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The correlati.ns of i.ns densi.y wi.h geomagneti. acti.i.y and solar dynami. pressure i. cusp regi.n

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Chi.ese Sci.nce Bulleti. 2007年第7期52卷 967-971页

作者： GUO Ji.nGuang SHi.Ji.nKui.ZHANG Ti.Long Li. ZhenXi.g A. FAZAKERLEY H. REME i. dandouras E. LUOEK State Key Laboratory of Space Weather CSSAR Chinese Academy of Sciences Beijing 100080 China Graduate Uni.ersi.y of the Chi.ese Academy of Sci.nces Beijing 100049 China Space Research i.sti.ute Austrian Academy of Sciences Graz A-8010 Austria MSSL University College London Holmbury St. Mary Dorking RH5 6NT UK CESR Toulouse 31028 France i.peri.l College London SW7 2BZ UK

A stati.ti.al study of the properti.s of i.ns (O+, He+ and H+) measured by the Cluster-i. i. cusp regi.n as a functi.n of the solar wi.d dynami. pressure and geomagneti. i.dex Kp respecti.ely was made dur-i.g the summer and fall of 2001-2003. The mai. results are that: (1) O+ i.n densi.y responds i. a si.-ni.i.ant way to geomagneti. i.dex Kp, and He+ i.n densi.y i. not correlated wi.h geomagneti. i.dex Kp, both of them have a si.ni.i.ant posi.i.e correlati.n wi.h solar wi.d dynami. pressure; (2) H+ i.n densi.y i. also observed to i.crease wi.h solar wi.d dynami. pressure, and not correlated wi.h geomagneti. i.dex Kp.

关键词：极隙区地磁活动离子密度太阳风动压相关性

Surveys on magnetospheri. plasmas based on the Double Star Project (DSP) explorati.n

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Sci.nce Chi.a(Technologi.al Sci.nces) 2008年第10期51卷 1639-1647页

作者： C. P. ESCOUBET C. M. CARR H. RME A. FAZAKERLEY H. LAAKSO i. dandouras M. DUNLOP ESA/ESTEC SCI-SH Keplerlaan 1 2200 AG Noordwijk The Netherlands i.peri.l College of Sci.nce Technology and Medicine London SW7 2BZ United Kingdom CESR BP4346 31028 Toulouse Cedex 4 France Mullard Space Sci.nce Laboratory Univ. College London Dorking Surrey RH5 6NT United Kingdom i.peri.l College of Sci.nce Technology and Medicine London SW7 2BZ United Kingdom Rutherford Appleton Laboratory Didcot Oxon OX11 0QX United Kingdom

The equatori.l and polar satelli.es of the Double Star Project (DSP) were launched successfully on December 29, 2003 and July 25, 2004, respecti.ely, and both of them are operati.g smoothly. The DSP provi.es a good opportuni.y for i.vesti.at-i.g the structure of the magnetosphere. Based on the DSP data collected duri.g 2004, we have surveyed the di.tri.uti.n of the magneti. fi.lds and plasmas i. the magnetosphere. i. i. found that: (1) Near the Earth’s equatori.l plane wi.hi. geo-centri. di.tances of less than 7 RE, the Earth’s magneti. fi.ld i. di.olar. i. the vi.ci.i.y of the magnetopause, the magneti. fi.ld i. enhanced by a factor of about 1.5, and on the ni.htsi.e, the magneti. fi.ld can vary si.ni.i.antly from the Earth’s di.pole fi.ld, li.ely caused by the presence of the near-Earth tai. current sheet. (2) i. the day-si.e magnetosheath, the electron and i.n densi.i.s are usually both i. the range of 10―30 cm?3; the i.n and electron temperatures are usually about 200 and 50 eV, respecti.ely. The flow pattern i. usually smooth, wi.h a low veloci.y i. the subsolar regi.n and wi.h si.ni.i.antly hi.her veloci.i.s i. the dawn and dusk flanks. (3) i. the regi.n between the magnetopause and plasmasphere the densi.y i. low, approxi.ately 0.5―5 cm?3, and the temperature i. hi.h, about 1―10 keV for i.ns and 0.1―5 keV for electrons. The i.n temperature has an apparent ani.otropy, wi.h the rati. of the perpendi.ular and parallel temperatures bei.g about 1.0―1.3 for the ni.ht- and dusk-si.e magnetosphere and about 1.3―2.0 for the day- and dawn-si.e magnetosphere. There i. an evi.ent sunward convecti.n of about 50 km/s i. the magnetosphere. On the dawn si.e, the flow becomes somewhat turbulent, and i. the vi.i.i.y of the ni.ht-noon meri.i.n plane, the convecti.n i. rather slow. (4) The hi.h-energy electrons wi.h energi.s hi.her than 2 MeV are mai.ly located i. the regi.ns wi.h 3 i.e of the hi.h-energy electrons area vari.s wi.h ti.e, i. may expand and shri.k

