Elemental Abundance variations of the Suprathermal Heavy Ion Population over solar cycle 23 M. Al Dayeh, J.R. Dwyer, H.K. Rassoul Florida Institute of.

Slides:

Advertisements

Similar presentations

SHINE 2008 Introduction Energetic ElectronsFluence AnalysisSummary George C. Ho and Glenn M. Mason The Johns Hopkins University Applied Physics Laboratory,

Advertisements

M.E. Wiedenbeck, JPL/Caltech Thanks to: the ACE/ULEIS &SIS Teams and the STEREO/LET, SIT, & SEPT Teams 9 June 20101ACE/SOHO/STEREO/Wind Workshop.

Heavy Ion Abundances in Large Solar Energetic Particle Events Spring AGU 2006, SH43B-04 Heavy Ion Abundances in Large Solar Energetic Particle Events Spring.

The Johns Hopkins University Applied Physics Laboratory SHINE 2005, July 11-15, 2005 Transient Shocks and Associated Energetic Particle Events Observed.

M. I. Desai Longitudinal Distribution of suprathermals and SEPs -- New Insights from ACE, Wind, and STEREO Southwest Research Institute, San Antonio, TX,

SEP Data Analysis and Data Products for EMMREM Mihir I. Desai & Arik Posner Southwest Research Institute San Antonio, Texas Mihir I. Desai & Arik Posner.

1 SEP Spectral and Compositional Variability at High Energies Tylka et al., ApJ 625, (2005) Tylka et al, ApJS 164, (2006) Tylka and Lee,

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

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.

Session A Wrap Up. He Abundance J. Kasper Helium abundance variation over the solar cycle, latitude and with solar wind speed Slow solar wind appears.

Explaining the Acceleration and Transport of Solar Energetic Particles C.M.S. Cohen Caltech And still trying....

Solar Energetic Particles and Shocks. What are Solar Energetic Particles? Electrons, protons, and heavier ions Energies – Generally KeV – MeV – Much less.

CME Workshop Elmau, Feb , WORKING GROUP C: ENERGETIC PARTICLE OBSERVATIONS Co-Chairs: Klecker, Kunow SUMMARY FROM WORKSHOP 1 Observations Questions.

Probing Ion Acceleration by Observing Gamma Rays from Solar Flares Albert Y. Shih 1 NASA Advisor: Brian R. Dennis 2 Faculty Advisor: Robert P. Lin 1 1.

Space Science MO&DA Programs - December Page 1 SS Interplanetary Propagation of Ions From Impulsive Solar Flares: ACE/ULEIS Data Impulsive solar.

Using Gamma Rays to Measure Accelerated Ions and Electrons and Ambient Composition Gerald Share 1,2, Ronald Murphy 2, Benz Kozlovky 3, and Juergen Kiener.

National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology A New JPL Interplanetary Solar High- Energy.

Constraints on Particle Acceleration from Interplanetary Observations R. P. Lin together with L. Wang, S. Krucker at UC Berkeley, G Mason at U. Maryland,

STEREO IMPACT Critical Design Review 2002 November 20,21,22 1 LET Performance Requirements Presenter: Richard Mewaldt

CME Workshop Elmau, Feb , WORKING GROUP C: ENERGETIC PARTICLE OBSERVATIONS Co-Chairs: Klecker, Kunow SUMMARY FROM SESSION 1B Discussion of.

High-Cadence EUV Imaging, Radio, and In-Situ Observations of Coronal Shocks and Energetic Particles: Implications for Particle Acceleration K. A. Kozarev.

Sinaia, September 6-10, Berndt Klecker Max-Planck-Institut für extraterrestrische Physik, Garching, Germany Workshop on Solar Terrestrial Interactions.

SHINE 2006 WG2/3 - CIRs & Energetic Particles 1 Review of CIR-related Particle Composition, Charge States, & Energy Spectra Joe Mazur The Aerospace Corporation.

Solar Energetic Particle Events: An Overview Christina Cohen Caltech.

26 June 2008SHINE, Zermatt, UT1 High-energy Elemental, Isotopic, and Charge-State Composition in 3 He-rich Solar Energetic Particle Events M.E. Wiedenbeck.

IHY Workshop A PERSONAL VIEW OF SOLAR DRIVERS for Solar Wind Coronal Mass Ejections Solar Energetic Particles Solar Flares.

Outstanding Issues Gordon Holman & The SPD Summer School Faculty and Students.

Observational Tests of Suprathermal Particle Acceleration (Dayeh/Hill  Hill/Desai) WORKING GROUP SUMMARY.

1 July 14, SHINE WorkshopKeauhou, Hawaii, USA Chanruangrith Channok, 1 David Ruffolo, 1 Mihir Desai, 2 and Glenn Mason 2 1 THAILAND 2 USA Finite-Time.

