Solar and Interplanetary Sources of Geomagnetic disturbances Yu.I. Yermolaev, N. S. Nikolaeva, I. G. Lodkina, and M. Yu. Yermolaev Space Research Institute.

Slides:

Advertisements

Similar presentations

Olga Khabarova & Vladimir obridko Heliophysical Laboratory, Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS (IZMIRAN), Moscow,

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.

Non-stationary solar wind structures and their influence on substorm bulge development I.V. Despirak 1, A.A. Lubchich 1, V. Guineva 2 1. Polar Geophysical.

Scale Size of Flux Ropes in the Solar Wind Cartwright, ML & Moldwin, MB IGPP/UCLA, Los Angeles, CA Background: The solar wind has long.

On the Space Weather Response of Coronal Mass Ejections and Their Sheath Regions Emilia Kilpua Department of Physics, University of Helsinki

Reviewing the Summer School Solar Labs Nicholas Gross.

ESS 7 Lecture 14 October 31, 2008 Magnetic Storms

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.

1 Diagnostics of Solar Wind Processes Using the Total Perpendicular Pressure Lan Jian, C. T. Russell, and J. T. Gosling How does the magnetic structure.

Altitude Response of Thermosphere Mass Density to Geomagnetic Activity in the Recent Solar Minimum Jeffrey P. Thayer, Xianjing Lui, and Jiuhou Lei MURI.

Space Weather Forecast Models from the Center for Integrated Space Weather Modeling The Solar Wind Forecast Model Carrington Rotation 1896Carrington Rotation.

Coronal Ejecta in October - November of 2003 and predictions of the associated geomagnetic events 1 Big Bear Solar Observatory, New Jersey Institute of.

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.

Identifying Interplanetary Shock Parameters in Heliospheric MHD Simulation Results S. A. Ledvina 1, D. Odstrcil 2 and J. G. Luhmann 1 1.Space Sciences.

Solar wind-magnetosphere- atmosphere coupling: effects of magnetic storms and substorms in atmospheric electric field variations Kleimenova N., Kozyreva.

Numerical simulations are used to explore the interaction between solar coronal mass ejections (CMEs) and the structured, ambient global solar wind flow.

Katya Georgieva Boian Kirov Simeon Asenovski

CR variation during the extreme events in November 2004 Belov (a), E. Eroshenko(a), G. Mariatos ©, H. Mavromichalaki ©, V.Yanke (a) (a) IZMIRAN), ,

Magnetospheric ULF wave activity monitoring based on the ULF-index OLGA KOZYREVA and N. Kleimenova Institute of the Earth Physics, RAS.

Magnetic Storm Generation by Various Types of Solar Wind: Event Catalog, Modeling and Prediction N. S. Nikolaeva, Yu.I. Yermolaev, and I. G. Lodkina Space.

Ultimate Spectrum of Solar/Stellar Cosmic Rays Alexei Struminsky Space Research Institute, Moscow, Russia.

Study of Local Heliospheric Current Sheet Variations from Multi-Spacecraft Observations D. Arrazola · J.J. Blanco · J. Rodríguez-Pacheco · M.A. Hidalgo.

Olga Khabarova Heliophysical Laboratory, Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS (IZMIRAN), Moscow, Russia

Space Weather from Coronal Holes and High Speed Streams M. Leila Mays (NASA/GSFC and CUA) SW REDISW REDI 2014 June 2-13.

Case Studies of Interplanetary Coronal Mass Ejections Interplanetary Coronal Mass Ejections – Different Phases of the Cycle Of particular interest to the.

Solar Cycle Trends and Case Studies of Interplanetary Coronal Mass Ejections Interplanetary Coronal Mass Ejections During Different Phases of the Cycle.

Cynthia López-Portela and Xochitl Blanco-Cano Instituto de Geofísica, UNAM A brief introduction: Magnetic Clouds’ characteristics The study: Event types.

The Sun- Solar Activity. Damage to communications & power systems.

Statistical properties of southward IMF and its geomagnetic effectiveness X. Zhang, M. B. Moldwin Department of Atmospheric, Oceanic, and Space Sciences,

Geoeffectiveness of Solar and Interplanetary Events Yuri I. Yermolaev, Michail Yu. Yermolaev, Georgy N. Zastenker, Anatoli A. Petrukovich, Lev M. Zelenyi.

1 The Geo-Response to Extreme Solar Events: How Bad Can it Get? Leif Svalgaard Stanford University, California, USA AOGS,

MAGNETOSPHERIC RESPONSE TO COMPLEX INTERPLANETARY DRIVING DURING SOLAR MINIMUM: MULTI-POINT INVESTIGATION R. Koleva, A. Bochev Space and Solar Terrestrial.