关键词： Earth’s magnetosphere space explorati.n geomagneti. fi.ld space plasmas

A Theoreti. i.terpretati.n of Movement of the Cusp Equatorward Boundary

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空间科学学报 2005年第5期25卷 412-418页

作者： J. B. Cao A. Leonovi.h G. C. Zhou Z. X. Li. H. Reme i. dandouras Center for Space Sci.nce and Appli.d Research Chinese Academy of Sciences Beijing 100080 China Chi.a-Russi. Joi.t Research Center on Space Weather Beijing 100080 China Centre d＇Etude Spati.le des Rayonnements 31028 Toulouse France

A preli.i.ary model i. proposed to descri.e quanti.ati.ely the posi.i.n and movement of cusp equatorward boundary. Thi. i.tegrated model, consi.ti.g of an empi.i.al model of the magnetopause and a compressed di.olar model of Open/Closed fi.ld li.e, connects quanti.ati.ely the solar wi.d condi.i.ns, subsolar magnetopause and cusp equatorward boundary. i. i. shown that the i.creasi.g solar wi.d dynami. pressure and the i.creasi.g southward i.terplanetary Magneti. Fi.ld (i.F) component dri.e the magnetopause to move i.ward and the cusp equatorward. Thi. model i. adopted to i.terpret quanti.ati.ely the cusp movement of August 14, 2001 observed by Cluster. The results show that the subsolar magnetopause moved earthward from 10.7 Re to 9.0Re duri.g the peri.d of 002300-002800 UT, and correspondi.gly the cusp equatorward boundary shi.ted equatorward. The observati.ns of Cluster C1 and C4 show the cusp equatorward boundary that Cluster C1 and C4 were crossi.g duri.g same i.terval moved equatorward by 4.6°. The cusp equatorward boundary veloci.y computed i. the theoreti.al model (10.7 km/s) i. i. good agreement wi.h the observed value(9.4km/s) calculated from the data of Ci. of Cluster C4 and C1.

关键词：太阳风赤道边界线磁场

pTC-1 observati.n of i.n hi.h-speed flow reversal i. the near-Earth plasma sheet duri.g substorm

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Sci.nce Chi.a(Technologi.al Sci.nces) 2008年第10期51卷 1721-1730页

作者： H. RME i. dandouras C. M. CARR Centre d'Etude Spati.le des Rayonnements CEDEX 4 F-31028 Toulouse France The Blackett Laboratory Imperial College London SW7 2BW UK

Based on measurements of FGM and Hi. on board TC-1 at i.s apogee on Septem-ber 14, 2004, we analyzed the i.n hi.h-speed flows i. the near-Earth plasma sheet observed duri.g the substorm expansi.n phase. Strong tai.ward hi.h-speed flows (Vx ～ -350 km/s) were fi.st seen at about X ～ -13.2 RE i. near-Earth magnetotai., one mi.ute later the flows reversed from tai.ward to earthward. The reversal process occurred qui.kly after the substorm expansi.n onset. The near-Earth magnetotai. plasma sheet was one of key regi.ns for substorm onset. Our analysi. showed that the i.n flow reversal from tai.ward to earthward was li.ely to be i. close relati.n wi.h the substorm expansi.n i.i.i.ti.n and mi.ht play an i.portant role i. tri.ger-i.g the substorm expansi.n onset.

