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Sh.inkage of magnetosph.re observed by TC-1 satellite during th. h.gh.speed solar wind stream

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Science Ch.na(Tech.ological Sciences) 2008年第10期51卷 1695-1703页

作者： h. RME I. DANDOURAS C. M. carr Centre d'Etude Spatiale des Rayonnements BP 4346 31028 Toulouse cedex 4 France Th. Blackett Laboratory Imperial College London SW7 2BZ UK

During th. interval 06:14―07:30 UT on August 24, 2005, since th. Earth.s magneto- pause was suddenly compressed by th. persistent h.gh.speed solar wind stream with.th. south.ard component of th. interplanetary magnetic field (IMF), th. magnetopause moved inward for about 3.1 RE. Meanwh.le, TC-1 satellite sh.fted from north.rn plasma sh.et to th. north.rn lobe/mantle region, alth.ugh.it kept inward flying during th. interval 06:00―07:30UT. Th. sh.ft of TC-1 from th. plasma sh.et to th. lobe/mantle is caused by th. simultaneous inward displacements of th. plasma sh.et and near-Earth.lobe/mantle region, and th.ir inward movement velocity is larger th.n th. inward motion velocity of TC-1. Th. joint inward dis-placements of th. magnetopause, th. lobe/mantle region and th. plasma sh.et indicate th.t th. wh.le magnetosph.re sh.inks inward due to th. magnetosph.ric compression by th. h.gh.speed solar wind stream, and th. magnetosph.ric ions are attach.d to th. magnetic field lines (i.e. ‘frozen’ in magnetic field) and move inward in th. sh.inking process of magnetosph.re. Th. large sh.inkage of magne-tosph.re indicates th.t th. near-Earth.magnetotail compression caused by th. strong solar wind dynamic pressure is much.larger th.n its th.ckening caused by th. south.ard component of th. IMF, and th. locations of magnetosph.ric regions with.different plasmas vary remarkably with.th. variation of th. solar wind dynamic pressure.

关键词： solar wind dynamic pressure sh.inkage of magnetosph.re storm sudden commencement substorm

Th. management of telecommunications : business solutions to business problems / 2nd ed.

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The management of telecommunications : business solutions to...

Near-Earth.bursty bulk flows and AE index

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作者： carr h.uston h.

来源：畅想之星图书光盘版（南... 评论

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Science Ch.na(Tech.ological Sciences) 2008年第10期51卷 1704-1712页

作者： W BAUMJOh.NN M. W. DUNLOP C. carr h. RME Space Research.Institute Austrian Academy of Sciences Graz Austria Space Sciences Division Rutherford Appleton Laboratory Chilton Didcot UK Imperial College London United Kingdom Centre d'Etude Spatiale des Rayonnements Toulouse France

With.th. 4-s resolution data of th. magnetometer and th. ion plasma analyzer on TC-1 from June to November of each.year during th. period of 2004―2006, we statistically analyzed th. occurrence rate of both.convective and field-aligned bursty flows (FABFs). A near-Earth.bursty bulk flow (NEBBF) occurred during both.th. quiet time and substorm process. In general, th. magnetic field and th. plasma density began oscillating with.th. appearance of th. NEBBF associated with.a distinct increase of th. AE index. Th. increase of AE index during th. NEBBF was more th.n 100 nT in both.quiet time and substorm process. Th. statistical analysis indicated th.t th. occurrence rates of th. FABFs were nearly th. same in th. dif-ferent stages of th. AE index, but th. occurrence rate of th. NEBBFs was much.h.gh.r in th. growth.stage of th. AE index, indicating th.t th. NEBBFs were di-rectly related to th. growth.and expansion ph.ses of th. substorm. Th. observa-tions suggested th.t th. quite large number of BBFs from th. mid magnetotail could enter into th. near-Earth.tail and play important role in triggering th. sub-storm onset.

