REPRESENTATION OF PLASMA TEMPERATURES IN IRI

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Presentation transcript:

REPRESENTATION OF PLASMA TEMPERATURES IN IRI Vladimir Truhlik Department of the Upper Atmosphere Institute of Atmospheric Physics, Academy of Sciences of the Czech Republic Praha, Czech Republic Email : vtr@ufa.cas.cz

Outline Introduction Tools Data Theoretical model Plasma temperatures Theory and basic processes Representation in IRI Electron temperature Ion temperature Swarm, LP data, access Conclusions COSPAR CBW

Introduction Knowledge of characteristics of ionized part in the Earth‘s outer atmosphere is important for studying of many phenomena especially propagation of electromagnetic signals (artificial – GPS; natural - VLF - whistlers, emissions etc.) Most important parameters which we study: Electron density (Ne) (propagation of radio waves) Ion composition (e.g., waves - whistler mode – LHR Lower Hybrid Resonance – important mean ion mass) Plasma temperatures (thermal balance, important for transfer of energy, scale height etc.) Electron temperature (Te) Ion temperature (Ti) Drifts etc. COSPAR CBW

IRI model Ne electron density – parameter of prime interest Electron temperature, ion temperature, ion composition (O+, H+, He+, molecular ions), drifts, ionospheric electron content (TEC), F1 and spread-F probability COSPAR CBW

Tools – data Data base – satellite data All available Te satellite data (source mainly NSSDC, ISAS, and PIs of individual experiments) Year-altitude coverage of the data sets include in our data base. The curve at the top shows the solar 10.7 cm radio flux (F10.7 index – 3 months average). COSPAR CBW

Tools – model Field Line Interhemispheric Plasma (FLIP) flow model (e.g. Richards, 2001; Richards, 2002) Includes: Continuity and momentum equations along the field line for O+, H+, He+, and N+. Energy balance equations for electrons and ions. Geometry of tilted offset dipole Two stream photoelectron model Photochemical equilibrium below 500km for ions NO+, O2+, N2+, O+(2P), and O+(2D) Continuity and momentum equations for minor neutral species NO, O(1D), N(2D), and N(4S) from 100 to 500km in each hemisphere ExB drift Inputs: EUV from EUVAC model Horizontal winds from HWM model or from equivalent winds obtained from measured hmF2 Neutral densities and temperature from the MSIS model Equatorial drift from e.g., Fejer-Scherliess model COSPAR CBW

Ionospheric plasma Ionosphere-plasmaphere system, part of the inner magnetosphere (interacts with regions below and above) Ionization of neutral atmosphere by solar EUV or energetic particles precipitation Energy of particles<1eV, high density (up to 1013 m-3) Quasi-neutrality Strong solar control, transport along magnetic field lines (upper ionosphere F2 region, topside ionosphere, plasmasphere, high latitude region) ExB drifts (equatorial region, high latitudes) COSPAR CBW

Plasma temperatures Thermal motion of particles (electrons and ions) E=3/2kT Electron temperature (Te) Ion temperature(s) Temperature of neutral particles – important (Tn) up to >500km COSPAR CBW

Plasma temperatures Equation of energy balance (for particle i – ions or electrons) n-density T-temperature k-Boltzmann constant κ- (kappa) thermal conductivity Q-source and loss of energy A – cross section of the flux tube COSPAR CBW

Electron temperature Equation of thermal balance (day, night – steady state - neglect changes with time) Qe – heating (from photoelectrons) local <350km non-local plasmaspheric Le – cooling – very complex – energy loss: <350km neutral particles O, N2(r,v), O2 (r,v) topside with ions O+, H+, He+ (Coulomb) Ke – thermal conductivity I – inclination of the geomagnetic field FLIP electron cooling rates in the equtorial region up to 350km as a function of altitude for various cooling terms (Coulomb —, rN2 —, rO2 —, vN2 —, vO2 —, fsO ……, O1D …..). Coulomb cooling in the topside is dominant COSPAR CBW

Electron temperature – altitude profiles in topside and plasmasphere Thermal conductivity Te profile – constant heat flux Te0, G0 – electron temperature and gradient (e.g. at 500km) LSA HSA COSPAR CBW

Ion temperature Equation (neglect time changes, neglect heat flux) Qi – heating from electrons (Coulomb heating) Li – cooling: neutral particles O, N2, O2 and other ions (O+, H+, He+ ) Resonant charge exchange Polarization reactions Rees and Roble, Rev. Geoph. and Sp. Ph., 1975 COSPAR CBW

