Magnetosphere response to impulse space weather events: relationships between PC, AE and SymH indices O. Troshichev and D.Sormakov Arctic and Antarcrtic.

Slides:



Advertisements
Similar presentations
The Bimodal Solar Wind-Magnetosphere- Ionosphere System George Siscoe Center for Space Physics Boston University ●Vasyliunas Dichotomization Momentum transfer.
Advertisements

Study of Pi2 pulsations observed from MAGDAS chain in Egypt E. Ghamry 1, 2, A. Mahrous 2, M.N. Yasin 3, A. Fathy 3 and K. Yumoto 4 1- National Research.
Solar and Interplanetary Sources of Geomagnetic disturbances Yu.I. Yermolaev, N. S. Nikolaeva, I. G. Lodkina, and M. Yu. Yermolaev Space Research Institute.
4/18 6:08 UT 4/17 6:09 UT Average polar cap flux North cap South cap… South cap South enter (need to modify search so we are here) South exit SAA Kress,
DEFINITION, CALCULATION, AND PROPERTIES OF THE Dst INDEX R.L. McPherron Institute of Geophysics and Planetary Physics University of California Los Angeles.
ESS 7 Lecture 14 October 31, 2008 Magnetic Storms
The role of solar wind energy flux for transpolar arc luminosity A.Kullen 1, J. A. Cumnock 2,3, and T. Karlsson 2 1 Swedish Institute of Space Physics,
IMF Bx influence on the magnetotail neutral sheet geometry and dynamics E. Gordeev, M. Amosova, V. Sergeev Saint-Petersburg State University, St.Petersburg,
Spatial distribution of the auroral precipitation zones during storms connected with magnetic clouds O.I. Yagodkina 1, I.V. Despirak 1, V. Guineva 2 1.
Anti-parallel versus Component Reconnection at the Magnetopause K.J. Trattner Lockheed Martin Advanced Technology Center Palo Alto, CA, USA and the Polar/TIMAS,
Occurrence and properties of substorms associated with pseudobreakups Anita Kullen Space & Plasma Physics, EES.
Identification and Analysis of Magnetic Substorms Patricia Gavin 1, Sandra Brogl 1, Ramon Lopez 2, Hamid Rassoul 1 1. Florida Institute of Technology,
Solar wind-magnetosphere coupling, substorms, and ramifications for ionospheric convection Steve Milan Adrian Grocott (Leics,
SuperDARN Workshop May 30 – June Magnetopause reconnection rate and cold plasma density: a study using SuperDARN Mark Lester 1, Adrian Grocott 1,2,
PLASMA TRANSPORT ALONG DISCRETE AURORAL ARCS A.Kullen 1, T. Johansson 2, S. Buchert 1, and S. Figueiredo 2 1 Swedish Institute of Space Physics, Uppsala.
Lecture 3 Introduction to Magnetic Storms. An isolated substorm is caused by a brief (30-60 min) pulse of southward IMF. Magnetospheric storms are large,
Absence of a Long Lasting Southward Displacement of the HCS Near the Minimum Preceding Solar Cycle 24 X. P. Zhao, J. T. Hoeksema and P. H. Scherrer Stanford.
1 Geomagnetic/Ionospheric Models NASA/GSFC, Code 692 During the early part of April 6, 2000 a large coronal “ejecta” event compressed and interacted with.
M. Menvielle and A. Marchaudon ESWW2 M. Menvielle (1) and A. Marchaudon (2) (1) Centre d’études des Environnements Terrestre et Planétaires UMR 8615 IPL/CNRS/UVSQ.
Solar wind-magnetosphere- atmosphere coupling: effects of magnetic storms and substorms in atmospheric electric field variations Kleimenova N., Kozyreva.
Magnetospheric ULF wave activity monitoring based on the ULF-index OLGA KOZYREVA and N. Kleimenova Institute of the Earth Physics, RAS.
Cynthia López-Portela and Xochitl Blanco-Cano Instituto de Geofísica, UNAM A brief introduction: Magnetic Clouds’ characteristics The study: Event types.
A.V. Belov 1, E. A. Eroshenko 1, H. Mavromichalaki 2, V.A. Oleneva 1, A. Papaioannou 2, G. Mariatos 2, V. G. Yanke 1 (1) Institute of Terrestrial Magnetism,
New Unifying Procedure for PC index calculations. P. Stauning Danish Meteorological Institute ( + 45
A. Kullen (1), L. Rosenqvist (1), and G. Marklund (2) (1) Swedish Institute of Space Physics, Uppsala, Sweden (2) Royal Institute of Technology, Stockholm,
Statistical properties of southward IMF and its geomagnetic effectiveness X. Zhang, M. B. Moldwin Department of Atmospheric, Oceanic, and Space Sciences,
Localized Thermospheric Energy Deposition Observed by DMSP Spacecraft D. J. Knipp 1,2, 1 Unversity of Colorado, Boulder, CO, USA 2 High Altitude Observatory,
Ground level enhancement of the solar cosmic rays on January 20, A.V. Belov (a), E.A. Eroshenko (a), H. Mavromichalaki (b), C. Plainaki(b), V.G.
MAGNETOSPHERIC RESPONSE TO COMPLEX INTERPLANETARY DRIVING DURING SOLAR MINIMUM: MULTI-POINT INVESTIGATION R. Koleva, A. Bochev Space and Solar Terrestrial.
2009 ILWS Workshop, Ubatuba, October 4-9, 2009 Transverse magnetospheric currents and great geomagnetic storms E.E.Antonova (1,2), M. V. Stepanova (3),
