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

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

Solar event associations, Flare/CME properties

Solar event associations, Flare/CME properties

Proton, Helium & Oxygen fluences for an SEP event

Proton, Helium & Oxygen fluences for an SEP event

Longitudinal Distribution of large gradual SEPs

Longitudinal Distribution of large gradual SEPs

Cane et al (1986)

Multi-spacecraft observationsMulti-spacecraft observations

Kallenrode et al. 1993 (Solar Physics).

STEREO will characterize the azimuthal distribution of SEP

Properties

STEREO will characterize the azimuthal distribution of SEP

Properties

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

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

• 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)

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.

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)

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).

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