IRI Te model Bil-1985- based on Brace and Theis Te maps (JASTP 1981) coordinates diplat and solar local time TTSA option (JASR 2001) replaced by new TBT-2012 (EPS, 2012) IRI2012/IRI2016 JF(2)-.true./.false. - Te,Ti computed/not computed JF(23)-.true./.false.-Bil-1985/TBT-2012 Ne/Te correlation (Brace and Theis, 1978) - JF(10) -.true./.false.-Te – Standard /Te - Using Te/Ne correlation COSPAR CBW

Ne/Te correlation Brace and Theis, 1978 IRI 300 and 400km COSPAR CBW

Ne/Te correlation validity? Hinotori, daytime, equatorial latitudes Kakinami et al., JGR 2011 “U” shape COSPAR CBW

TBT-2012 Te model Employs the all available satellite Te data Include solar activity variation for day and night - an example for 550km and equinox: Employs minimum of independent coordinates to solve problem of limited data coverage Longitudinal structure neglected when it is used latitude coordinate based on the configuration of the real magnetic field coordinates invdip and magnetic local time Te PF10.7=200 Te PF10.7=150 Te PF10.7=90 Corrected Te model Data empirical profile COSPAR CBW

Magnetic latitude coordinates diplat: where I is the dip angle or magnetic inclination -longitudinal variation of Te reduced in equatorial latitudes Invariant latitude – invl (e.g. Roederer 1970): where the invariant radius R and the McIlwain L parameter obey -longitudinal variation of Te reduced at mid-latitudes (Smilauer and Afonin, ASR 1985) – plasma distributed along magnetic field lines invdip – combination of diplat and invl (Truhlik et al. 2001): COSPAR CBW

invdip (or invdiplat) magnetic local time (MLT) modified latitude – invdip (ASR Vol.27, No.1, 101,2001) longitudinal variation reduced to a second order effect ____ invdip _ _ _ dip latitude ____ invdip _ _ _ invariant latitude Configuration of the real geomagnetic field (IGRF 1990 at 600km) in different latitude coordinates in steps of 10° COSPAR CBW

Data base – satellite data All available Te satellite data (source mainly NSSDC, ISAS, and PIs of individual experiments) Year-altitude coverage of the data sets include in our data base. The curve at the top shows the solar 10.7 cm radio flux (F10.7 index – 3 months average). COSPAR CBW

Te model - Data distribution KOMPSAT DMSP ISIS 2 AE ISIS 2 IK 24 ISIS 1 Hinotori 9 million points – non-uniform distribution highest population corresponds to circularly orbiting satellites COSPAR CBW

Main (core) Te model equinox solstice 350km 550km Data grouped - altitudes: 350, 550, 850, 1400 and 2000km seasons: equinox, solstice A system of associated Legendre polynomials up to the 8th order was employed. Plm = associated Legendre function θ = invdip colatitude (0..π) ϕ = magnetic local time (0..2π). 350km 550km Te increases with altitude. At low latitudes (±30 invl) during the nighttime the Te altitude gradient is very small. Morning enhancement (morning overshoot) at equatorial latitudes and at low altitudes (350, 550 to 850 km) For solstices its maximum is shifted to the the winter hemisphere Dependence on invariant latitude is more prominent at lower altitudes (350 to 850 km). Generally the lowest electron temperature is observed close to the equator and increases with increasing invariant latitude. 850km 1400km 2000km

Model of the solar activity variation Solar activity variation of Te Qe and Le depend on solar activity – increase with increasing solar activity Te can increase, decrease or stay constant with increasing solar activity depending on altitude, latitude, local time and season => COSPAR CBW

Model of the solar activity variation Driven by PF10.7 index PF10.7=(F107A+F107D)/2 Normalized latitude profiles of Te for 3 levels of solar activity for day (13h MLT) and night (1h MLT): a) low PF10.7 < 110 b) medium 110 <= PF10.7 < 180 c) high F10.7=>180) Quadratic fit inside 110 <= PF10.7 < 180; Outside linear extrapolation Local time dependence approximated by a harmonic function Obtain a correction function TePF107(mlt,invdip,PF107) For fixed altitude and local time Te(mlt,invdip,PF107)=Te(mlt,invdip)+TePF107(mlt,invdip,PF107) COSPAR CBW

Solar activity correction function – example for 550km equinox ∆Te/K PF10.7=(F10.7D+F10.781)/2 Solar activity correction function—an example for 550 km equinox. * represent the normalized values from the normalized latitudinal profiles for low, medium and high solar activity. The dashed line represents a mathematical interpolation/extrapolation in solar activity using the three values. COSPAR CBW

