1. Relative Timing of Electron Acceleration and Proton Release in X-class Solar Events
Alexei Struminsky1,2
 1 Space Research Institute
2 Moscow Institute of Physics and Technology

2. INTRODUCTION
Interaction of accelerated electrons (microwaves; HXR; SXR derivative)
Interaction of accelerated protons (nuclear and pion gamma lines)
Electron release (radio type II; type III) – signature of open magnetic field lines;
Proton release time derived from proton onset at some point in the heliosphere, GLE onset – release of first protons;
Only a difference of 10 min between EM signature and proton release time is reliable (Klecker et al., 2010)
Is it possible to add something new to this picture?
Yes, if we will use new instruments with better statistical accuracy and compare different events with each other.

3. Plasma Temperature
SHH (the Kiplinger (1995) law) – something important happened during the late impulsive phase
Temperature time profiles of gradual events are different during preflare and impulsive phases, but have nearly the same slope after min
A zero time allowing to compare different events

4. Microwaves 15.4 GHz
Accelerated electrons during 0-20 min, in some cases before and later
Active impulsive phase (0-20 min) – accelerated electrons effectively heat the flare plasma
Influence of accelerated electrons on plasma heating is minor during the SXR decay phase (after 20 min)

5. HXR + protons (ACS SPI)
Anti Coincidence System of Spectrometer on Integral (ACS SPI) – gamma rays (>150 keV)
A response of ACS SPI to solar HXR is within statistical errors for 26/10/03 and 14/12/06;
ACS SPI – secondary gamma (solar protons) after 20 min with two exceptions (20/01/05–earlier, 19/01/05 – later).

6. PROTON ONSET (GOES)
Do not contradict to acceleration of first protons during the active impulsive phase
Nearly simultaneous release of first protons and prolonged injection with different intensities during the SXR decay phase

7. PROTON ONSET (02/11/2003)
ACS SPI above background at the proton onset in large HXR events

8. PROTON ONSET (17/01/2005) LASCO C2 Halo CME 17/01/05
09:30: km/s
09:54: km/s

9. PROTON ONSET (19/01/2005) Large fluctuations of the ACS SPI background
Proton event – ACE EPHIN
Why the SEP event of 2005 January 19 is so small?
G XRA 1-8A X E-01
G XFL N15W E E+05
//// SVI C RSP II/
//// SVI C RSP IV/2
19/01/05 LASCO C2 Halo CME 08:29: km/s
III – not reported, confinement of particles within loops?

10. PROTON ONSET (GLE events)
28/10/03 GLE onset at 12 min (11:12 UT, Biber et al., 2005), pion decay after 4 min (11:04 UT SONG, Kusnetsov et al., 2006), arrival of first protons is below the ACS SPI background, approximately at 12 min.
02/11/03, GLE onset at 20 min (17:29 UT), arrival of first protons is below the ACS SPI background, approximately at 12 min.
17/01/05 GLE onset >120 min, arrival of first protons is below the ACS SPI background, approximately at 12 min
20/01/05 GLE and ACS SPI onset 10 min (06:50 UT, Vashenyuk et al., 2006), pion decay after 6 min (06:46 UT SONG, Kuznetsov et al., 2006).
13/12/06 GLE onset 27 min (02:49 UT), arrival of first protons is below the ACS SPI background, approximately at 14 min.

11. CONCLUSIONS
The choice of zero time allows us to compare different events in the same time scale
Acceleration of relativistic solar protons occurs after 4-8 min since zero time and has a clear flare signature, the conditions for proton acceleration should be created
First relativistic protons arrive to the Earth with 4-6 min delay relatively to the flare signature (10-14 min after zero time)
A different rate of proton intensity increasing shows a role injection function, which depends on time and energy