>https://orcid.org/0000-0002-2517-4846</orcidid><orcidid>https://orcid.org/0000-0002-5973-8339</orcidid><orcidid>https://orcid.org/0000-0001-5824-2852</orcidid><orcidid>https://orcid.org/0000-0002-8587-0202</orcidid><orcidid>https://orcid.org/0000-0002-7209-7732</orcidid></search><sort><creationdate>20151110</creationdate><title>NATURE OF THE MHD AND KINETIC SCALE TURBULENCE IN THE MAGNETOSHEATH OF SATURN: CASSINI OBSERVATIONS</title><author>Hadid, L. Z. ; Sahraoui, F. ; Kiyani, K. H. ; Retinò, A. ; Modolo, R. ; Canu, P. ; Masters, A. ; Dougherty, M. K.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c435t-fcab06075e0a3d8c848a282a2e1ab66120f89ba3e18233d142236f256c36d3c43</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2015</creationdate><topic>Astrophysics</topic><topic>Cassini mission</topic><topic>Compressibility</topic><topic>Computational fluid dynamics</topic><topic>Earth and Planetary Astrophysics</topic><topic>Fluid flow</topic><topic>magnetic fields</topic><topic>Magnetohydrodynamic turbulence</topic><topic>Magnetosheath</topic><topic>planets and satellites: individual (Saturn)</topic><topic>plasmas</topic><topic>Sciences of the Universe</topic><topic>Solar and Stellar Astrophysics</topic><topic>Turbulence</topic><topic>Turbulent flow</topic><topic>waves</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Hadid, L. Z.</creatorcontrib><creatorcontrib>Sahraoui, F.</creatorcontrib><creatorcontrib>Kiyani, K. H.</creatorcontrib><creatorcontrib>Retinò, A.</creatorcontrib><creatorcontrib>Modolo, R.</creatorcontrib><creatorcontrib>Canu, P.</creatorcontrib><creatorcontrib>Masters, A.</creatorcontrib><creatorcontrib>Dougherty, M. K.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Hadid, L. Z.</au><au>Sahraoui, F.</au><au>Kiyani, K. H.</au><au>Retinò, A.</au><au>Modolo, R.</au><au>Canu, P.</au><au>Masters, A.</au><au>Dougherty, M. K.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>NATURE OF THE MHD AND KINETIC SCALE TURBULENCE IN THE MAGNETOSHEATH OF SATURN: CASSINI OBSERVATIONS</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJL</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2015-11-10</date><risdate>2015</risdate><volume>813</volume><issue>2</issue><spage>1</spage><epage>6</epage><pages>1-6</pages><issn>2041-8205</issn><issn>2041-8213</issn><eissn>2041-8213</eissn><abstract>ABSTRACT Low-frequency turbulence in Saturn's magnetosheath is investigated using in situ measurements of the Cassini spacecraft. Focus is put on the magnetic energy spectra computed in the frequency range of ∼[10−4, 1]Hz. A set of 42 time intervals in the magnetosheath were analyzed, and three main results that contrast with known features of solar wind turbulence are reported. (1) The magnetic energy spectra showed a ∼f−1 scaling at MHD scales followed by an scaling at sub-ion scales without forming the so-called inertial range. (2) The magnetic compressibility and the cross-correlation between the parallel component of the magnetic field and density fluctuations indicate the dominance of the compressible magnetosonic slow-like modes at MHD scales rather than the Alfvén mode. (3) Higher-order statistics revealed a monofractal (multifractal) behavior of the turbulent flow downstream of a quasi-perpendicular (quasi-parallel) shock at sub-ion scales. Implications of these results on theoretical modeling of space plasma turbulence are discussed.</abstract><pub>The American Astronomical Society</pub><doi>10.1088/2041-8205/813/2/L29</doi><tpages>6</tpages><orcidid>https://orcid.org/0000-0001-5437-9923</orcidid><orcidid>https://orcid.org/0000-0002-2517-4846</orcidid><orcidid>https://orcid.org/0000-0002-5973-8339</orcidid><orcidid>https://orcid.org/0000-0001-5824-2852</orcidid><orcidid>https://orcid.org/0000-0002-8587-0202</orcidid><orcidid>https://orcid.org/0000-0002-7209-7732</orcidid><oa>free_for_read</oa></addata></record> |
fulltext | fulltext_linktorsrc |
identifier | ISSN: 2041-8205 |
ispartof | Astrophysical journal. Letters, 2015-11, Vol.813 (2), p.1-6 |
issn | 2041-8205 2041-8213 2041-8213 |
language | eng |
recordid | cdi_proquest_miscellaneous_1793273826 |
source | IOP Publishing Free Content |
subjects | Astrophysics Cassini mission Compressibility Computational fluid dynamics Earth and Planetary Astrophysics Fluid flow magnetic fields Magnetohydrodynamic turbulence Magnetosheath planets and satellites: individual (Saturn) plasmas Sciences of the Universe Solar and Stellar Astrophysics Turbulence Turbulent flow waves |
title | NATURE OF THE MHD AND KINETIC SCALE TURBULENCE IN THE MAGNETOSHEATH OF SATURN: CASSINI OBSERVATIONS |
url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-05T20%3A37%3A55IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_O3W&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=NATURE%20OF%20THE%20MHD%20AND%20KINETIC%20SCALE%20TURBULENCE%20IN%20THE%20MAGNETOSHEATH%20OF%20SATURN:%20CASSINI%20OBSERVATIONS&rft.jtitle=Astrophysical%20journal.%20Letters&rft.au=Hadid,%20L.%20Z.&rft.date=2015-11-10&rft.volume=813&rft.issue=2&rft.spage=1&rft.epage=6&rft.pages=1-6&rft.issn=2041-8205&rft.eissn=2041-8213&rft_id=info:doi/10.1088/2041-8205/813/2/L29&rft_dat=%3Cproquest_O3W%3E1773837146%3C/proquest_O3W%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=1773837146&rft_id=info:pmid/&rfr_iscdi=true |