Ion Acceleration Near CME-driven shocks Paper No. 84, SH1.3 ICRC 2011, Beijing, China Ion Acceleration Near CME-driven shocks Paper No. 84, SH1.3 ICRC.

Spectral Properties of Heavy Ions Associated with Interplanetary Shocks at 1 AU SHINE 2004 Big Sky, Montana M. I. Desai University of Maryland, College.

Solar Energetic Particles: recent observational progress for shock-related and impulsive events Glenn Mason 1, Mihir Desai 1, Joe Mazur 2, and Joe Dwyer.

The SEP Acceleration and Transport Link of the Chain

Coronal Sources of Impulsive Fe-Rich Solar Energetic Particle Events S. W. Kahler AFRL Space Vehicles Directorate, Kirtland AFB, NM, USA D. V. Reames IPST,

ACE Page 1 ACE ACE PresentorInstitution. ACE Page 2 ACE Mass Fractionation in the Composition of Solar Energetic Particles Although it is well known that.

LASCO C2 Jan 24, 2006, www image Future progress understanding Solar Energetic Particles Glenn Mason, JHU/APL 10th RHESSI Workshop Annapolis, MD August.

SEP Acceleration C.M.S. Cohen Caltech. Outline Shock acceleration in the IPM –ESP events –Observations vs theory –Observations driving theory Flare acceleration.

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.

Project: Understanding propagation characteristics of heavy ions to assess the contribution of solar flares to large SEP events Principal Investigator:

He + Increase in SEP Events with a High Source Temperature and Implication for Acceleration Site ICRC, 2011, Beijing Z. Guo; E. Moebius; M. Popecki Space.

Review of Observations of Particles From Solar Flares and Their Clues to the Structure of the IMF Joe Mazur The Aerospace Corporation Glenn Mason Johns.

1 SEP “Campaign Events” for SHINE 2003 Question: Can we identify solar/interplanetary factors that drive SEP spectral and compositional variability at.

SHINE SEP Campaign Events: Detailed comparison of active regions AR9906 and AR0069 in the build-up to the SEP events of 21 Apr 2002 and 24 Aug 2002 D.

Composition and spectral properties of the 1 AU quiet- time suprathermal ion population during solar cycle23 M Al-Dayeh, M I Desai, J R Dwyer, H K Rassoul,

Pre-accelerated seed populations of energetic particles in the heliosphere N. A. Schwadron* and M. Desai Southwest Research Institute *Also, Boston University.

SHINE 2006 Student Day Working Group III summary Zermatt, Utah, July 31 - August 4 Gang Li.

Observations of Broad Longitudinal Extents of 3 He-rich SEP Events M.E. Wiedenbeck 1, G.M. Mason 2, C.M.S. Cohen 3, N.V. Nitta 4, R. Gómez-Herrero 5, D.K.

The Suprathermal Tail Properties are not well understood; known contributors Heated solar wind Interstellar and inner source pickup ions Prior solar and.

Solar Energetic Particles (SEP’s) J. R. Jokipii LPL, University of Arizona Lecture 2.

Variability of the Heliospheric Magnetic Flux: ICME effects S. T. Lepri, T. H. Zurbuchen The University of Michigan Department of Atmospheric, Oceanic,

Composition and spectral properties of the quiet-time suprathermal ion population ACE Team meeting October 13-14, 2008 M Al-Dayeh 1, M I Desai 1, J R Dwyer.

Introduction to SEPs Christina Cohen Caltech. Outline What are SEPs? ›And why do we care? How are the measured? ›on the ground ›in space What is the SEP.

1 Introduction to the SHINE Campaign Events 2002 April 21 and 2002 August 24 Allan J. Tylka Code 7652, Naval Research Laboratory, Washington DC 20375

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.

Particle spectra at CME-driven shocks and upstream turbulence SHINE 2006 Zermatt, Utah August 3rd Gang Li, G. P. Zank and Qiang Hu Institute of Geophysics.

Southwest Research Institute

Elemental Abundance variations of the Suprathermal Heavy Ion Population over solar cycle 23 M. Al Dayeh, J.R. Dwyer, H.K. Rassoul Florida Institute of.

Spectral Properties of Large Gradual Solar Energetic Particle Events

Measurements of Suprathermal Ions in the Inner Heliosphere from Solar Probe Plus and Solar Orbiter George C. Ho SPP SWT September 14-15th, 2016.