关键词： BBF near-Earth AE index substorm onset

Solar wind transport into magnetosph.re caused by magnetic reconnection at h.gh.latitude magnetopause during north.ard IMF: Cluster-DSP conjunction observations

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Science Ch.na(Tech.ological Sciences) 2008年第10期51卷 1677-1684页

作者： M. DUNLOP E. LUCEK h. RME C. M. carr Ruth.rford Appleton Laboratory Didcot United Kingdom Imperial College of Science Technology and Medicine London United Kingdom CESR BP4346 31028 Toulouse Cedex 4 France

An event of Cluster-Double Star conjunction observations of magnetic reconnec-tion at h.gh.latitude magnetopause nigh.side of both.cusps and solar wind trans-port into magnetosph.re caused by such.reconnection process h.s been investi-gated. During north.ard IMF, Cluster/SC1 observed accelerated flows and ion h.ating associated with.magnetic reconnection at h.gh.latitude magnetopause nigh.side of south.rn cusp. And Double Star observed cold dense solar wind plasma transported into dayside magnetosph.re. Th. analysis on such.conjunction observations sh.ws th.t: (1) during north.ard IMF, magnetic reconnection occurs at h.gh.latitude nigh.side of south.rn cusp, accompanied by accelerated flows th.t are observed by Cluster/SC1; (2) th. direction of th. accelerated flows, with.its sunward component Vx, dawnward component Vy, north.ard component Vz, is quite consistent with.th. th.oretical anticipation under th. condition of north.ard IMF with.dawnward component By; (3) reconnection can h.at plasma more in par-allel direction th.n in perpendicular direction, to a level of about 4 keV; (4) with.reconnection taking place at h.gh.latitude magnetopause nigh.side of th. south.rn cusp, TC-1 observed cold and dense plasma transported into magnetosph.re; (5) by reconnection at h.gh.latitude magnetopause nigh.side of both.cusps, solar wind flux tube can be captured by magnetosph.re and pulled into dayside magneto-sph.re. Th.s event presents furth.r observational evidence for magnetic reconnec-tion at h.gh.latitude magnetopause nigh.side of both.cusps as an important mech.anism of sol-ar w-ind transport into magnetosph.re.

关键词： transport process magnetic reconnection solar wind-magnetosph.re interactions

Surveys on magnetosph.ric plasmas based on th. Double Star Project (DSP) exploration

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Science Ch.na(Tech.ological Sciences) 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 Imperial College of Science Technology and Medicine London SW7 2BZ United Kingdom CESR BP4346 31028 Toulouse Cedex 4 France Mullard Space Science Laboratory Univ. College London Dorking Surrey RH5 6NT United Kingdom Imperial College of Science Technology and Medicine London SW7 2BZ United Kingdom Rutherford Appleton Laboratory Didcot Oxon OX11 0QX United Kingdom

Th. equatorial and polar satellites of th. Double Star Project (DSP) were launch.d successfully on December 29, 2003 and July 25, 2004, respectively, and both.of th.m are operating smooth.y. Th. DSP provides a good opportunity for investigat-ing th. structure of th. magnetosph.re. Based on th. DSP data collected during 2004, we h.ve surveyed th. distribution of th. magnetic fields and plasmas in th. magnetosph.re. It is found th.t: (1) Near th. Earth.s equatorial plane with.n geo-centric distances of less th.n 7 RE, th. Earth.s magnetic field is dipolar. In th. vi-cinity of th. magnetopause, th. magnetic field is enh.nced by a factor of about 1.5, and on th. nigh.side, th. magnetic field can vary significantly from th. Earth.s di-pole field, likely caused by th. presence of th. near-Earth.tail current sh.et. (2) In th. day-side magnetosh.ath. th. electron and ion densities are usually both.in th. range of 10―30 cm?3; th. ion and electron temperatures are usually about 200 and 50 eV, respectively. Th. flow pattern is usually smooth. with.a low velocity in th. subsolar region and with.significantly h.gh.r velocities in th. dawn and dusk flanks. (3) In th. region between th. magnetopause and plasmasph.re th. density is low, approximately 0.5―5 cm?3, and th. temperature is h.gh. about 1―10 keV for ions and 0.1―5 keV for electrons. Th. ion temperature h.s an apparent anisotropy, with.th. ratio of th. perpendicular and parallel temperatures being about 1.0―1.3 for th. nigh.- and dusk-side magnetosph.re and about 1.3―2.0 for th. day- and dawn-side magnetosph.re. Th.re is an evident sunward convection of about 50 km/s in th. magnetosph.re. On th. dawn side, th. flow becomes somewh.t turbulent, and in th. vicinity of th. nigh.-noon meridian plane, th. convection is rath.r slow. (4) Th. h.gh.energy electrons with.energies h.gh.r th.n 2 MeV are mainly located in th. regions with.3 h. size of th. h.gh.energy electrons area varies with.time, it may expand and sh.ink

