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Шестая ежегодная конференция "Физика плазмы в солнечной системе" PowerPoint PPT Presentation


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Шестая ежегодная конференция "Физика плазмы в солнечной системе" 14 – 18 февраля 2011 г. ИКИ РАН, Москва. Различные подходы к моделированию ионосферных эффектов геомагнитных бурь. М.В. Клименко 1,2 ; В.В. Клименко 1 , К.Г. Ратовский 3 , Л.П. Гончаренко 4.

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Шестая ежегодная конференция "Физика плазмы в солнечной системе"

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1418 2011 . ,

.. 1,2; .. 1, .. 3, .. 4

1 . .. , , , [email protected]

2 , ,

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4 , , , ,


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  • Mayr H.G., Volland H.(1973) Magnetic Storm Characteristics of the Thermosphere. J. Geophys. Res., 78(13), 22512264.

  • Mayr H.G., Hedin A.E.(1977) Significance of Large-Scale Circulation in Magnetic Storm Characteristics With Application to AE-C Neutral Composition Data. J. Geophys. Res., 82(7), 12271234.

  • Namgaladze A.A., Zakharov L.P., Namgaladze A.N.(1981) Numerical modeling of the ionospheric storms. Geomagn. Aeron., 21(2), 259265 (in Russian).

  • Maeda S., Fuller-Rowell T.J., Evans D.S.(1989) Zonally Averaged Dynamical and Compositional Response of the Thermosphere to Auroral Activity During September 18-24, 1984. J. Geophys. Res., 94(A12), 1686916883.

  • Sojka J.J., Schunk R.W., Denig W.F.(1994) Ionospheric response to the sustained high geomagnetic activity during the March89 great storm. J. Geophys. Res., 99(A11), 2134121352.

  • Reddy C.A., Mayr H.G.(1998) Storm-time penetration to low latitudes of magnetospheric-ionospheric convection and convection-driven thermospheric winds. Geophys. Res. Lett., 25(16), 30753078.

  • Frster M., Namgaladze A.A., Yurik R.Y.(1999) Thermospheric composition changes deduced from geomagnetic storm modeling. Geophys. Res. Lett., 26(16), 26252628.

  • Maruyama N., Richmond A.D., Fuller-Rowell T.J., Codrescu M.V., Sazykin S., Toffoletto F.R., Spiro R.W., Millward G.H.(2005) Interaction between direct penetration and disturbance dynamo electric fields in the storm-time equatorial ionosphere. Geophys. Res. Lett., 32, L17105, doi:10.1029/2005GL023, 763.

  • Fuller-Rowell T., Codrescu M., Maruyama N., Fredrizzi M., Araujo-Pradere E., Sazykin S., Bust G.(2007) Observed and modeled thermosphere and ionosphere response to superstorms. Radio Sci., 42, RS4S90, doi:10.1029/2005RS003392.

  • Lu G., Goncharenko L.P., Richmond A.D., Roble R.G., Aponte N.(2008) A dayside ionospheric positive storm phase driven by neutral winds. J. Geophys. Res., 113, A08304, doi:10.1029/2007JA012, 895

  • Balan N., Shiokawa K., Otsuka Y., Kikuchi T., Vijaya Lekshmi D., Kawamura S., Yamamoto M., and Bailey G.J. (2010) A physical mechanism of positive ionospheric storms at low latitudes and midlatitudes. J. Geophys. Res. 115, A02304, doi:10.1029/2009JA014515.


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Model GSM TIP Brief Description

Global Self-consistent Model of the Thermosphere, IonosphereandProtonosphere(GSM TIP) was developed in West Department of IZMIRAN. The model GSM TIP was described in detail inNamgaladze et al., 1988, 1990, 1991.

The model is added by the new block of electric field calculation Klimenko et al., 2006a,b, 2007.

Namgaladze, A.A., Korenkov, Yu.N., Klimenko, V.V., Karpov, I.V., Bessarab, F.S., Surotkin, V.A., Glushenko, T.A., Naumova, N.M. Pure and Applied Geophysics (PAGEOPH) 127, No. 2/3, 219254, 1988.