关键词： near-Earth magnetotai. magnetospheri. substorm plasma sheet i.n hi.h speed flow

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磁层快速对流事件的多点卫星联合观测

地球物理学报 2007年第5期50卷 1277-1282页

作者：马玉端曹晋滨周国成刘振兴 H. Reme i. dandouras E. Lucek 中国科学院空间天气学重点实验室北京100080 Centre d'Etude Spati.le des Rayonnements i.peri.l College London

本文利用星簇Cluster的三颗卫星(C1,C3和C4)在2001年和2002年的数据,研究了快速对流事件(RCE,Rapi. Convecti.n Event)及其与亚暴的关系.结果显示单点卫星对RCE的观测,不能反映磁尾RCE的真实情况.在2002年7月25日发生的一次RCE事件,C1... 详细信息

本文利用星簇Cluster的三颗卫星(C1,C3和C4)在2001年和2002年的数据,研究了快速对流事件(RCE,Rapi. Convecti.n Event)及其与亚暴的关系.结果显示单点卫星对RCE的观测,不能反映磁尾RCE的真实情况.在2002年7月25日发生的一次RCE事件,C1和C3观测到这次RCE,C4却没有观测到.在三颗卫星联合观测到的306次RCE中,C1观测到215次,C3观测到266次,C4观测到227次.统计研究表明,单点卫星观测到的RCE的平均时间也不能准确反映磁层内的RCE.由此推论在整个中心等离子体片内,快速对流事件所承担的能量和磁通量的输运量,可能远大于单点卫星观测给出的结果.用速度来定义的磁尾爆发性整体流(BBF,Bursty Bulk Flow)与亚暴的关系,比用磁通量定义的RCE与亚暴的关系要更加紧密.

关键词： RCE 磁通量持续时间输运

The radi.l evoluti.n of earthward BBFs duri.g substorm

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Sci.nce Chi.a Earth Sci.nces 2010年第10期53卷 1542-1551页

作者： REME H dandouras i.LUCEK E DUNLOP M Centre d'Etude Spati.le des Rayonnements Blackett Laboratory Imperial College London Rutherford Appleton Laboratory

We here study the occurrence rate,probabi.i.y functi.n of veloci.y and durati.n of earthward bursty bulk flows(BBFs) i. the i.ner Plasma Sheet(i.S,β>0.5) usi.g the data of Cluster i. 2001 and *** occurrence rate of earthward BBFs i.creases wi.h di.tance from the Earth up to ?19 RE,whi.h i. i. agreement wi.h the previ.us observati.ns of the radi.l evoluti.n of *** 54% of earthward BBFs i. expansi.n phase have a veloci.y larger than 600 km/s,whereas only 38% of earthward BBFs i. growth and recovery phases have a veloci.y larger than 600 km/*** average veloci.y of earthward BBFs i. expansi.n phase i. 732 km/s,larger than those i. growth phase(631 km/s) and recovery phase(617 km/s).The durati.ns of earthward BBFs decrease wi.h the decrease of downtai. di.tance from Earth due to the braki.g of earthward *** durati.n of earthward BBFs i. expansi.n phase i. larger than that i. growth and recovery *** average durati.ns i. growth,expansi.n,and recovery phases are respecti.ely 49.3,71.5,and 47.6 ***,the rati.s of transports of energy of earthward BBFs i. growth,expansi.n,and recovery phases can be esti.ated to be 0.51:1:***,the earthward BBFs i. the expansi.n phase have the largest capabi.i.y of the transport of energy and can produce the largest braki.g effects,such as i.erti.l currents and auroral acti.i.i.s.

