EVENT of 20 JANUARY 2005 INJECTION TIME of IONS, PROTONS and ELECTRONS

Slides:



Advertisements
Similar presentations
High Energy Astrophysics Jim Ryan University of New Hampshire.
Advertisements

NBYM 2006 A major proton event of 2005 January 20: propagating supershock or superflare? V. Grechnev 1, V. Kurt 2, A. Uralov 1, H.Nakajima 3, A. Altyntsev.
Investigating the Origin of the Long-Duration High- Energy Gamma-Ray Flares Gerry Share, Jim Ryan and Ron Murphy (in absentia) Steering Committee Overseer.
The Johns Hopkins University Applied Physics Laboratory SHINE 2005, July 11-15, 2005 Transient Shocks and Associated Energetic Particle Events Observed.
On the link between the solar energetic particles and eruptive coronal phenomena On the link between the solar energetic particles and eruptive coronal.
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.
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.
R. P. Lin Physics Dept & Space Sciences Laboratory University of California, Berkeley The Solar System: A Laboratory for the Study of the Physics of Particle.
Hot Precursor Ejecta and Other Peculiarities of the 2012 May 17 Ground Level Enhancement Event N. Gopalswamy 2, H. Xie 1,2, N. V. Nitta 3, I. Usoskin 4,
Extreme CME Events from the Sun Nat Gopalswamy NASA/GSFC Extreme Space Weather Events (ESWE) workshop, Boulder, CO May 14-17, 2012.
SH1 and SH2.1 (Sun & Corona, IP Transport) C. M. S. Cohen (Caltech)
Solar Energetic Particles and Shocks. What are Solar Energetic Particles? Electrons, protons, and heavier ions Energies – Generally KeV – MeV – Much less.
Five Spacecraft Observations of Oppositely Directed Exhaust Jets from a Magnetic Reconnection X-line Extending > 4.3 x 10 6 km in the Solar Wind Gosling.
CME Workshop Elmau, Feb , WORKING GROUP C: ENERGETIC PARTICLE OBSERVATIONS Co-Chairs: Klecker, Kunow SUMMARY FROM WORKSHOP 1 Observations Questions.
Institute of Astronomy, Radio Astronomy and Plasma Physics Group Eidgenössische Technische Hochschule Zürich Swiss Federal Institute of Technology, Zürich.
Working Group 2 - Ion acceleration and interactions.
Solar Flare Particle Heating via low-beta Reconnection Dietmar Krauss-Varban & Brian T. Welsch Space Sciences Laboratory UC Berkeley Reconnection Workshop.
Temporal Variability of Gamma- Ray Lines from the X-Class Solar Flare of 2002 July 23 Albert Y. Shih 1,2, D. M. Smith 1, R. P. Lin 1,2, S. Krucker 1, R.
GEANT-4/Spenvis User Meeting November 2006 Solar Energetic Particle Modelling Activities at ESA A.Glover 1, E. Daly 1,A. Hilgers 1, SEPEM Consortium 2.
Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,
CME Workshop Elmau, Feb , WORKING GROUP C: ENERGETIC PARTICLE OBSERVATIONS Co-Chairs: Klecker, Kunow SUMMARY FROM SESSION 1B Discussion of.
Solar Energetic Particles -acceleration and observations- (Two approaches at the highest energy) Takashi SAKO Solar-Terrestrial Environment Laboratory,
Solar Origin of energetic particle events Near-relativistic impulsive electron events observed at 1 AU M. Pick, D. Maia, S.J. Wang, A. Lecacheux, D. Haggery,
High-Cadence EUV Imaging, Radio, and In-Situ Observations of Coronal Shocks and Energetic Particles: Implications for Particle Acceleration K. A. Kozarev.
SHINE 2008 June, 2008 Utah, USA Visit our Websites:
Radiation conditions during the GAMMA-400 observations:
Finite Gyroradius Effect in Space and Laboratory 1. Radiation belt (Ring current) 2. Auroral phenomena (Substorm current) 3. Shock acceleration and upstream.
Solar Energetic Particle Events: An Overview Christina Cohen Caltech.