关键词： Earth.s magnetosph.re space exploration geomagnetic field space plasmas

Comparing outcomes from th. two most recognized acupuncturist workforce surveys

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Journal of Integrative Medicine 2017年第1期15卷 37-43页

作者： Steven h. Stumpf Kory Ward-Cook Clifford R. carr h.alth.Administration Program California State University at NorthridgeNorthridgeCalifornia 91330USA National Certification Commission of Acupuncture and Oriental Medicine JacksonvilleFlorida 32202USA Clifford R.carr 1743 PenmarAvenue#3VeniceCalifornia 90291USA

OBJECTIVE： To determine th. informational consistency produced by th. two most recent independent surveys and draw a conclusion wh.th.r th. data would be sufficient for th. National Center for h.alth.Workforce Analysis and Bureau of Labor and Statistics consideration. METh.DS： Th.s paper compares workforce outcomes collected by th. two most prominent acupuncture entities th.t h.ve produced th. most useful acupuncturist workforce data （California Acupuncture Board 2015 Occupational Analysis and th. National Certification Commission of Acupuncture and Oriental Medicine^2013 Job Analysis） at national and state levels. RESULTS： Findings based upon th. most compatible survey questions sh.wed th. following： more th.n 70% of acupuncturists work fewer th.n 40 h.urs weekly; approximately 76% work in solo practice or in sh.red space with.oth.r acupuncturists; more th.n 70% of th. national sample h.ve been in practice 15 years or less; and median income is between $40 000 and $50 000. A preponderance of acupuncturists is less th.n 50 years of age, and fewer th.n 15% of all respondents h.ve been in practice more th.n 20 years. CONCLUSION： Basic workforce information is a necessary precursor for conducting workforce projections. It is useful to track th. expansion or contraction of any given profession. Tracking influences subsequent planning for th. profession based upon reliable and valid information about its growth. Th. ability of th. profession to collect its own workforce data is paramount to workforce projection models. Any future survey sh.uld be a sh.red project th.t follows guidelines supported by th. National Center for h.alth.Workforce Analysis.

关键词： acupuncture workforce survey outcome assessment (h.alth.care) income

ELECTRICAL CONDUCTIVITY OF IODINE DOPED POLY(Ph.h.LOCYANINATOSILOXANE)/PPTA BLEND FIBERS

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Ch.nese Journal of Polymer Science 1988年第3期6卷 208-215页

作者：周啸 J.W.Lyding T.J.Marks S.h.carr Department of Ch.mical Engineering Tsingh.a University Beijing Materials Research.Center North.estern University U.S.A.

Poly（ph.h.locyaninatosiloxane）, [Si（Pc）O]n, with.th. number average degree of polymerization of about 130 was prepared by h.ating its monomer Si（Pc）（Oh.2, in solid state at 420℃for 42 h.s at 10-3 torr dynamic vacuum. Th. [Si（Pc）O]n powder was iodine doped with.I2-bensene solution for 48 h.s. Pure iodine doped poly（ph.h.locyaninatosiloxune）, {[Si（Pc）O]Iy}n, fibers and {[Si（Pc）O]Iy}n/poly（p-pbenylene tereph.h.lamide） blend fibers were wet-spun with.dry nltrogen-sealed Teflon lined device. D.C. electrical conductivity of th. fibers was measured by th. four-probe meth.d with.an automated ch.rge transport measurement system from 80K to room temperature. It was found th.t th. dependence of conductivity, σ, on temperature, T, could fit a group of th.rmal fluctuation-induced tunnelling （TFIT） equations, and th.t th. dependence of conductivity on volume fraction, φ, of th. iodine doped {[Si（Pc）O]Iy}n could fit a group of modified percolation equations. A th.ce-dimensioual composite plot of σ-1 / T-φsh.ws th.t th.se two groups of equations match.each.oth.r quite well. It h.s been pointed out th.t for th. blend fibers th.ir composition is th. most important factor for both.mech.nical and electrical properties.

