sep data analysis and data products for emmrem mihir i. desai & arik posner southwest research...
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SEP Data Analysis and Data Products for EMMREM
SEP Data Analysis and Data Products for EMMREM
Mihir I. Desai & Arik Posner
Southwest Research Institute San Antonio, Texas
Mihir I. Desai & Arik Posner
Southwest Research Institute San Antonio, Texas
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Time-intensity profiles of 0.1 - 500 MeV protons during the 2003 October-November storms
Time-intensity profiles of 0.1 - 500 MeV protons during the 2003 October-November storms
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Solar event associations, Flare/CME properties
Solar event associations, Flare/CME properties
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Proton, Helium & Oxygen fluences for an SEP event
Proton, Helium & Oxygen fluences for an SEP event
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Longitudinal Distribution of large gradual SEPs
Longitudinal Distribution of large gradual SEPs
Cane et al (1986)
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Multi-spacecraft observationsMulti-spacecraft observations
Kallenrode et al. 1993 (Solar Physics).
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STEREO will characterize the azimuthal distribution of SEP
Properties
STEREO will characterize the azimuthal distribution of SEP
Properties
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Instruments & Energy coverageInstruments & Energy coverage
Table 1: Instruments and Energy Coverage Energy Range
(MeV or MeV/nucleon)
S/C Instr. Ions (H/He – Fe)
Electrons
ACE ULEIS 0.04 – 9.7 … ACE SIS 7.0 –90 …
SAMPEX PET 19 – 400 1.2 – 8.0 GOES EPS 0.8– 500 0.6 - >2 Wind STICS 0.006 – 0.2 … Wind STEP 0.02 – 2 … SoHO COSTEP 4 – 150 0.2 – 15
STEREO SEPT 0.02 – 7.0 0.02 – 0.4 STEREO SIT 0.03 – 2.0 … STEREO LET 1.5 – 30 … STEREO HET – 100 – 5.0 Ulysses KET 4 to >2000 2 to >10
LRO CRaTER LET (~1 to >100)
MSL RAD ~2-200 0.15-15 Odyssey MARIE LET
(1-30 keV/ m)
Add other datasets: e.g, SoHO/ERNE;Messenger
Add other datasets: e.g, SoHO/ERNE;Messenger
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SEP Analysis & Products for EMMREM
SEP Analysis & Products for EMMREM
• Event lists, and products for inputs into module━ Time-histories━ Energy Spectra━ Peak Intensities ━ Format (?)
• Radial and Longitudinal Distributions━ Moon orbit━ Mars━ Radial Alignment━ Longitudinal extrapolation (how without SEP
propagation)
• Validation using MSL/RAD; LRO/CRaTER
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• Kahler et al. (late 1970s and early 1980s) found strong correlation with CMEs
• Cane et al. (1986) made association with 2 types of radio bursts
Solar Energetic Particles (SEPs)
Solar Energetic Particles (SEPs)
only flares
Old picture - up to 1990s’
Current picture - two classes
• First discovered - Forbush 1946 from ground based ion counters
• Closely related to H flares - (Meyer 1956)
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Where?At CME-shocks or in flares
Source material?Ambient corona, solar wind, or other
Mechanisms?Reconnection or CME-shock acceleration
Transport to Earth?Scattering, Turbulence, fluctuations
SEPs: Big QuestionsSEPs: Big Questions
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
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Two-Class Picture - 70’s-90’sTwo-Class Picture - 70’s-90’s
Reames (1995)
Wild et al. (1963)
Lin (1970)
Pallavacini et al (1974)
Kahler et al. (1978)
Mason et al. (1984; 1986)
Cane et al. (1986; 1988; 1991)
Reames 1988; 1995; 1999)
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Encounter Encounter suprathermal suprathermal material in the material in the corona and the corona and the IP mediumIP medium
486CME shocksCME shocks
(Mason et al. 1999 ApJ, 525, L133).
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Emerging Picture - since-90’sEmerging Picture - since-90’sTwo-stage acceleration process
STEP 1: Production of a suprathermal seed populations
STEP 2: Acceleration at CME-driven shocks
Image Credit: ILWS Sentinels Science Definition Team Report