关键词： substorm growth expansi.n recovery durati.n energy transport

ULF Waves Associ.ted wi.h Solar Wi.d Decelerati.n i. the Earth＇s Foreshock

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Chi.ese Physi.s Letters 2009年第11期26卷 258-261页

作者：符慧山曹晋滨杨彪 Lucek E Reme H dandouras i State Key Laboratory of Space Weather Center for Space Science and Applied Research Beijing 100190 Graduate Uni.ersi.y of Chi.ese Academy of Sci.nces Beijing 100049 Bei.i.g Uni.ersi.y of Aeronauti.s and Astronauti.s Beijing 100190 i.sti.ute of Space Physi.s and Appli.d Technology Peking University Beijing 100871 Blackett Laboratory Imperial College Prince Consort Road London SW7 2BZ UK Centre d'Etude Spati.le des Rayonnements 31028 Toulouse France

Characteri.ti.s of ULF waves associ.ted wi.h the solar wi.d decelerati.n i. the Earth＇s foreshock on 6-7 Apri. 2003 i. studi.d usi.g the wave telescope techni.ue. i. the satelli.e frame, the ULF waves are the left-handed polari.ed and quasi.anti.parallel propagati.g mode, wi.h a power peak at about 18.63mHz. The wave vector i. the GSE coordi.ates i. esti.ated to be k = （-4.29, 2.28, 1.21）×10^-4 km^-1, i. the solar wi.d frame, the frequency of waves becomes - 9.39 mHz after the Doppler shi.t correcti.n. The propagati.n di.ecti.n of the waves i. thus reversed and correspondi.gly the polari.ati.n of the waves becomes ri.ht-handed. The above-menti.ned characteri.ti.s of the ULF waves i. the solar wi.d frame i.di.ate that the ULF waves associ.ted wi.h the solar wi.d decelerati.n are the Alfven-whi.tler waves, whi.h have been frequently reported i. both the observati.ns and computer si.ulati.ns.

关键词： Plasma physi.s Envi.onmental and Earth sci.nce Astrophysi.s and astroparti.les

MHD and ki.eti. analysi. of flow bursts i. the Earth's plasma sheet

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Sci.nce Chi.a(Technologi.al Sci.nces) 2014年第1期57卷 55-66页

作者： MA YuDuan CAO Ji.Bi. FU Hui.han REME H. dandouras i. YANG JunYi.g WANG Zhi.i.ng TAO Dan YANG Ji.n School of Astronauti.s Beihang University SOA Key Laboratory for Polar Sci.nce Polar Research Institute of China Uni.ersi.y of Toulouse UPS-OMP IRAP Toulouse 31028 France The French Nati.nal Centre for Sci.nti.i. Research The Research Institute in Astrophysics and Planetology BP 44346F-31028 Toulouse cedex 4 France Nanji.g Uni.ersi.y of Aeronauti.s and Astronauti.s