SOLAR EXTREME EVENTS AND GRATE GEOMAGNETIC STORMS E.E. Antonova, M.V. Stepanova Skobeltsyn Institute of Nuclear Physics Moscow State University, Moscow,
Response of the Magnetosphere and Ionosphere to Solar Wind Dynamic Pressure Pulse KYUNG SUN PARK 1, TATSUKI OGINO 2, and DAE-YOUNG LEE 3 1 School of Space.
Energy conversion at Saturn’s magnetosphere: from dayside reconnection to kronian substorms Dr. Caitríona Jackman Uppsala, May 22 nd 2008.
Earth’s Magnetosphere NASA Goddard Space Flight Center
Mapping high-latitude TEC fluctuations using GNSS I.I. SHAGIMURATOV (1), A. KRANKOWSKI (2), R. SIERADZKI (2), I.E. ZAKHARENKOVA (1,2), Yu.V. CHERNIAK (1),
Forecast of Geomagnetic Storm based on CME and IP condition R.-S. Kim 1, K.-S. Cho 2, Y.-J. Moon 3, Yu Yi 1, K.-H. Kim 3 1 Chungnam National University.
Testing the Equipotential Magnetic Field Line Assumption Using SuperDARN Measurements and the Cluster Electron Drift Instrument (EDI) Joseph B. H. Baker.
GEOSYNCHRONOUS SIGNATURES OF AURORAL SUBSTORMS PRECEDED BY PSEUDOBREAKUPS A. Kullen (1), S. Ohtani (2), and H. Singer (3) A. Kullen (1), S. Ohtani (2),
ESS 7 Lecture 13 October 29, 2008 Substorms. Time Series of Images of the Auroral Substorm This set of images in the ultra-violet from the Polar satellite.
IAGA Symposium A12.2 Geomagnetic networks, computation and definition of products for space weather and space climate Melbourne, Australia, 2011 GLOBAL,
E.E. Antonova1,2, I.P. Kirpichev2,1, Yu.I. Yermolaev2
Simultaneous in-situ observations of the feature of a typical FTE by Cluster and TC1 Zhang Qinghe Liu Ruiyuan Polar Research Institute of China
Guan Le NASA Goddard Space Flight Center Challenges in Measuring External Current Systems Driven by Solar Wind-Magnetosphere Interaction.
Athens University – Faculty of Physics Section of Nuclear and Particle Physics Athens Neutron Monitor Station Study of the ground level enhancement of.
Global Structure of the Inner Solar Wind and it's Dynamic in the Solar Activity Cycle from IPS Observations with Multi-Beam Radio Telescope BSA LPI Chashei.
Study on the Impact of Combined Magnetic and Electric Field Analysis and of Ocean Circulation Effects on Swarm Mission Performance by S. Vennerstrom, E.
ABSTRACT Disturbances in the magnetosphere caused by the input of energy from the solar wind enhance the magnetospheric currents and it carries a variation.
Particle precipitation has been intensely studied by ionospheric and magnetospheric physicists. As particles bounce along the earth's magnetic fields they.
Extreme Event Symposium 2004 MAGNETOSPHERIC EFFECT in COSMIC RAYS DURING UNIQUE MAGNETIC STORM IN NOVEMBER Institute of Terrestrial Magnetism,
R. Maggiolo 1, M. Echim 1,2, D. Fontaine 3, A. Teste 4, C. Jacquey 5 1 Belgian Institute for Space Aeronomy (IASB-BIRA); 2 Institute.
Earth’s Magnetosphere Space Weather Training Kennedy Space Center Space Weather Research Center.
Source and seed populations for relativistic electrons: Their roles in radiation belt changes A. N. Jaynes1, D. N. Baker1, H. J. Singer2, J. V. Rodriguez3,4.
Drivers and Solar Cycles Trends of Extreme Space Weather Disturbances
Lecture 12 The Importance of Accurate Solar Wind Measurements
Extremely Intense (SML ≤ nT) Supersubstorms (SSS)
Johns Hopkins Applied Physics Laboratory, Laurel MD, USA
Introduction to Space Weather Interplanetary Transients
Evidence for Dayside Interhemispheric Field-Aligned Currents During Strong IMF By Conditions Seen by SuperDARN Radars Joseph B.H. Baker, Bharat Kunduri.
Effects of Dipole Tilt Angle on Geomagnetic Activities
The Physics of Space Plasmas
Environmental conditions during the charging anomaly of the two geosynchronous satellites reported: TELSTAR 401 and Galaxy 15 Elena Saiz, A. Guerrero,
Advances in Ring Current Index Forecasting
Yuki Takagi1*, Kazuo Shiokawa1, Yuichi Otsuka1, and Martin Connors2  
Introduction to Space Weather
Subauroral heliosphere-geosphere coupling during November 2004 ionospheric storms: F2-region, North-East Asia Chelpanov M. A., Zolotukhina N.A. Institute.
Swedish Institute of Space Physics, Kiruna
High-Speed Plasma Flows Observed in the Magnetotail during Geomagemtically Quiet Times: Relationship between Magnetic Reconnection, Substorm and High-Speed.
P. Stauning: The Polar Cap (PC) Index for Space Weather Forecasts
Searching for relationships between the solar regular daily magnetic variation at mid latitude and the solar irradiance at different ionizing wavelengths.
Added-Value Users of ACE Real Time Solar Wind (RTSW) Data
Presentation transcript:

Magnetosphere response to impulse space weather events: relationships between PC, AE and SymH indices O. Troshichev and D.Sormakov Arctic and Antarcrtic Research Institute, St.Petersburg olegtro@aari.ru The Solar-Terrestrial Physics Symposium (STP14) York University, Toronto, Canada, July 9-13, 2018 1 1

Introduction Classic magnetic storm includes two energizing parts and a subsequent recovery. The first part consists of a sudden commencement (SC) and an initial phase, which are result of change in compression of the magnetosphere following the passage of a discontinuity (such as a shock front) propagating in the solar wind. A rise time of SC (impulsive increase produced in the geomagnetic H-component) is one to six minutes and an amplitude of several tens of nT. The initial phase produced by currents flowing on magnetopause (DCF) typically lasts few hours, during which the field remains compressed by the solar wind pressure increase following the discontinuity. The second phase is the main phase. It is depression of the magnetic field produced by a ring current (DR), which is developed in the inner magnetosphere. Since solar wind discontinuities usually involve changes in both pressure and the interplanetary magnetic field (IMF) direction, magnetic storms typically show both compression and inflation effects. The summary effect of both contributors, which is maximal in the equatorial region, is evaluated by the 1-hour Dst index or 1-min SymH index depicting a longitudinally averaged magnetic field variation at low latitudes [Sugiura, 1976]. In course of magnetic storms developing the DR current effect far exceeds the DCF current effect, that is why the effect of impulse space weather events (interplanetary shocks) can be revealed only during the initial phase. In this study we examine relationships between the magnetic activity indices (PC, AL, SymH) and corresponding changes in the solar wind parameters (solar wind dynamic pressure Pd, southward IMF component, solar wind velocity Vsw and interplanetary electric field Ekl) during the initial phase produced by shock front propagating in solar wind.

