論文紹介 「 Chromosphereic Diagnostics 」 (Uitenbroek, ASP Conf. Series, 2006, vol.354,...

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Chromosphereic Diagnostics (Uitenbroek, ASP Conf. Series, 2006, vol.354, 313-323). NAOJ/ ) SXT Seminar 2008/09/22. Abstract. formation height Eddington-Barbier Relation, contribution function, response function 3 - PowerPoint PPT Presentation

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  • Chromosphereic Diagnostics (Uitenbroek, ASP Conf. Series, 2006, vol.354, 313-323)NAOJ/)

    SXT Seminar 2008/09/22

  • Abstract formation height Eddington-Barbier Relation, contribution function, response function 3non-LTE condition response function NaID1, CaII, Hresponse funcitonH

  • 1. The Chromosphere - 1HHcrimson emissionBalmer line narrow wavelength band

    hydrodynamic force magnetic force

  • 1. The Chromosphere - 2emission1VAL modelVernazza et al., 1973, 1976, 1981

    butVAL model (Carlsson & Stein, 1994, 1997, 2002)

  • 1.1 Observing Considerations pressure scale height, sound speed, sound crossing time

    exposure time

  • 1.2 Observable - 1lineoptically thick

    1,UV >160nmDoppler shift intensity, velocity modulationflux

  • 1.2 Observable - 2 2, UV linesUVfluxDoppler shiftmodulation

    3, CaII&K, HI, MgI, NaID, HI, CaII IR triplet, HeI 1083 2

    4

  • 2. Estimation for Formation HeightRadiative Transfer Equationintensity

    I : intensitys : path length emission coefficient absorption coefficientS : source funciton : optical depth

  • 2.1 Estimate with Eddington - Barbier Relation - 1Source function S=a+b I=a+b=S(=1) intensity=1source function =1

    NaID1 (=589.597 nm) source function

  • 2.1 Estimate with Eddington - Barbier Relation - 2lowNonlinearhighLinier

  • 2.2 The Contribution Function - 1 z

    C(z)atmosphere intensitycontribution functionNaID1 contribution function (quiet Sun1

  • 2.2 The Contribution Function - 2Far wing: photosphereCore: Higher Layer @800km100200kmcontribution

  • 2.2 The Contribution Funciton - 3 z C(z) zd/dz intensity

    Eddington-Barbier relationformation heightintensity source function contribution function

  • 2.3 The Response Function - 1Contribution Function accounts foropacity, source function

    non-LTE condition excitation, de-excitation, scattering Response Function

  • 2.3 The Response Function - 2Response Function R(z) Physical Property X(z)

    Stokes (I,Q,U,V)

    Response Function

  • 2.3 The Response Function - 3X(z)Hstep1(zz)

  • 2.3 The Response Function - 43Eddington-Barbier RelationContribution FunctionSource FunctionOpacityResponse Function

    line formation height

  • 3. Comparison of Formation Height Estimates for CaII K - 1formation heightsestimate continium,K1,K2(reversal),K3 lineEddington-Barbier relation, contribution function, response funcionquiet Sunplane-parallel

    continium,K1contribution function response functionK2,K3:response functioncontribution function

  • 3. Comparison of Formation Height Estimates for CaII K - 2Contribution FunctionResponse FunctionEddington - Barbier Relation

  • 3. Comparison of Formation Height Estimates for CaII K - 3Source FuncrtionPlanck Function

  • 3. Comparison of Formation Height Estimates for CaII K - 4contribution function non-LTE conditionformation height

    continium,K1700kmLTE condition K2,K3700km non-LTE condition

    contribution functionformation height

  • 4. Response of Chromospheric Lines to Magnetic Fields - 1non-LTE conditionLTE condition

    Schaffenberger (2006)Stokes I,V Response FunctionModel FALC1000G

  • 4. Response of Chromospheric Lines to Magnetic Fields - 2 Physical PropertyX(z)

    CaII 854.21nm Stokes I,V Response Function Non-LTE conditionStokes V Response Function

  • 4. Response of Chromospheric Lines to Magnetic Fields - 3

  • 4. Response of Chromospheric Lines to Magnetic Fields - 4500800kmcircular polarization8001100kmcircular polarization

  • 4. Response of Chromospheric Lines to Magnetic Fields - 5

    1B>0234opacity5optical depth path length6formation height 7source function

  • 4. Response of Chromospheric Lines to Magnetic Fields - 6500800kmsource function CP 8001100kmsource function CP Source FunctionPlanck Function=1

  • 4. Response of Chromospheric Lines to Magnetic Fields - 7Na I D2Stokes IV response function

    Stokes V response function CaII response function

  • 4. Response of Chromospheric Lines to Magnetic Fields - 8response function

  • 4. Response of Chromospheric Lines to Magnetic Fields - 9

    1Zeeman splitting line core2opacity3path length4formation height 5intensity

  • 4. Response of Chromospheric Lines to Magnetic Fields - 10500km1000kmtail

  • 5. Na I D Dopplergram in a Two-Dimensional Atmosphere - 1Na I D2

    1, filter positionline center 7.5pmfilter function7.5pm2intensity

  • 5. Na I D Dopplergram in a Two-Dimensional Atmosphere - 2BlueshiftRedshift 3intensityresponse function

    4NaID2200600km

  • 5. Na I D Dopplergram in a Two-Dimensional Atmosphere - 3

  • 6Response Functions of H to temperature and velocity - 1HHH10eVHHHHintensity

  • 6Response Functions of H to temperature and velocity - 2HStokes Iresponse function Carlsson & Stein, 2002)

    WingphotosphereintensityCoreupper photosphere intensity

  • 6Response Functions of H to temperature and velocity - 3 Response Function Component

  • 6Response Functions of H to temperature and velocity - 4Coreresponse function

    12n2(H)3Hopacity4path length5line formation height 6source functionintensityS

  • 6Response Functions of H to temperature and velocity - 5Hresponse function

    profileblueshiftblue wing (negative response)=intensityred wing (positive response)=intensity

  • 6Response Functions of H to temperature and velocity - 6

  • 6Response Functions of H to temperature and velocity - 7response function500kmheightfine structureHfiltergram

    (5001000km )fine structure

  • 7. Conclusions - 1Contribution Function formation height over estimate LTE, non-LTE

    Response Function source function

  • 7. Conclusions - 2line formation estimate transfer equation line formation

    HStokes I response function Gudisken,2006)