2004 September 11CAWSES Theme 2 Meeting, Beijing Solar Sources of Geoeffective Disturbances N. Gopalswamy NASA/GSFC Greenbelt, MD

1 Large Solar Events in Historical Context Leif Svalgaard HEPL, Stanford University AGU Fall 2013, SH23D-02.

27-Day Variations Of The Galactic Cosmic Ray Intensity And Anisotropy In Different Solar Magnetic Cycles ( ) M.V. Alania, A. Gil, K. Iskra, R.

Identifying the Role of Solar-Wind Number Density in Ring Current Evolution Paul O’Brien and Robert McPherron UCLA/IGPP.

Lessons for STEREO - learned from Helios Presented at the STEREO/Solar B Workshop, Rainer Schwenn, MPS Lindau The Helios.

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.

The spatial and temporal distribution of solar and galactic cosmic rays S. V. Tasenko 1, P. V. Shatov 1, I. A. Skorokhodov 1, I. V. Getselev 1,2, M. Podzolko.

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

Adjustable magnetospheric event- oriented magnetic field models N. Yu. Ganushkina (1), M. V. Kubyshkina (2), T. I. Pulkkinen (1) (1) Finnish Meteorological.

Intermittency Analysis and Spatial Dependence of Magnetic Field Disturbances in the Fast Solar Wind Sunny W. Y. Tam 1 and Ya-Hui Yang 2 1 Institute of.

May 23, :45ISEA, Crete, Greece. S10 Ionospheric storms and space weather effects Penetration Characteristics of the Interplanetary Electric Field.

O N THE INFLUENCE OF THE CORONAL HOLE LATITUDE AND POLARITY ON THE GEOMAGNETIC ACTIVITY AND COSMIC RAY VARIATIONS Abunina Maria, IZMIRAN, Russia Abunin.

GEOEFFECTIVE INTERPLANETARY STRUCTURES: 1997 – 2001 A. N. Zhukov 1,2, V. Bothmer 3, A. V. Dmitriev 2, I. S. Veselovsky 2 1 Royal Observatory of Belgium.

Coronal and Interplanetary Magnetic Fields in October-November 2003 and November CMEs Vasyl Yurchyshyn Big Bear Solar Observatory,

CME Propagation CSI 769 / ASTR 769 Lect. 11, April 10 Spring 2008.

What we can learn from the intensity-time profiles of large gradual solar energetic particle events (LGSEPEs) ？ Guiming Le(1, 2,3), Yuhua Tang(3), Liang.

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.

Elena Saiz, C. Cid, A. Guerrero, J. Palacios, Y. Cerrato Space Research Group - Space Weather University of Alcalá (Spain)

29 ICRC, Pune, India, 2005 Geomagnetic effects on cosmic rays during the very strong magnetic storms in November 2003 and November 2004 Belov (a), L. Baisultanova.

The ICME’s magnetic field and the role on the galactic cosmic ray modulation for the solar cycle 23 Evangelos Paouris and Helen Mavromichalaki National.

ABSTRACT Disturbances in the magnetosphere caused by the input of energy from the solar wind enhance the magnetospheric currents and it carries a variation.

What is a geomagnetic storm? A very efficient exchange of energy from the solar wind into the space environment surrounding Earth; These storms result.

Extreme Event Symposium 2004 MAGNETOSPHERIC EFFECT in COSMIC RAYS DURING UNIQUE MAGNETIC STORM IN NOVEMBER Institute of Terrestrial Magnetism,

ESS 261 Lecture April 28, 2008 Marissa Vogt. Overview  “Probabilistic forecasting of geomagnetic indices using solar wind air mass analysis” by McPherron.

Measurements of the Orientation of the Heliospheric Magnetic Field Neil Murphy Jet Propulsion Laboratory.

The CME geomagnetic forecast tool (CGFT) M. Dumbović 1, A. Devos 2, L. Rodriguez 2, B. Vršnak 1, E. Kraaikamp 2, B. Bourgoignie 2, J. Čalogović 1 1 Hvar.

Drivers and Solar Cycles Trends of Extreme Space Weather Disturbances

Drivers and Solar Cycles Trends of Extreme Space Weather Disturbances

Johns Hopkins Applied Physics Laboratory, Laurel MD, USA

Introduction to Space Weather Interplanetary Transients

Investigations of CME in muon flux detected in hodoscopic mode

Consequences of the Anomalous Expansion of CMEs in Solar Cycle 24

Solar Wind Transients and SEPs

Forecasting the arrival time of the CME’s shock at the Earth

Yuki Takagi1*, Kazuo Shiokawa1, Yuichi Otsuka1, and Martin Connors2

The properties of CMEs embedded in extreme solar wind

Introduction to Space Weather

Presentation transcript:

Solar and Interplanetary Sources of Geomagnetic disturbances Yu.I. Yermolaev, N. S. Nikolaeva, I. G. Lodkina, and M. Yu. Yermolaev Space Research Institute (IKI - ), RAS, Moscow, Russia Several results have been published and may be found in Space Weather Effects on Humans:in Space and on Earth International Conference IKI, Moscow, June 4-8, 2012

History After Richard Carrington’s observation of strong solar flare on 1 September 1859 and strong magnetic storm in 18 hours after flare there was point of view that solar flares are sources of magnetic storms. Modern observations showed that after most part of flares there is no magnetic storms and many storms are observed without any solar activity.