Namgaladze, A.A., Korenkov, Yu.N., Klimenko, V.V., Karpov, I.V., Bessarab, F.S., Surotkin, V.A., Glushchenko, T.A., Naumova, N.M. Geomagnetism and Aeronomy 30, No. 4, 612619, 1990.

Namgaladze, A.A., Korenkov, Yu.N., Klimenko, V.V., Karpov, I.V., Surotkin, V.A., Naumova, N.M. J. Atmos. Terr. Phys. 53, 11131124, 1991.

Klimenko, M.V., Klimenko, V.V., Bryukhanov, V.V. Geomagn. Aeron. 46, No. 4, 457466, doi:10.1134/S0016793206040074, 2006a.

.., .., .. 8, 3, 77-92, 2006b.

Klimenko, M.V., Klimenko, V.V., Bryukhanov, V.V. Adv. Radio Sci. 5, 385392, 2007.


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, (O2, N2, O) , , (O+, H+) , O2+ NO+, . , . . . 80 520 . 175 ~15 . 5 15 , , 175 . , . . , 2 . .


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Quiet conditions

= 35.7 (kV) setting at geomagnetic latitudes 75

j2= 310-8 A/m2

(Region 2 Field-Aligned Currents (R2 FAC) j2

setting at geomagnetic latitudes 70)


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Storm

= 26.4 + 13.3Kp (kV)

at geomagnetic latitudes 75

Feshchenko, Maltsev (2003)

j2 = 2.7810-8 + 0.3210-8Kp (A/m2)

with delay 0.5 h

GMLat(j2) = 70 for Kp 3.0

GMLat(j2) = 65 for 3.0 < Kp 6.0

GMLat(j2) = 60 for 6.0 < Kp

Iijima and Potemra (1976),

Kikuchi et al. (2008)

FluxStorm/FluxQuiet = 0.55 + 0.64Kp

with delay 0.5 h

with turn of a maximum precipitation

from midnight to the morning sector


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Effect of additional precipitations

Magnetosphere convection without R2 FAC and without (dark blue asterisks)

and with additional precipitations (red asterisks). Dark blue circles quiet conditions.

Norilsk

Yakutsk

Irkutsk

Hainan

Millstone Hill


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Effect of R2 FAC

Magnetosphere convection with additional precipitations and without (blue asterisks) and with (red asterisks) R2 FAC. Blue circles quiet conditions.

Norilsk

Yakutsk

Irkutsk

Hainan

Millstone Hill


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Effect of R2 FAC displacement

Magnetosphere convection with additional precipitations and with R2 FAC without (blue asterisks) and with R2 FAC displacement (red asterisks). Blue circles quiet conditions.

Norilsk

Yakutsk

Irkutsk

Hainan

Millstone Hill


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Simulation results

Magnetosphere convection without additional precipitations and R2 FAC (blue asterisks)

and with precipitation and R2 FAC with displacement (red asterisks) .

Blue circles quiet conditions.


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FIRST SUMMARY

1. Comparison of model calculation results of the different ionospheric parameters with experimental data under middle- and low- latitude stations reveals the satisfactory consent.

2. The reasons of distinctions of calculation resultsand observational data are the folowing:

a) the use of 3-hour Kp-indexes at modelling of temporal dependence of input model parameters;

b) the dipole approach of geomagnetic field;

c) absence in model calculations the effects of solar flares which are taken place during the considered period.


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  • The use in model GSM TIP the dipole approach of geomagnetic field does not allow considering its distortion observed during storms:

    • Its compression on the dayside of magnetosphere

    • Its expansion on night side of magnetosphere.

  • By the compression of a geomagnetic field on the day side it is possible to explain the additional contribution to the positive disturbance in electron concentration in the afternoon. At the compression the volume of plasma tube decreases that leads to the enhancement of electron concentration. Unfortunately, now the model GSM TIP does not describe this process.


