極端紫外分光による 木星内部磁気圏の観測

68
極極極極極極極極極 極極極極極極極極極 極極極極極極極極極極 極極極極極極極極極極 2009 極 07 極 08 極 ISAS STP seminar 極極 / 極極極 / 極極極極

Upload: lucas

Post on 14-Feb-2016

94 views

Category:

Documents


0 download

DESCRIPTION

極端紫外分光による 木星内部磁気圏の観測. 2009 年 07 月 08 日 ISAS STP seminar 東大 / 吉川研 / 吉岡和夫. Contents. Introduction 極端紫外光( EUV )を用いた観測 EUV スペクトルを用いた温度・密度パラメタの導出 木星内部磁気圏  - 研究の動機 - 極端紫外分光器の開発 EXCEED 主鏡 回折格子 検出器 MCP with photocathode RAE 防護壁 Model spectrums 解析手法 EUV スペクトルを用いた電子温度、密度の導出 今後の課題 - PowerPoint PPT Presentation

TRANSCRIPT

  • 20090708ISAS STP seminar//

  • Chap. 0 : CONTENTS*ContentsIntroductionEUVEUV--

    EXCEEDMCP with photocathodeRAEModel spectrums

    EUV

    CASSINI*

  • *ContentsIntroductionEUVEUV--

    EXCEEDMCP with photocathodeRAEModel spectrums

    EUV

    CASSINIChap. 0 : CONTENTS

    Chap. 0 : CONTENTS

  • MCPRAEEUV2EUVMCP107RAE

    SELENE/UPI/TEX3MCP ~0.1 pC7 bits128128 pixelsRAE : 1~100 k Ohm*MCP + RAE (PHEBUS/BBM)MCP + RAEChap.2 :

    Chap.2 :

  • MCPRAEEUV~10bits~RAE (Resistive Anode Encoder)+RuO2121(x,y)*LLChap.2 :

    Chap.2 :

  • 2RAE MCP~~*Chap.2 :

    Chap.2 :

  • Chap.2 : *RAE10 bits (1024 * 1024 pixels)SELENE/UPI/TEX7 bits

    (Point)RAEMCP, 10 pF1110 bitsRAE1 *

  • Chap.2 : *RAE 11mm (minimum)

    RuO2 [s]10pFAmptek/A2252.4 us10 k Ohm*

    RAE500 k100 k 50 k 10 k 5 k 1 k 10 pF18.13.611.790.420.180.043 pF6.931.380.700.100.070.02

  • Chap.2 : *RAE 2 -100 OhmRAEA225FRAE10 k Ohm0.5 us200 300 OhmRAE1mm, 10 k Ohm()*

  • Chap. 0 : CONTENTS*ContentsIntroductionEUVEUV--

    EXCEEDMCP with photocathodeRAEModel spectrums

    EUV

    CASSINI*

  • *EUVEUV (Extreme Ultraviolet)30 150 nm (8 40 eV)FUVHeII 30.4, NeI 73.4, SIII 68.0 nm, HI 121.6 nm, etc.

    EUVVoyager 1, 1977, He, H, OEUVE, 1992, HeIPlanet-B, 1998, (HeII)Cassini, 2004, (HeII)SELENE/KAGUYA, 2007~, (HeII, OII)EUVChap. 1 : INTRODUCTION

    Chap. 1 : INTRODUCTION

  • *EUVEUV 24Chap. 1 : INTRODUCTION

    Chap. 1 : INTRODUCTION

  • *~~* ** 1 AU = 1.5E+8 km ~ 2000 RJ Chap. 1 : INTRODUCTION

    71500 km6400 km9h55min24 h*420,000 nT31,000 nT [1 ton/s]5.1 AU**1 AU

    Chap. 1 : INTRODUCTION

  • *10RJ5.9RJ58.2 km/s100 eV5 eV100 eVNeutrals(Pick up)Ions(S+, O+, etc.)Core electronsUV radiationTransportFast neutralHot electrons???Chap. 1 : INTRODUCTION

    Chap. 1 : INTRODUCTION

  • *Voyager 1, 2GALILEOCASSINIIUE, HUT, HST

    ~eVCASSINI/UVISEUVSteffl et al., 2004

    CASSINI1Voyager Sitteler and Strobel, 1987eV100 1000 eV1Voyager 1Chap. 1 : INTRODUCTION

    Chap. 1 : INTRODUCTION

  • Chap. 0 : CONTENTS*ContentsIntroductionEUVEUV--

    EXCEEDMCP with photocathodeRAEModel spectrums

    EUV

    CASSINI*

  • *EUVEXCEED-2012110.3 nm FWHM, 10 arcsec.