Solar flares and magnetic storms during

Main reason of magnetospheric disturbances is negative (southward) component of Interplanetary Magnetic Field (IMF Bz < 0) Non-disturbed solar wind contains IMF which lies in ecliptic plane => Bz =0 ! Only disturbed types of solar wind may be geoeffective.

Large-scale types of solar wind (From Yermolaev, Cos.Res.,1990; Planet. Space Sci., 1991)

General concept of storm effectiveness of solar and interplanetary events Fast stream Slow stream

Aims of research Occurrence rate of different types of solar wind Geoeffectiveness (number of selected type of solar wind resulted in magnetic storm with Dst < - 50 nT divided by total number of this type) Efficiency (with `output/input` criteria) in generation of magnetic storms by different types of solar wind

Example of OMNI data and calculated parameters in our database ftp://ftp.iki.rssi.ru/pub/omni (  left) and identification of solar wind types ftp://ftp.iki.rssi.ru/pub/omni/catalog/ (  bottom) ftp://ftp.iki.rssi.ru/pub/omni

Yearly number of different types of large-scale solar wind phenomena Heliospheric current sheet HCS ~ 124±81per year (maximum near solar minimum) Corotating interaction region CIR ~ 63±15 (at decrease of cycle) Interplanetary СМЕ or Ejecta ~ 99±38 (at increase and decrease of cycle) Magnetic cloud МС ~ 8±7 (at decrease of cycle) Sheath before Ejecta and МС are observed at half of Ejecta и МС (near maximum of cycle)

Durations of different types of large-scale solar wind phenomena ~ 29±5 h for IСМЕ (Ejecta), ~ 24±11 for magnetic cloud МС, ~ 20±4 for CIR, ~16±3 for Sheath before ICME (Ejecta), ~ 9±5 for Sheath before MC, ~5±2 for HCS.

Distribution of different types of solar wind during

Distribution of interplanetary sources of magnetic storms

Distribution of interplanetary sources of magnetic storms (taking data gaps into account)

Distribution of interplanetary sources of magnetic storms

Geoeffectiveness of different types of large-scale solar wind phenomena Geoeffectiveness solar wind phenomena

Duration of main phases of magnetic storms and double superposed epoch method

Behavior of parameters obtained by double superposed epoch method

Variations of parameters obtained by double superposed epoch method

Behavior of solar wind parameters in various types of streams during magnetic storms with Dst ≤ –50 nT

Connection of magnetospheric indexes with Bz component of IMF

Connection of magnetospheric indexes with Ey component of electric field

Efficiency of various types of solar wind streams

Number of events N, geoeffectiveness (probability) P and efficiency Ef=Dst/Ey

Conclusions On the basis of our «Catalog of large-scale solar wind phenomena during » (see data on site ftp://ftp.iki.rssi.ru/omni/ and paper by Yermolaev et al., Cosmicftp://ftp.iki.rssi.ru/omni/ Research, 2009, №2) we obtained: 1. Occurrence rate of different types of solar wind:  average number: 124±81 events per year for HCS, 8±6 for МС, 99±38 for Ejecta, 46±19 for Sheath before Ejecta, 6±5 for Sheath before МС, и 63±15 for CIR;  duration of events: ~ 29±5h for Ejecta, ~ 24±11 for МС, ~ 20±4 for CIR, ~16±3 for Sheath before Ejecta, ~ 9±5 for Sheath before MC, ~5±2 for HCS;  Time distribution: steadt types of solar wind (FAST+ SLOW + HCS) 60%, CIR 10%, MC 2%, EJECTA 20%, Sheath 9%. 2. Geoeffectiveness of events: for MC, for Ejecta, for CIR, for MC with Sheath, for MC without Sheath, for Ejecta with Sheath, 0.08 for Ejecta without Sheath. These results are published in Cosmic Research. 2009, № 5 and 2010, № 1

Conclusions(2) 3. Efficiency Dependencies of Dst (or Dst*) on the integral of Bz (or Ey) over time are almost linear and parallel for different types of drivers (time evolution of main phase of storms depends not only on current values of Bz and Ey but also on their prehistory). We estimated efficiency of storm generation as “output/input”= Dst/integated Ey(Bz) ratio. Efficiency of storm generation by MC is the lowest one (i.e. at equal values of integrated Bz or Ey the storm is smaller than for another drivers) and Efficiency for Sheath is the highest one. Several results have been published in Ann.Geophys and Journal Geophys. Res., 2012 may be found in