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,

Slides:

Advertisements

Similar presentations

Cosmic Rays and Space Weather

Advertisements

1 Belov A., Baisultanova L., Eroshenko E., Yanke V. (IZMIRAN, Russia), Mavromichalaki H. (Athens University, Greece), Pchelkin V. (PGI, Russia) Magnetospheric.

THREE-DIMENSIONAL ANISOTROPIC TRANSPORT OF SOLAR ENERGETIC PARTICLES IN THE INNER HELIOSPHERE CRISM- 2011, Montpellier, 27 June – 1 July, Collaborators:

Investigation of daily variations of cosmic ray fluxes in the beginning of 24 th solar activity cycle Ashot Chilingarian, Bagrat Mailyan IHY-ISWI Regional.

Cosmic Ray Using for Monitoring and Forecasting Dangerous Solar Flare Events Lev I. Dorman (1, 2) 1. Israel Cosmic Ray & Space Weather Center and Emilio.

NMDB Kiel Meeting, 3-5/12/2008 On the possibility to use on-line one-minute NM data of NMDB network and available from Internet satellite CR data for.

Study of Galactic Cosmic Rays at high cut- off rigidity during solar cycle 23 Partha Chowdhury 1 and B.N. Dwivedi 2 1 Department of Physics, University.

Petukhov I.S., Petukhov S.I. Yu.G. Shafer Institute for Cosmophysical Research and Aeronomy SB RAS 21st European Cosmic Ray Symposium in Košice, Slovakia.

Cosmic Rays and Space Weather Erwin O. Flückiger Laurent Desorgher, Rolf Bütikofer, Benoît Pirard Physikalisches Institut University of Bern

21 ECRS, Kosice, 12/09/2008 Trapped charge particles measurements in the radiation belt by PAMELA instrument Vladimir V. Mikhailov (MEPHI) for PAMELA collaboration.

Bastille Day 2000 Solar Energetic Particles Event: Ulysses observations at high heliographic latitudes M. Zhang Florida Institute of Technology.

Towards a European Infrastructure for Lunar Observatories Bremen, Wednesday 23 rd March 2005 A 3D cosmic ray detector on the Moon X. Moussas University.

PHOEBUS* on LISA: A Proposal for Solar Physics on LISA INFN-SPAZIO/2 Riunione sulle prospettive della Fisica Astroparticellare nello spazio LNF, 16 Febbraio.

Belle Tamir, Sharet High School Nitzan Atia, Tchernichovsky High School Netanya, Israel.

1 Interactive DataBase of Cosmic Ray Anisotropy (DB A10) Asipenka A.S., Belov A.V., Eroshenko E.F., Klepach E.G., Oleneva V. A., Yanke, V.G. IZMIRAN, Pushkov.

SHINE 2008 June, 2008 Utah, USA Visit our Websites:

Efficacy of Muon Detection for Solar Flare Early Warning Canadian Muon Workshop St-Émile-de-Suffolk, Québec, Canada October 17-19, 2011 NRCan DND Carleton.

ОПАСНОСТИ МАГНИТНЫХ БУРЬ И ВОЗМОЖНОСТИ ИСПОЛЬЗОВАНИЯ МИРОВОЙ СЕТИ НЕЙТРОННЫХ МОНИТОРОВ И МЮОННЫХ ТЕЛЕСКОПОВ ДЛЯ ПРЕДСКАЗАНИЯ ПОДХОДА К ЗЕМЛЕ МОЩНЫХ МЕЖПЛАНЕТНЫХ.

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

CME-GEOMETRY AND COSMIC-RAY ANISOTROPY OBSERVED BY A PROTOTYPE MUON DETECTOR NETWORK K. Munakata 1, T. Kuwabara 1, J. W. Bieber 2, P. Evenson 2, R. Pyle.

SHINE Meeting, July 31 – August 4, 2006 Neutron Monitor Observations of the January 20, 2005 Ground Level Enhancement John W. Bieber 1, John Clem 1, Paul.

ESWW10, Antwerpen, 2013 Cosmic ray variations caused by magnetic clouds in the interplanetary disturbances A. ABUNIN,M., ABUNINA, A. BELOV, E. EROSHENKO,

Title Relativistic Solar Particle Events of 19 th Solar Cycle: Modeling Study Yu.V. Balabin, E.V. Vashenuyk, B.B. Gvozdevsky Polar Geophysical.

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

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

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.

CME trajectory deduced from cosmic ray measurements K. Munakata, T. Kuwabara and J. W. Bieber.

IMF Prediction with Cosmic Rays THE BASIC IDEA: Find signatures in the cosmic ray flux that are predictive of the future behavior of the interplanetary.

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

1 IGY The ALERT signal of ground level enhancements of solar cosmic rays: physics basis, the ways of realization and development Anashin V., Belov A.,

NMDB - the European neutron monitor database Karl-Ludwig Klein, for the NMDB consortium.