George C. Ho1, David Lario1, Robert B. Decker1, Mihir I. Desai2,

LET Performance Requirements Presenter: Richard Mewaldt

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

Student Day Working Group III summary

Organizers: Mihir Desai, Joe Giacalone, Eric Christian

Relative abundances of quiet-time suprathermal ions at 1 AU

Conveners: M. A. Dayeh (SwRI), R. Bucik (MPS/UG), and C. Salem (UCB)

Solar Energetic Particle Spectral Breaks

ACE Reveals Isotopic Composition of Interstellar Material

Presentation transcript:

Elemental Abundance variations of the Suprathermal Heavy Ion Population over solar cycle 23 M. Al Dayeh, J.R. Dwyer, H.K. Rassoul Florida Institute of Technology, Melbourne, FL 32901, USA M. I. Desai Southwest Research Institute, San Antonio, TX, 78238, USA G. M. Mason Johns Hopkins University, Applied Physics Laboratory, Laurel MD 20723, USA and J. E. Mazur The Aerospace Corporation, El Segundo, CA 92957, USA SHINE Workshop, Zermatt, Utah July 30, 2006

Energetic particle populations in the heliosphere

Solar Energetic Particle (SEP) Events “Small”Event Spatial Size “Big” ~hoursDuration~days ~1000 / year over the whole SunFrequency at Solar Max ~10 / year Restricted to magnetically-connected longitudes, ~W30-W80 Source LocationOver the whole Sun ~1.0Event-Integrated Fe/O ~ x – 1000x enhancements *Trans-Fe (30 < Z < 82) Nominal coronal values ~16-20 Fe Charge States ~10-14 ~ 1 3He/4He~ Resonant wave-particle interactions at Flare/Reconnection Site Acceleration Mechanism Shock, driven by fast CME

SEPs at Earth Satellites Radiation Health Ground based systems Supra- thermals Ambient Corona and Solar Wind Previous SEP accelerated material (Remnants) Seed Particles Coronal & Interplanetary Shocks (Fast CMEs) Statement of the problem Complicated recipe: Mixed ingredients Particle Transport Diffusive acceleration Particle-Plasma Wave Interactions

More complications: Large elemental abundance variability within Gradual events. A zoo of energy spectra (spectral breaks!). Big Questions still not answered: Acceleration mechanisms? [shocks, flares] Transport effects? [elemental abundances/spectra] Accelerated material? [Coronal/SW, Flare]

(Mewaldt et al., 2001 AIP conference Proceedings 598, 165) Seed particles?

Instrumentation Ultra Low Energy Isotope Spectrometer (ULEIS): Launched onboard ACE on August 25, 1997 Time of Flight Mass Spectrometer Measured species: Protons to Gold Energy range: 45 keV to few MeV/nuc Instrument geometrical factor: ~1.3 cm 2 sr Supra Thermal Energetic Particle Telescope (STEP): Launched onboard Wind on November 1, 1994 Time of Flight Mass Spectrometer Measured species: Protons to Fe Energy range: ~30 keV to ~2 MeV/nuc Instrument geometrical factor: 2 x 0.4 cm 2 sr

Data Set: Survey of 52 Gradual events at the suprathermal energy range 45 well detected by Wind and ACE of which 32 have known solar liftoff location Selection Criteria: Temporal intensity profile Velocity dispersion Excluded: Shocks, upstream events, saturation times Work being done MeV/nuc

C/O at low energies: F C F NO F Ne Correction Matrix

Solar Cycle variation of C/O, NeS/O, and Fe/O at MeV/nuc  Clear dependence on the solar cycle Solid plot: 27-day running average Symbols: Annual averages

Solar Cycle Compositional Variation in SEP events  No dependence on the solar cycle  Large event-to-event fluctuations  Remnant flare signature

C/O and Fe/O Energy dependence  constant C/O  Fe/O decreases with increasing energy  Rigidity effect

Case study: STEP and ULEIS C/O data at MeV/nuc  Why such a large difference ?

Case study: STEP and ULEIS C/O data at MeV/nuc  Why such a large difference ?

Case study: STEP and ULEIS C/O data at MeV/nuc  Not an azimuthal effect  Efficiency check?

Summary 1.C/O, NeS/O, and Fe/O daily variations show solar cycle dependence at low energies (0.08 MeV/nuc to 0.32 MeV/nuc). 2.LSEPs C/O and Fe/O ratios show large event-to-event fluctuations and no dependence on the solar cycle or solar longitude. 3.At solar maximum, ACE\ULEIS measures a high C/O values compared to Wind\STEP; the difference is on the order of 30%. This difference does not appear to be an azimuthal sampling or instrumental effect; more investigation will be done in the near future. 4.C/O stays constant with increasing energy while Fe/O decreases. We suggest that this behavior is due to acceleration preference based on rigidity effects where the higher the rigidity (Fe), the lower the acceleration efficiency.

Thank you M.A.D 2006