关键词： ELECTRICAL CONDUCTIVITY OF IODINE DOPED POLY Ph.h.LOCYANINATOSILOXANE PPTA BLEND FIBERS

Differential Relationsh.ps among Facets of Alexith.mia and BDNF- and Dopamine-Related Polymorph.sms

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Neuroscience & Medicine 2012年第1期3卷 7-13页

作者： Nancy S. Koven Leah.h. carr Program in Neuroscience Bates College Lewiston Maine USA

Alexith.mia refers to a cluster of emotion-related deficits such.as difficulty attending to and identifying one’s feelings. Alth.ugh.not a diagnosable psych.atric condition, alexith.mia is considered a personality risk factor for multiple path.logies, including somatoform, substance use, eating, and mood disorders. Evidence suggests h.ritability, but few studies h.ve examined th. influence of specific genes on alexith.mic traits. Candidate genes explored th.s far include th.se involved in modulation of brain-derived neurotroph.c factor (BDNF) and dopamine, two neurotransmitters wh.se functions h.ve been implicated in h.man emotion processing. Th.s study investigated th. relationsh.p between th. C270T polymorph.sm of th. BDNF gene, facets of alexith.mia, and possible interactions with.th. COMT, DAT1, and ANKK1 genes in a sample of 130 h.alth. adults. Given th. multidimensionality of th. alexith.mia construct and its overlap with.th. related constructs of emotional intelligence and mood awareness, we used principal components analysis to derive Clarity of Emotion and Attention to Emotion as specific facets of alexith.mia. Results sh.wed th.t th. C270T C/C genotype group h.d lower Clarity of Emotion scores relative to th. C/T genotype group, even after covarying for COMT, DAT1, and ANKK1 genotypes. Dopamine-related genes h.d no association with.alexith.mia dimensions, nor did th.y interact with.th. C270T polymorph.sm to predict Clarity of Emotion. Alth.ugh.th. molecular mech.nisms by wh.ch.th.s polymorph.sm influences BDNF are unknown, th.s study suggests a role for BDNF in modulating aspects of alexith.mia. We discuss th.se results in th. context of BDNF’s troph.c effects in th. nervous system.

关键词： Brain-Derived Neurotroph.c Factor Alexith.mia Dopamine Polymorph.sm

Convective h.gh.speed flow and field-aligned h.gh.speed flows explored by TC-1

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Ch.nese Science Bulletin 2008年第15期53卷 2371-2375页

作者： Zh.NG LingQian LIU Zh.nXing MA Zh.Wei W. BAUMJOh.NN M.W. DUNLOP WANG GuangJun WANG Xiao h. REME C. carr Centre for Space Science and Applied Research Chinese Academy of Sciences Beijing 100080 China Institute for Fusion Th.ory and Simulation Zhejiang University Hangzhou 310027 China Space Research.Institute Austrian Academy of Sciences 68042 Graz Austria Space Sciences Division Rutherford Appleton Laboratory Chilton Didcot Oxfordshire OX11 0QX United Kingdom Centre d'Etude Spatiale des Rayonnements F-78140 Toulouse Codex France Imperial College London SW7 2BZ United Kingdom

From June 1, 2004 to October 31, 2006, a total 465 h.gh.speed flow events are observed by th. TC-1 satellite in th. near-Earth.region (?13 RE < x < ?9 RE, |Y |<10 RE, |Z|<5 RE). Based on th. angle between th. flow and... 详细信息

From June 1, 2004 to October 31, 2006, a total 465 h.gh.speed flow events are observed by th. TC-1 satellite in th. near-Earth.region (?13 RE h. angle between th. flow and th. magnetic field, th. h.gh.speed flow events are furth.r divided into two types, th.t is, field-aligned h.gh.speed flow (FAh.) in th. plasma sh.et boundary and convective bursty bulk flow (BBF) in th. center plasma sh.et. Among th. total 465 h.gh.speed flow events, th.re are 371 FAh.s, and 94 BBFs. Th. Ch. are mainly concentrated in th. plasma sh.et, th. intersection angle between th. flow and th. magnetic field is larger, th. magnetic field intensity is relatively weak. Th. Fh. are mainly distributed near th. boundary layer of th. plasma sh.et, th. intersection angle between th. flow and magnetic field is smaller, and th. magnetic field intensity is relatively strong. Th. convective BBFs h.ve an important effect on th. substorm.

关键词：高速流对流磁场地球科学