IMF Prediction with Cosmic Rays THE BASIC IDEA: Find signatures in the cosmic ray flux that are predictive of the future behavior of the interplanetary.

Solar cycle dependence of EMIC wave frequencies Marc Lessard, Carol Weaver, Erik Lindgren 1 Mark Engebretson University of New HampshireAugsburg College.

Exploitation of Space Ionizing Radiation Monitoring System in Russian Federal Space Agency STRUCTURE OF THE MONITORING SYSTEM The Monitoring System includes.

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

IAGA Symposium A12.2 Geomagnetic networks, computation and definition of products for space weather and space climate Melbourne, Australia, 2011 GLOBAL,

Japan, ICRC 2003 Daejeon, UN/ESA/NASA/JAXA Workshop, Sept 2009 Satellite Anomalies and Space Weather By Lev Dorman for INTAS team (A. Belov, L. Dorman,,

20th ESA Symposium Lev Dorman (1, 2) for the Team (A. Belov, I. Ben Israel, U. Dai, L. Dorman,, E. Eroshenko, N. Iucci, Z. Kaplan, O. Kryakunova, A. Levitin,

Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University.

Athens University – Faculty of Physics Section of Nuclear and Particle Physics Athens Neutron Monitor Station Study of the ground level enhancement of.

ENERGY ESTIMATION OF THE INTERPLANETARY PLASMA DURING STRONGEST GEOMAGNETIC STORMS OF THE CURRENT 24 SOLAR CYCLE ON MARCH 2015 The geomagnetic storms.

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

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.

Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy of SB RAS Transparency of a magnetic cloud boundary for cosmic rays I.S. Petukhov, S.I. Petukhov.

Understanding SEP properties through Neutron Monitor data modeling Neutron Monitor Network: a tool for revealing the relativistic SEP properties Ground.

It is considered that until now in the 24th cycle of solar activity 2 ground level enhancements of solar cosmic rays (GLEs) are registered: on May 17,

THREE-DIMENSIONAL ANISOTROPIC TRANSPORT SIMULATIONS: A PARAMETER STUDY FOR THE INTERPRETATION OF MULTI-SPACECRAFT SOLAR ENERGETIC PARTICLE OBSERVATIONS.

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.

SEP Event Onsets: Far Backside Solar Sources and the East-West Hemispheric Asymmetry S. W. Kahler AFRL Space Vehicles Directorate, Kirtland AFB, New Mexico,

GLOBAL SURVEY METHOD: WHAT DO NEUTRON MONITORS SEE? Belov A.1, Eroshenko E.1, Abunin A. 1, Abunina M. 1, Yanke V. 1, Oleneva V.1, Mavromichalaki H.2, Papaioannou.

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

1 Temperature effect of the muon component of cosmic ray and practical possibilities of its accounting Berkova M., Belov A., Smirnov D., Eroshenko E.,

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

GLOBAL SURVEY METHOD: WHAT DO NEUTRON MONITORS SEE? Belov A.1, Eroshenko E.1, Abunin A. 1, Abunina M. 1, Yanke V. 1, Oleneva V.1, Mavromichalaki H.2, Papaioannou.

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,

Effects of January 2010 stratospheric sudden warming in the low-latitude ionosphere L. Goncharenko, A. Coster, W. Rideout, MIT Haystack Observatory, USA.

IMF Prediction with Cosmic Rays THE BASIC IDEA: Find signatures in the cosmic ray flux that are predictive of the future behavior of the interplanetary.

Earth’s Magnetosphere Space Weather Training Kennedy Space Center Space Weather Research Center.

GROUND-LEVEL EVENT (GLE)

ESA SSA Measurement Requirements for SWE Forecasts

A Relation between Solar Flare Manifestations and the GLE Onset

Magnetic Clouds: The Cylindrical Elliptic Approach

Presenter: Paul Evenson

Development of a GLE Alarm System Based Upon Neutron Monitors

Effects of Dipole Tilt Angle on Geomagnetic Activities

Ulysses COSPIN High Energy Telescope observations of cosmic ray and solar energetic particles intensities since its distant Jupiter flyby in 2004 R.B.

Quantification of solar wind parameters from measurments by SOHO and DSCOVR spacecrafts during series of Interplanetary Coronal Mass Ejections in the.

. Multipoint, galactic cosmic ray observations associated with a series of interplanetary coronal mass ejections: the case study of June 2015 A. Papaioannou1,

On the relative role of drift and convection-diffusion effects in the long-term CR variations on the basis of NM and satellite data Lev Dorman (1, 2) Israel.