Title Relativistic Solar Particle Events of 19 th Solar Cycle: Modeling Study Yu.V. Balabin, E.V. Vashenuyk, B.B. Gvozdevsky Polar Geophysical.
IHY Workshop A PERSONAL VIEW OF SOLAR DRIVERS for Solar Wind Coronal Mass Ejections Solar Energetic Particles Solar Flares.
Decay Phase of Proton and Electron SEP Events E.I. Daibog 1, K. Kecskeméty 2, Yu.I. Logachev 1 1 Skobeltsyn Inst. of Nuclear Physics, Moscow State Univ.,
The PLANETOCOSMICS Geant4 application L. Desorgher Physikalisches Institut, University of Bern.
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.
1 20 January 2005: Session Summary SHINE 2006 Zermatt, Utah, 31 July - 4 August Invited Talks Riley: what was the Alfven speed in the corona at.
Operation of the Space Environmental viewing and Analysis Network (Sevan) in 24-th Solar Activity Cycle A. Chilingarian A. Chilingarian Yerevan Physics.
Project: Understanding propagation characteristics of heavy ions to assess the contribution of solar flares to large SEP events Principal Investigator:
A comparison of CME-associated atmospheric waves observed in coronal (Fe XII 195A) and chromospheric ( He I 10830A) lines Holly R. Gilbert, Thomas E. Holzer,
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.
Cosmic Rays at 1 AU Over the Deep Solar Minimum of Cycle 23/24 Cosmic Ray Transport in the Helioshealth: The View from Voyager AGU Fall Meeting San Francisco,
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,
Ion Acceleration in Solar Flares Determined by Solar Neutron Observations 2013 AGU Meeting of the Cancun, Mexico 2013/05/15 Kyoko Watanabe ISAS/JAXA,
1 SEP Timing Studies: An Excruciatingly Brief Review Allan J. Tylka US Naval Research Laboratory, Washington DC SHINE 2006 Where was the CME when the SEPs.
Earth’s Magnetosphere Space Weather Training Kennedy Space Center Space Weather Research Center.
SOLAR COSMIC RAYS AND OZONE LAYER OF THE EARTH (3D modeling) M27 Alexei Krivolutsky 1, Georgy Zakharov 1, Tatyana Vyushkova 1, Alexander Kuminov 1, and.
Interplanetary proton and electron enhancements associated with radio-loud and radio-quiet CME-driven shocks P. Mäkelä 1,2, N. Gopalswamy 2, H. Xie 1,2,
George C. Ho1, David Lario1, Robert B. Decker1, Mihir I. Desai2,
A Relation between Solar Flare Manifestations and the GLE Onset
ARTEMIS – solar wind/ shocks
Solar Radio Imaging Array SIRA
Coupled ion acceleration and
Suprathermal Particle Density Variations over the Solar Cycle
Particle Acceleration at Coronal Shocks: the Effect of Large-scale Streamer-like Magnetic Field Structures Fan Guo (Los Alamos National Lab), Xiangliang.
Modeling the SEP/ESP Event of December 13, 2006
N. Gopalswamy, H. Xie, S. Akiyama, P. Mäkelä, S. Yashiro, I. Usoskin
D.N. Baker, S. Kanekal, X. Li, S. Elkington
Solar Flare Energy Partition into Energetic Particle Acceleration
Karl-Ludwig Klein & Rositsa Miteva
Alexei Struminsky1,2  1 Space Research Institute
SMALL SEP EVENTS WITH METRIC TYPE II RADIO BURSTS
Quantification of solar wind parameters from measurments by SOHO and DSCOVR spacecrafts during series of Interplanetary Coronal Mass Ejections in the.
Detection of Solar Neutrons and Protons by the ground level detectors
Forbush and GCRDs First rigorous experimental observation of Cosmic Ray Flux Decrease was obtained by S. E. Forbush in , after deep statisitcal.
SEP EVENTS AND THE ROLE OF FLARES AND SHOCKS
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.
SIDC Space Weather Briefing
SIDC Space Weather Briefing
SIDC Space Weather Briefing
Max-Planck-Institut für extraterrestrische Physik
Presentation transcript:

EVENT of 20 JANUARY 2005 INJECTION TIME of IONS, PROTONS and ELECTRONS Hamlet Martirosyan YERPHI / CRD

INJECTION TIME of FIRST REGISTRATED IONS He, C, O, Mg, Fe Collisionless Propagation , ΔT = L/c *1/β , T(Injection) = T(Registration)- ΔT

Ion Propagation Collisionless or diffusion? ΔT ~ L2/D ~ L2/ V.λ λ= λoR2-δ T(Regist)=a.(Etotal/Z).R δ-3+T(Inject)

Light ions Collisionless Propagation

Z - dependence INJECTION TIME of IONS Ions of All Energies the Given Type were Injected Simultaneously (Injection - Energy independence) Z - dependence

Simultaneous registration of protons

Protons Injection Time Shock Speed - ~700Km/s Flare Coordinate - N12W58 Mag. Field Line Nominal Length ~1.017au Simultaneous registration of protons tinject=tregist – Δt (Δt - Real Propagation Time) Δt(E) ≥ 1.017au / Vp(E)

Protons Injection and Registration Time

PROTONS ACE / EPAM , GOES

Electrons WIND

Neutron Monitors NM Rc GV GLE Start Oulu 0.8 6:51UT Sanae 1.06 6:49UT Yakutsk 1.7 6:50UT Kiel 2.29 6:51UT Moscow 2.46 6:51UT Novosibir 2.91 6:53UT Lomnicki 4 6:55UT Hermanus 4.9 7:00UT Jungfrau. 4.48 6:59UT Bacsan 5.6 7:00UT Alma Ata 6.61 7:03UT Aragats 7.6 7:05UT

NEUTRON MONITORS GLE START

RELATIVISTIC ENERGY REGION NEUTRON MONITORS GLE START and INJECTION TIME

PROTONS 100Mev <E< 500Mev GOES E > 0.5GEV NUTRON MONITORS

ELECTRONS E > 20Kev EInject ~LnLn(E)

INJECTION of IONS, PROTONS and ELECTRONS

PROTONS FLUX CORRELATION

CONCLUSION I AREA of ACCELERATION High Energy Protons (E > 100Mev) and Electrons (E > 20Kev) were accelerated and injected in the flare . Protons Injection 6:36 – 6:56UT Electrons Injection 6:33 – 6:43UT All Ions were accelerated and injected on a shock wave . Ions Injection 6:48 – 7:10UT Flare Start 6:28UT CME Onset 6:33UT (N. Gopalswamy et al.)

CONCLUSION II ACCELERATION RATE HIGH ENERGY PROTONS (E > 50Mev) TInject(E) = 3.05*E + 9.26 => dE/dT ~ Const >0 HIGH ENERGY ELECTRONS (E > 20Kev) TInject(E) = 26.6*LnLn(E) – 29.475 => dE/dT ~ E*Ln(E), E=E0*exp(exp(ατ))

LOW ENERGY PROTONS and ELECTRONS Formation of E < 50 Mev Protons E < 20 Kev Electrons in Interplanetary Space Acceleration or deacceleration ?

LOW ENERGY PROTONS and ELECTRONS DEACCELERATION VERSION

INTERACTIVE SOLAR WIND or «ANTI _ SHOCK»

INTERACTIVE SOLAR WIND «ANTI - SHOCK» 8 NOVEMBER 2000

ASEC Monitors Data