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    Solar Flares


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    Quiet conditions

    Kp = 1

    AE = 0

    F10.7 = 101 on 09.09.2005

    F10.7 = 118 on 10.09.2005

    F10.7 = 111 on 11.09.2005

    F10.7 = 120 on 12.09.2005

    F10.7 = 115 on 13.09.2005

    F10.7 = 118 on 14.09.2005

    = 38.0 kV setting at geomagnetic latitudes 75

    j2 = 310-9 A/m2

    (Region 2 field aligned currents j2 setting at geomagnetic latitudes 65)

    Storm time conditions

    09.09.2005 09:00 UT 14:01 UT quiet conditions,

    14:01 UT 16:00 UT SSC,

    16:00 UT 18:00 UT main phase,

    18:00 UT 06:00 UT 10.09.2005 recovery phase;

    10.09.2005 06:00 UT 13:00 UT SSC,

    13:00 UT 20:00 UT main phase,

    20:00 UT 01:14 UT 11.09.2005 recovery phase;

    11.09.2005 01:14 UT 05:00 UT SSC,

    05:00 UT 11:00 UT main phase,

    11:00 UT 24:00 UT 14.09.2005 recovery phase.


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    Storm time conditions

    = 38 + 0.089AE, kVat geomagnetic latitudes75

    Feshchenko, Maltsev (2003)

    Region 2 Field aligned currents according to

    Cheng et al. (2008); Snekvik et al. (2007)

    in quiet conditions and at recovery phase of storm

    j2= 310-9 + 6 10-12AE, A/m2

    at SSC phase of storm with 30 min delay

    j2= 310-9 + 1.5 10-11AE, A/m2

    in active phase of storm

    j2= 310-9 + 3.6 10-11AE, A/m2

    The displacement of Region 2 field aligned currents to the lower latitudes as by

    Sojka et al. (1994)

    65 for 40 kV;

    60 for 40 kV < 50 kV;

    55 for 50 kV < 88.5 kV;

    50 for 88.5 kV < 127 kV;

    45 for 127 kV < 165.4 kV;

    40 for 165.4 kV < 200 kV;

    35 for 200 kV <


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    Kp=0.0

    Particle Precipitation

    Model of Zhan and Paxton, 2008

    Energy (keV) & Energy Flux (erg/cm2)

    Kp=6.0

    Kp=2.0

    Kp=4.0

    Kp=7.0

    Kp=5.0

    Kp=7.7


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    September 10, 2005

    Ionospheric Storm

    Millstone Hill


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    Goncharenko et al., 2007


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    September 10, 2005

    Ionospheric Storm

    Arecibo


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    Goncharenko et al., 2007


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    Ionospheric Effects in TEC of

    Storm Sequence

    September 1014, 2005


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    TEC Disturbances

    during Storm Sequence on 09-13 September, 2005

    Model GPS Model GPS


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    Simulation results

    Calculation results: dark blue circles without solar flares, light red circles with solar flares, light blue circles quiet conditions. Experimental data: light black circles quiet conditions, dark black circles storm time conditions.


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    1. , AE 3- Kp- .

    2. , Kp-.

    3. , , .

    4. , , F3- .

    5. , .


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    Acknowledgments

    Authors express the huge gratitude for use ofthe ionospheric observational data during the period on September 8-14, 2005 obtained from SPIDR.

    Authors acknowledge the Kyoto Center of geomagnetic data for providing geomagnetic activity indices and World Data Center in Boulder for providing solar activity indices during the period on September 8-14, 2005.

    We are grateful to the IGS community for providing GPS permanent data.

    Weacknowledge the GUVI team, Irkutsk and Yakutsk digisonde teams and Arecibo and Millstone Hill ISR teams for processing the data and making the experimental data available.

    We want to say many thanks to Dr. Habaruelema for GPS TEC data above Grahamstown, Dr. L-.A. Maccinel for processing of digisondes data and Dr. Zakharenkova I.E. for plotting of global maps of GPS TEC deviations.

    This investigations were carried out at financial support of Russian Foundation for Basic Research (RFBR) Grant 08-05-00274.


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    Thank you very much

    for your attention


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