Model of the solar activity variation of Te To include solar activity variation instead of Ti data use FLIP simulated values and the similar way as for TBT-2012 to use following approach: Driven by PF10.7 index PF10.7=(F107A+F107D)/2 Normalized latitude profiles of Ti for 3 levels of solar activity for day (13h MLT) and night (1h MLT) and also dawn (6h MLT) and dusk (18h MLT): a) low PF10.7 < 110 b) medium 110 <= PF10.7 < 180 c) high F10.7=>180) -Quadratic fit inside 110 <= PF10.7 < 180; Outside linear extrapolation -Local time dependence approximated by a smooth function -Obtain a correction function TePF107(mlt,invdip,PF107) For fixed altitude and local time Ti(mlt,invdip,PF107)=Ti(mlt,invdip)+TiPF107(mlt,invdip,PF107)

Latitude profiles of Te high medium low solar activity

Solar activity correction function – example for 550km equinox ∆T/K PF10.7

IRI Ti representation Tn Ti Te Altitude profiles (e.g. Bilitza, 1990): IRI-2012 or IRI-2016 Altitude profiles (e.g. Bilitza, 1990): - at the altitude of 200km Ti = Tn - Tn from MSIS(86) – includes solar activity variation 430km Ti from the AEROS A model (latitudinal profiles for day and night, Bilitza 1981) Ti <= Te in topside Tn <= Tn <=Te Tn Ti Te COSPAR CBW

Ion temperature - proposed model Data altitudes: 350km, 550km, 850km, 1000km Latitude (invdip) and MLT 2 seasons, equinox no hemispheric differences Modeling grid 9x18=162 bins Spherical harmonics (orthogonal system) up to 8th order Plm = associated Legendre function θ = invdip colatitude (0..π) ϕ = magnetic local time (0..2π).

Contour plots of Ti – new Ti model equinox solstice Ti increases with altitude. At low latitudes (±30deg invl) during the nighttime the Ti altitude gradient is very small. Morning enhancement (morning overshoot) at equatorial latitudes (550, 850 km) For solstices its maximum is shifted to the the winter hemisphere Generally the lowest ion temperature is observed close to the equator and increases with increasing invariant latitude. 350km 550km 850km 1000km

Relation of Te, Ti and Tn IRI Tn Tn Ti Ti Te COSPAR CBW

New data access - Swarm mission Project of ESA Primary purpose – monitoring of the geomagnetic field Launch date - 22 November 2013 (almost four years of data) Constellation of three identical satellites Satellite A (Alpha) + C (Charlie) Altitude: ~480km, inclination: 87.4° side-by-side flying (Δlon: 1.4°, ΔLT:6min) 160km distance at equator Orbital delay: 6s Satellite B (Bravo) Altitude: ~520km, inclination: 88° All satellites 270 days to cover all LT COSPAR CBW

Swarm mission - orbit Satellite local time Orbit altitudes Separation of the satellites - evolution COSPAR CBW

Swarm mission – future plans D. Sieg – Swarm DQW Oct. 2017 Preference - keep Swarm alive at least one solar cycle COSPAR CBW

Swarm mission - experiments Payload Vector Field Magnetometer (VFM) Absolute Scalar Magnetometer (ASM) Electric Field Instrument (EFI) Accelerometer (ACC) Laser Range Reflector (LRR) Measurement of density, temperature, drift velocity and electric field Thermal ion imager (TII) Langmuir probes (LP) COSPAR CBW

Langmuir probes - Swarm EFI Developped by IRF Uppsala 2 probes: Probe 1 in high gain, probe 2 in low Probe 1 – nitrated titanium (TiN) Probe 2 gold-plated titanium (Au) Data from probes telemetred to ground Principle: 128Hz applied to the I-V characteristics Measure the resulting current “ripple” technique, harmonic (sub)mode – used ~99% 1% classical sweep COSPAR CBW

Langmuir probes – access to data Various products released 0.5s Ne, Te - Provisional data set “PREL” (ASCII) (until July 2015) (harmonic mode, merged hi and low gain probes) 0.5s Ne, Te – Level 1b, Operational data set “OPER” (cdf) – (harmonic mode, high gain) from July 2015 16Hz Ne - Faceplate plasma density (limited interval) only for validation 0.5s Extended data set (both hi and low gain separately) only for validation 128s Ne, Te sweep mode - only for validation ftp://swarm-diss.eo.esa.int/ Many products still in validation/correction/calibration process but it is already provided for scientific community - after registration COSPAR CBW

Conclusions Global models of electron and ion temperatures are included in IRI These models include most important dependencies (on latitude, altitude, local time, and solar activity) Only limited spatial resolution - up to the 8th order of spherical harmonics More data is needed to better describe small scale features (anomalies, enhancements, troughs, longitudinal dependency etc.) Better description of parameters depending on solar/magnetic activity variation especially during period of current very different solar cycles from those which were known during previous decades It is important task to include independent Ti model COSPAR CBW