PC index: Physical backgrounds The variable solar wind coupling with the geomagnetic field constantly generates the “magnetospheric field-aligned electric currents” flowing along the geomagnetic field lines [Langel, 1975; McDiarmid et al.,1977; Iijima & Potemra, 1982; Bythrow & Potemra, 1983]. The currents are distributed along the poleward boundary of the auroral zone (Region 1 FAC) and flow into the polar ionosphere on the dawn side and flow out of the ionosphere on the dusk side of the auroral zone. These currents are responsible for the cross-polar cap potential difference and ionospheric currents producing the polar cap magnetic disturbances [Troshichev and Tsyganenko, 1979]. PC index has been introduced [Troshichev and Andrezen, 1985; Troshichev et al., 1988] to characterize the polar cap magnetic activity produced by the interplanetary electric field EKL [Kan and Lee, 1979] EKL=Vsw*(By2+Bz2)1/2sin2θ/2 where Vsw – solar wind speed, By, Bz –azimuthal and vertical IMF components. РС index is determined as a value of the EKL-produced magnetic disturbances at the near-pole stations (Thule and Vostok) with allowance for UT time, season and hemisphere.

Resolutions of XXII Scientific Assembly of International Geomagnetism and Aeronomy Association (12th IAGA), Merida, Меxico, August 2013 No. 3: Polar Cap (PC) index IAGA, noting that polar cap magnetic activity is not yet described by existing IAGA geomagnetic indices, considering that the Polar Cap (PC) index constitutes a quantitative estimate of geomagnetic activity at polar latitudes and serves as a proxy for energy that enters into the magnetosphere during solar wind-magnetosphere coupling, emphasising that the usefulness of such an index is dependent on having a continuous data series, recognising that the PC index is derived in partnership between the Arctic and Antarctic Research Institute (AARI, Russian Federation) and the National Space Institute, Technical University of Denmark (DTU, Denmark) recommends use of the PC index by the international scientific community in its near-real time and definitive forms, and urges that all possible efforts be made to maintain continuous operation of all geomagnetic observatories contributing to the PC index. Therein lies the principal distinction of the PC index from various coupling functions (which are characteristics of the solar wind arriving to the Lagrange point L1) and from AL and Dst indices (which are characteristics of the energy realized in form of magnetospheric substorm and magnetic storms). 4

Experimental data indicative of the PC index as a proxy of the solar wind energy incoming into the magnetosphere In course of magnetospheric substorms and magnetic storms the PC index strongly follows the time evolution of interplanetary electric field EKL (correlation R > 0.5 in 98% of events) with delay time ΔT ~ 20-30 min. The value of delay time ΔT is controlled by the EKL growth rate (dEKL/dt). Development of magnetospheric substorms and magnetic storms is generally preceded by the PC index growth. Magnetospheric substorms start as soon as the PC index exceeds the threshold level PC=1.5 mV/m, irrespective of the substorm growth phase duration and type of substorm (isolated or extended). Intensity of magnetic disturbances in the auroral zone (AL index) before and after the substorm sudden onset is linearly related to PC value. Steady exceeding the threshold level PC=1.5 mV/m is necessary and sufficient condition for the storm beginning, like to case of magnetic substorms; In course of magnetic storms the SymH index generally follows the time evolution of the 30-min smoothed PC index irrespective of type and intensity of magnetic storms. In case of classic storms the maximal depression of geomagnetic field (i.e magnetic storm intensity Dstmin), follows, with delay ~60 min, the maximal value of smoothed PC (PCmax), the values PCmax and Dstmin being connected by linear relationship. The low (R<0.50) or negative correlation between EKL and PC was observed in ~ 10% of examined events suggesting that the solar wind fixed by ACE did not encounter the magnetosphere in these cases. Therefore, the PC index might be useful to monitor the space weather and real state of the magnetosphere and to keep check whether or not the solar wind fixed in Lagrange point L1 actually encounters the magnetosphere

Correlation between PC and the solar wind parameters (BZ, Vx, EKL) in course of magnetic storms Correlation between the PC and IMF Bz (R>0.5) is observed in 397 storm events of 429 (92.5%), with typical delay time ΔΤ=20-30 min in response of PC to Bz changes. Correlation between PC and the solar wind velocity VX R>0.5 is observed only in 86 events of 429 (20%). The best connection is between PC and EKL : correlation coefficients R>0.5 take place in 422 storm events of 429 (98.4%).