i. an attempt to study the flow bursts i. the Earth＇s plasma sheet we select an event that took place on August 7, 2004 i. the expansi.n phase of a substorm, usi.g data from the geomagneti. i.dex, solar wi.d data, plasma and magneti. fi.ld observa- ti.ns from C1 Cluster satelli.e （the Cluster mi.si.n has 4 satelli.es） and from Double Star TC-1 satelli.e. i. MHD approach, TC-1 fi.stly observed the tai.ward flow, then the earthward, and fi.ally the flow altemated i. two di.ecti.ns. C1 fi.stly ob- served the earthward plasma flow, and then the tai.ward plasma flow. Before flow bursts are observed by TC-1 and C1, there are di.turbances i. local entropy wi.h thei. tai.ward local entropy larger than those of the earthward. The ki.eti. features of the plasma flow observed by C1 are si.i.ar to those i. MHD. However, ki.eti. characteri.ti.s of the plasma flow observed by TC-1 are far more than the descri.ti.n i. MHD. The i.adequacy mai.ly exi.ts i. two cases：（i. the fi.stly enhanced tai.ward flows gi.en i. MHD are found wi.hout si.ni.i.ant i.crease of the energeti. tai.ward flux; （i.） the almost stagnant flow i. MHD i. composed of the enhanced energeti. i.n flux i. both earthward and tai.ward di.ecti.ns. The earthward flow burst observed by TC-1 mi.ht be multi.le overshoots and rebounds. The earthward flow burst observed by C1 mi.ht be si.ply rebounded i. the near-Earth. The pulsati.n observed by C1 i. earli.r than that observed by TC-1 wi.h the former i.tensi.y less than that of the latter. After the energeti. i.n flux i. the tai.ward di.ecti.n i. si.ni.i.antly enhanced, the power spectrum i.tensi.y of the ULF wave commences to i.crease obvi.usly, whi.h may suggest that the stream i.stabi.i.y i. closely correlated wi.h ULF pulsati.ns.

关键词： MHD ki.eti. flux entropy

Multi.spacecraft observati.ns of earthward flow bursts

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Sci.nce Chi.a(Technologi.al Sci.nces) 2012年第5期55卷 1305-1311页

作者： MA YuDuan CAO Ji.Bi. REME Henry dandouras i.nni. DUNLOP Malcolm LUCEK Eli.abeth School of Astronauti.s Beihang UniversityBeijing 100191China SOA Key Laboratory for Polar Sci.nce Polar Research Institute of ChinaShanghai 200136China Centre d'Etude Spati.le des Rayonnements Toulouse 31028France RutherforAppleton Laboratory OxfordshireUK Blackett Laboratory Imperial College LondonLondon SW72AZUK

On the basi. of the plasma, electri. and magneti. fi.lds joi.tly observed by Cluster and the Double Star TC-i.spacecraft i. the Earth＇s magnetotai., we have i.vesti.ated the earthward flow bursts by i.troduci.g the momentum equati.n i. the X-di.ecti.n i. the i.eal condi.i.ns of magneto hydrodynami.s （MHD）. One earthward flow burst wi.h a peak i. excess of 500 km/s was selected, when the four spacecraft of Cluster were located around -16 RE and TC-1 was located around -10 RE i. the X-di.ecti.n. The i.ter-spacecraft di.tances i. Y and Z di.ecti.ns were smaller than the stati.ti.al spati.l scales of the bursty bulk flows. When the Y components of E and -VxB were compared, there was no clear breakdown of the frozen-i. condi.i.n duri.g the earthward flow burst. Wi.h the measured plasma and magneti. parameters from two spacecraft at di.ferent posi.i.ns i. the magnetotai., the X component of the pressure gradi.nt was calculated. Magneti. tensi.n was calculated usi.g the mag- neti. fi.ld measured at four poi.ts, whi.h could be compared wi.h the assumed constant i. the past research wi.h si.gle satel- li.e. When the pressure gradi.nt and the magneti. tensi.n were put i.to the MHD momentum equati.n, some samples of the earthward flow bursts were accelerated and some were decelerated. The braki.g process of the earthward flow burst was more compli.ated than what the past results had shown. The accelerated samples accounted for about one thi.d of the whole earth- ward flow bursts and di.conti.uously located among the decelerated elements. The ori.i.al si.gle earthward flow burst event mi.ht be spli. i.to several short flow bursts when i. was movi.g to the Earth. Our results may partly i.lustrate that the durati.n of fast flows duri.g three phases of substorm becomes short near the Earth. The results are consi.tent wi.h the past results that fast flows i.trude to places earthward the typi.al braki.g regi.n.

关键词： flow burst pressure gradi.nt magneti. tensi.n braki.g