    EXCEEDChap. 2 : EUV

    MCPRAE0.3 nm FWHMRAE10 30 SN

    Chap. 2 : EUV

  • *~~ 2(60 um)

    20cm, 5.4, F8F/85.4

    Pt, Sic, SiEXCEEDPt02% @30.4 nm22% @58.4 nm15% @83.4 nmSi---% @30.4 nm02% @58.4 nm15% @83.4 nmSiC00% @30.4 nm13% @58.4 nm30% @83.4 nm

  • *CVD-SiC3CVD-SiCCVD(SiO2, H2, CH4, etc.SiCSiC0.5 nmCVD-SiC

  • *CVD-SiC2CVD-SiC30 50%

  • *10 arcsec, 0.3 nm FWHM+160 145 nm

    +1+1

    CVD-SiC

  • *CVD-SiC+18, 15, 20, 22, 26, 39 nm+122 nm

  • Chap.2 : *MCP (Micro channel plate)MCP10um2*

  • CsICsI, KBr1330~84 nm105~135 nm201.5102*

    30-84 nm105-135 nmCsI / Bare1.5 - 25 - 80

  • *EXCEEDCASSINI/UVIS Esposito et al., 1996EXCEEDEXCEEDCASSINI/UVIS3003

  • Chap. 0 : CONTENTS*ContentsIntroductionEUVEUV--

    EXCEEDMCP with photocathodeRAEModel spectrums

    EUV

    CASSINI*

  • *EXCEEDEXCEEDCHIANTI6.3130 * 30EXCEED

  • *SII, SIII, OII, etc.Aij1 cm2-Nj

  • *EXCEED1SIII680ASIII700ASIII1191ASIII1191ATE= 0.5 eV, t = 1 h

  • *EXCEED1SIII680ASIII700ASIII1191ASIII1191ATC = 5 eVTH = 100 eVfH= 1 %, t = 1 h

  • *EXCEED~100RJ10~1001TE, TH, FH, etc.

  • RAEPhotocathode

    EXCEEDS/N

    Cassini

    *

  • *

  • *

  • *

    ORBIT []Pioneer 10P10197231973Flyby1.8 RJPioneer 11P11197341974Flyby0.5 RJVoyger 2V21977819797FlybyVoyger 1V11977919793FlybyEUV600 - 1700International Ultraviolet ExplorerIUE197811978 - 1996GSO ~30000 km)UV1150 - 1980 1800 - 3200Einstein spacecraftHEAO-21978121978 - 1981Earth500 kmX-ray2 - 50GalileoGLL1989101995 - 2000UVS, VISPWS, PLSHubble Space TelescopeHST199041990 -Earth ??? KmSTIS, UVROSATRST199061991, 1992Earth580 kmX-rayUlysesesULS1990101992FlybyHopkins Ultraviolet TelescopeHUT1199012199012Space shuttle ColumbiaEUV, FUV912 - 1850 415 - 912(2nd)&Astro-1EUVEEUVE199261992 - ?? Earth~350 kmHopkins Ultraviolet TelescopeHUT21995519955Space Shuttle EndeavourFUV820 - 1840Astro-2CASSINICAS1997102000-2001Flyby5RJEUV, FUV584 - 1120 1100 - 1750 ?EXCEED20132013-2014Earth1000 kmEUV584 - 1412

