ESP Spectral Evolution

Slides:

Advertisements

Similar presentations

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

Advertisements

Thick Target Coronal HXR Sources Astrid M. Veronig Institute of Physics/IGAM, University of Graz, Austria.

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

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

SEP Acceleration Mechanisms Dennis K. Haggerty and Edmond C. Roelof Johns Hopkins U./Applied Physics Lab. ACE/SOHO/STEREO/Wind Workshop Kennebunkport,

The Acceleration of Anomalous Cosmic Rays by the Heliospheric Termination Shock J. A. le Roux, V. Florinski, N. V. Pogorelov, & G. P. Zank Dept. of Physics.

Theory of Shock Acceleration of Hot Ion Populations Marty Lee Durham, New Hampshire USA.

Heavy ion spectral breaks in large SEP events LWS Team Meeting CIT, Pasadena, CA Jan 10 th -11 th, 2008 Gang Li.

Basic Statistical Concepts

Seed Population for Particle Acceleration... Anywhere in the Universe Shock heating based on many factors: v shock : shock speed  Bn : magnetic.

CIR Session Summary at Kennebunkport Marty Lee Durham, New Hampshire USA.

Shock Acceleration of Thermal and Hot Seed Ion Populations Martin A. Lee University of New Hampshire September 16-17, 2008.

1 Dynamic Motion of Bow Shock and Magnetopause Observed by THEMIS Hui Zhang (BU) Q.-G. Zong (Umass Lowell) D. G. Sibeck (GSFC) T. A. Fritz (BU)

Solar Energetic Particle Events: An Overview Christina Cohen Caltech.

STB CIR events #17,19,20,22 are from period Dec 2007-Feb 2008 (Bucik et al., AnGeo, 2009) these two bursts periods show an excess in number of counts beyond.

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

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

Foreshock studies by MEX and VEX FAB: field-aligned beam FAB + FS: foreshock M. Yamauchi et al.

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.

Ed Stone Symposium February 11, 2006 Voyager Observations of Galactic and Anomalous Cosmic Rays in the Heliosheath F.B. M c Donald 1, W.R. Webber 2, E.C.

How to Make Starlight (part 1) Chapter 7. Origin of light Light (electromagnetic radiation) is just a changing electric and magnetic field. Changing electric.

“Welcome to the Periodic Kingdom… … This is a land of the imagination, but it is closer to reality than it appears to be. This is the Kingdom of chemical.

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

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.

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

Matt Hill Gang Li SHINE 2007 Session summary for Shock geometry & upstream and downstream phenomena 1-day session: Tuesday morning Tuesday afternoon.

Blackbody Spectrum Remember that EMR is characterized by wavelength (frequency) Spectrum: distribution of wavelength (or frequency) of some EMR Blackbody:

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,

Joint session WG4/5 Points for discussion: - Soft-hard-soft spectral behaviour – again - Non-thermal pre-impulsive coronal sources - Very dense coronal.

Periodic Trends: Periodic Properties  Certain physical and chemical properties recur at regular intervals, and/or vary in regular fashion, when the elements.

Monitoring the Seyfert Galaxy Mkn766 Continuum and Fe line variability Mkn766 is a highly variable Seyfert 1 galaxy. The richness of.

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.

Tasks: Pasadena, 9/18/08. Exponential Rollovers Origin of double power laws? Need analysis and simulation. Correlating E and Q/A dependence; explore different.

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

Microwave emission from the trapped and precipitated electrons in solar bursts J. E. R. Costa and A. C. Rosal1 2005, A&A, 436, 347.

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

Coronal X-ray Emissions in Partly Occulted Flares Paula Balciunaite, Steven Christe, Sam Krucker & R.P. Lin Space Sciences Lab, UC Berkeley limb thermal.

Probing Turbulence At and Near CME-driven shocks Using Energetic Particle Spectra Living with a Star Team meeting Sep 18th, 2008 Pasadena, CA Gang Li From.

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.

SEPT/STEREO Observations of Upstream Particle Events: Almost Monoenergetic Ion Beams A. Klassen, R. Gomez-Herrero, R. Mueller-Mellin and SEPT Team, G.

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.