Correlation between PC and AL/SymH indices in course of magnetic storms Correlation between the EKL field and AL index (R>0.5) is observed in 411 storm events of 429 (96%). Correlation between the PC and AL indices is always better than R=0.5, in 72% of storms the correlation coefficients being higher than 0.75. The AL index responds to the PC index changes with delay times ΔΤ=0÷10 min; Correlation between the PC and SymH indices (R>0.5) is observed in 81% of storm events) being better than between EKL and SymH (in 68% of storm events).

Method of the analysis Selection of magnetic storms events with distinctive initial phase was carried out by data on the solar wind dynamic pressure (Pd), obtained from the GSFC/SPDF OMNI/Web interface at http://omniweb.gsfc.nasa.gov. The SC magnitude was identified as a Pd increase by value more than 10 nP within 5 minutes. The events with gaps in the solar wind data were excluded from the analysis if the gaps were in excess of 30% of the event data series Sets of 1-min data on the PC, AL and SymH indices were used in the analysis. The PC index, as a mean value of the appropriate PC indices in the northern and southern hemispheres, was taken. To release effects of the Pd impulses themselves the only magnetic storms events, developing against the background of the relatively quiet conditions, lasting during one hours or more prior SC, were only examined. As a result, the total number of the analyzed events for the period of 1998-2016 turned out to be N=84. The actual moment of the solar wind contact with magnetosphere was determined by sharp jump in the SymH index, the moment of this jump was identified as SC moment (T0). All separated events were examined at interval of T0±40 minutes, where is a moment of sharp increase in Sym H index. ..

Relationship between actual SC moments (derived from SymH data) and SC moments estimated from the Pd measurements on board ACE spacecraft Solar wind dynamic pressure Pd was evaluated by data on solar wind parameters measured on board ACE spacecraft in the point of libration (at the distance of ~ 1.5 million km upstream of the Earth) reduced to the magnetopause. The actual contact of the fixed solar wind with the magnetosphere can differ from estimated time, if the shock front was propagated with acceleration or deceleration. Comparison of actual and estimated SC moments demonstrates that both options can meet in reality. Time, min

Initial phase under conditions of southward IMF Bz<0 and growing Vsw Magnetic disturbances in the auroral zone (AL index) and PC index reach maximum values under conditions of southward IMF (Bzmean~-3 nT) and growing solar wind velocity (mean Vsw increases from 200 to 500 km/c during initial phase).

Initial phase under conditions of southward IMF Bz<0 and steady Vsw Under conditions of southward IMF (Bzmean~-3 nT) and steady solar wind velocity (Vswmean~380km/c) during initial phase the intensity of magnetic disturbances in auroral zone (AL index) sharply decreases (~150 km/sec) for the same values of dynamic pressure.

Initial phase under conditions of northward IMF Bz>0 and growing Vsw Under conditions of norththward IMF (Bzmean~ 4 nT) and growing solar wind velocity (Vswmean~475km/c) the mean intensity of magnetic disturbances in auroral zone (AL index) during initial phase negligibly increases (from 50 to 100 nT).

Initial phase under conditions of northward IMF Bz>0 and steady Vsw Under conditions of norththward IMF (Bzmean~ 4 nT) and steady solar wind velocity (Vswmean~475km/c) the mean intensity of magnetic disturbances in auroral zone (AL index) remains on zero level during initial phase (in spite of action of same Pd impulse).

Total relationships between Pd, SymH, PC and AL during initial phase Growing Vsw Steady Vsw Bz<0 Bz>0 Pd (nP) ~10 Sym H (nT) 30 18 20 PC (mV/m) 2.5 1.8 1.5 0.5 AL (nT) 300 50 75 ~0 Conclusions: Intensity of magnetospheric disturbances is strongly dependent on the IMF polarity and the solar wind velocity variability and can be quiet different for the same power of the pressure impulses (Pd). The disturbances are maximal for conditions of southward IMF and growing solar wind velocity Vsw and fall to minimum under conditions of northward IMF and steady Vsw (with the same power of the solar wind dynamic pressure Pd!!!). It means that the pressure shocks themselves are not promote (or insignificantly promote) the solar wind energy input into the magnetosphere which is controlled mainly by the interplanetary electric field EKL~Vsw*(BY2+BZ2)1/2 and displayed by the PC index.

Thank you for attention! . PC web site: http://pcindex.org