NMDB - the European neutron monitor database

Presentation transcript:

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, Ionosphere and Radio Wave Propagation (IZMIRAN), 42092, Troitsk, Moscow Region, Russia (2) Nuclear and Particle Physics Section, Physics Department, Athens University Pan/polis-Zografos Athens, Greece 20 th ECRS, 5-8 September 2006, Lisboa Portugal Cosmic ray modulation in August-September 2005 Abstract During the burst of solar activity in August- September 2005, close to the minimum of the current solar cycle, a big amount of powerful X- ray flares was recorded. Among them the flare X17.0 on September 7, was outstanding. Within a relatively short period (22 August – 17 September) two severe magnetic storms were recorded as well as several Forbush effects, which have been studied using hourly mean variations of the cosmic ray density and anisotropy derived from the data of the neutron monitor network. The behavior of certain characteristics of the high energy cosmic rays during these Forbush effects is being analyzed together with interplanetary disturbances and their solar sources in comparison with the variations of the geomagnetic activity. A big and long enough cosmic ray pre-decrease is selected before the shock arrival on September 15,  Perturbation of the interplanetary space in August-September 2005 caused a series of modulation effects in CR, as a result of solar flare activity.  In the forming of this disturbed situation three eastern, one central and one western CMEs, associated with X-ray flares, took part.  Modulating effect of disturbed regions on the galactic cosmic rays revealed in a series of Forbush effects, three of which are distinguished by the magnitude of CR density decrease: August (amplitude 6.4% for the CR with rigidity 10GV), 11 September (12.1%) and 15 September (5.1%). In all these cases very fast shocks arrived at the Earth with the mean velocity of propagation exceeded 1100km/s.  Western (22.08) and eastern (07 and 09.09) flares were very remote sources, even in these cases significant effects in CR and in the Earth’s magnetosphere were recorded.  In the 15 th of September, a big and long lasted pre-decrease in the CR density preceded the shock arrival, which is clearly isolated also by the longitude and pitch-angle distribution of the CR intensity. Acknowledgments: This work is supported by the RFBR grants and , by the program of RAN Presidium ‘Neutrino Physics’, NSF grant ATM (USA & Canadian stations) and by Greek Project PYTHAGORAS II from European Social Funds and National Resources. We are also thankful to all collaborators providing continue ground level monitoring of the CR and to all researchers presenting operatively data on the satellite measurements on the internet  Belov A., Baisultanova L., Eroshenko E., Mavromichalaki H., Yanke V, Pchelkin V, Plainaki C., Mariatos G.: Magnetospheric effects in cosmic rays during the unique magnetic storm on November 2003, JGR, 110, A09S20, doi: /2005JA011067, 2005  Belov, A. V., J. W. Bieber, E. A. Eroshenko, P. Evenson, R. Pyle, and V. G. Yanke: Pitch-angle features in cosmic rays in advance of severe magnetic storms: neutron monitor observations, 27-th ICRC,.9, , 2001  Kiel M.: 2nd ESA SWW (14-18 November 2005) Holland, ‘Radiation Effects on Spacecraft over Countermeasures Selected Cases’ spaceweather.net/spweather/workshops/eswwII/proc/Sessi on4/Presentation_KEIL.ppshttp:// spaceweather.net/spweather/workshops/eswwII/proc/Sessi on4/Presentation_KEIL.pps  Papaioannou, A., M. Gerontidou, G. Mariatos,,H. Mavromichalaki, C. Plainaki, E. Eroshenko, A. Belov, V. Yanke: ‘Unusually extreme cosmic ray events in July 2005’, 2nd ESA SWW (14-18 November 2005) Holland, wII/proc/Session1/SESWW-Papaioannou-Poster-pdf. wII/proc/Session1/SESWW-Papaioannou-Poster-pdf Conclusions References  Behavior of the CR density (А0) and ecliptic component of the CR anisotropy (Ах-Ау) with rigidity 10 GV during 9-13 (upper panel) & (lower panel) September Vertical vectors represent the north-south component of the anisotropy. Triangles mark timing of shock arrival.  Parameters of the solar wind (upper panel), density (A0) and anisotropy (Axy) of the CR (mid panel) and Dst and Kp indices of geomagnetic activity as well (lower panel).  Distribution of the CR variations by the asymptotic longitudes after deduction of the isotropic part (red circles-decrease of intensity, yellow-increase relatively to the base value; the size of circle is proportional to the variation magnitude; vertical lines are the timing of the shocks (upper panel); pitch angle distribution of the CR variations in two hours prior the SSC (lower panel) Cosmic Ray Modulation  Vm – mean velocity of the disturbance propagation from Sun to Earth; VH-product of the maximum SW velocity and IMF intensity in the fixed time near Earth; А0-the CR density variation, Аху- equatorial component of the CR anisotropy derived by GSM method.  Important eastern solar flares (X17; X6.2) were followed by significant proton fluxes, as for particles >10MeV it was increased up to pfu. Rosetta /SREM located 30 o behind the Earth at a distance ~1.3 AU, registered a proton flux ~ pfu.