Low-energy Ion Distributions at the Termination Shock Rob Decker Johns Hopkins Univ., Applied Physics Lab., Laurel, MD SHINE, June-2008, Zermatt.

Observations of spectral shapes of suprathermal H +, He + and He ++ G. Gloeckler Department of Atmospheric, Oceanic and Space Sciences University of Michigan,

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

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,

Marty Lee Durham, New Hampshire USA

Session #8: Corotating Interaction Regions and the Connection Between Their Trailing Edge and Energetic Particle Acceleration at 1 AU Organizers: Robert.

Searching for Extreme SEP Events with STEREO

Progress Toward Measurements of Suprathermal Proton Seed Particle Populations J. Raymond, J. Kohl, A. Panasyuk, L. Gardner, and S. Cranmer Harvard-Smithsonian.

Two Years of NoRH and RHESSI Observations: What Have We Learned

Suprathermal Particle Density Variations over the Solar Cycle

Modeling the SEP/ESP Event of December 13, 2006

Organizers: Mihir Desai, Joe Giacalone, Eric Christian

Rick Leske, A. C. Cummings, R. A. Mewaldt, and E. C. Stone

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

Finding Order in ESP Events?

Periodic Trends: Periodic Properties

On the Spectral Components of the June 2000 Solar Energetic Particle Events J. Torsti, J. Laivola, P. Mäkelä, I-V. Lehtinen and O. Saloniemi Space Research.

Heavy-Ion Acceleration and Self-Generated Waves in Coronal Shocks

Geoffrey Reeves LANL.gov NewMexicoConsortium.org

V1 and V2 Measurements of Galactic and Anomalous Cosmic Rays in the Outer Heliosphere and the Heliosheath during Solar Cycle #23 W.R. Webber (The.

The spectral evolution of impulsive solar X-ray flares

Solar Energetic Particle Spectral Breaks

Current status Minjung Kim

Presentation transcript:

ESP Spectral Evolution C.M.S. Cohen, R.A. Mewaldt, G.M. Mason, J.C. Kasper, G.C. Ho, M.A. Lee

Study Motivation Saw unrolling of spectra before shock passage Point of unrolling varied with event Thought might be related to shock properties and how well confined ions were to shock region

Oct/Nov 2003 Solid = preshock Open = postshock Rollover point varies in energy from <1 to > 5 MeV/n

Event Selection Started with 400 shocks from 1997-2006 Examined 1 hour O intensities at 0.5, 1, and 3 MeV/n within ± 10 hours of shock Selected shocks with Peak intensities at 0.5 MeV/n within 2 hours of shock passage Peak intensity at 0.5 MeV/n > 2 times the intensity 5 hours before shock All 1 MeV/n intensities correspond to >5 counts 14 events selected

Examples of Selection Selected Not Sel. Not Sel.

Shock Evolution Examples Some shocks show unrolling (left) Some just show ‘lifting’ (right)

More Examples Unrolling point can differ in energy Bottom example has higher value than top example Unrolling ‘rate’ can differ Bottom example is more gradual than top example

Categorization Pre-shock spectra normalized to shock spectra, and again at 24 MeV/n point Cat 1 = unrolling (5 events) Cat 2 = lifting (4 events) Cat 3 = other Delta = reduction factor relative to shock value

Shock Parameters Cat 1 events show ~ correlation expected between power law index and compression ratio (ala DSA) Cat 2 events are harder than DSA predicts

Delta Values Not correlated with density compression ratios

Delta Values Not correlated with density compression ratios Not correlated with Theta but larger for slower shocks

Change in Delta values with energy and time (i.e. unrolling rate) Unrolling rate (between 5 and 2 hours pre-shock) is slower for stronger shocks A sign of better confinement??

Protons Started similar analysis with proton data EPAM GOES Complications because GOES is in different position (so need to time shift data but by how much?) the magnetosphere (so get additional effects)

Good, Bad, Ugly Some events show nice unrolling

Good, Bad, Ugly Some events show nice unrolling Some events show lifting

Good, Bad, Ugly Some events show nice unrolling Some events show lifting Some events EPAM and GOES don’t match

Other Complications Kasper shock parameters Local acceleration vs trapped population along for the ride Richardson and anisotropies may be the answer