  • r [] R [/mm] a [mm]2aI [A/mm]AB*

  • *21C : C_MCP = R1 : R20

  • *1pF1pF1pFF.G.1 pFV, fV1V2

  • *

  • * CVD-SiC coated mirror and grating -0.3~0.5 nm10.4 degree.+14

  • *1979Voyager 1/UVS

    HSTUV15RJClarke et al., 1998

    Bhattacharya and Thorne 200115 RJ

  • *10RJ15 30 RJLoss cone2 erg/cm2/sec18.4RJ40 100 erg/cm2/sec~ 100 erg/cm2/sec15 ~ 29 keV18.4RJ

  • *Control of Jupiters radio emission and aurorae by the solar wind, D.A. Gurnett et al., 2002, Nature2000CASSINIGalileoCASSINI: RPWS, MAG, CAPS, UVISGALILEO: PWS

  • *CASSINI0.5 5.6 MHz

    CASSINIGALILEO0.5 5.6 MHz19h55m32GALILEO1GALILEO

  • *1CASSINI/MAGCASSINI/CAPSGALILEO: PWS1CASSINI16721 km/sCASSINI/UVIS110.8 113.1

  • *2BGALILEO/PWSTrapped continuum radiation fp or 13GALILEO528 km/sLow-mach-numberInterplanetary shock

  • *

  • *Dungey cycleIMFGalileo150~200RJ (Joy et al., 2002)

    1500RJ10%

    1000Kivelson and Southwood 2005, JGR

  • *10McComas and Baganel., 2007IMFOPEN MAGNETIC FLUXIMFCLOSED FLUX10RJ2

  • * UVISParkinson et al., 2006 HeH58.4 nm

  • *

    &19801990

    CASSINIGALILEO2000EXCEED

  • *NCT

  • *~ 70 RJ

    3< 10 RJ10 40 RJ> 40 RJ

    Khurana et al., 2003

  • *Plasma
  • *~5.9 RJ100 eV5 eVFast neutral: 400 RJ Mendillo et al., 1990

    Energy crisisVayager1PWS

  • *Neutrals(Pick up)Ions(S+, O+, etc.)Core electronsUV radiationTransportFast neutralPick up Shemansky 1988, Delamere and Bagenal 2003 CHIANTI Shemansky et al., 1988, Delamere and Bagenal 2003

  • *S, S+, S++, S++, O, O+, ele.

  • *Energy source and lossElectron impact ionization: Voronov 1997 Recombination: Michael and shull 1982Charge exchange reactionSmith and Strobel 1985Te=5 eV, Ts=100 eV, Ns=500, Ne=2000 1 eV/s/cm^3

  • *Electron temperatureCoulomb collisionRadiationTransportCoulomb interactionNs=500 /cm^3, Ts=100 eV, Ne=2000, Te=5 eV 0.05 [eV/cm^3/sec]

  • *Coulomb collisionRadiationTransportRadiative rate coefficient

    CHIANTI

    Ns=500 /cm^3, Ne=1000, Te=5 eV 0.5 [eV/cm^3/sec]Electron temperature

  • *Neutral source rate O/S ratioHot electron fractionHot electron temperatureTransport time Voyager1, 2 and Cassini

    Voyager 1neS+/neS++/neS+++/neO+/neO++/neTiVoyager 2neS+/neS++/neS+++/neO+/neO++/neCassinineS+/neS++/neS+++/neO+/neO++/nePUV

  • *S, S+, S++, S+++ , O, O+, O++

  • *Voyger1, Voyager2, Cassini

    Voyager 1Voyager 2CassiniNeutral source (10-4 cm-3s-1)10307O/S ratio 4.04.01.7Hot electron fraction (%)0.230.120.3Hot electron temperature (eV)60060040Transport time (days)502350

  • *Neutrals(Pick up)Hot electronsUV radiationTransportFast neutralIons(S+, O+, etc.)Core electrons

    Voyager 1Voyager 2CassiniEnergy flow (10-4 eV cm-3s-1)0.411.120.66S ionization 121614S charge exchange15138O ionization793O charge exchange485115Hot electron thermal coupling181160Fast neutrals20405Transport10186UV radiation704289

  • *EXCEED12

    160 cm

  • *

    Voyager1, Voyager2, Cassini

    EXCEED

  • *Hot electron 60%UV90%

  • *

    ******a=r/R