SITB 40 160 ke V SITB 80 160

SIT-B 40 -160 ke. V

SIT-B 80 -160 ke. V • these additional counts during the bursts events are considerably reduced above 80 ke. V! • notice that in CIR histograms species like C, N, O and Ne. S are not resolved in this energy range (or linear scale effect? ) 2

t al. , JGR, 2014; but G. M. Mason reports in the Aug 13, 2014 e-mail a below 80 ke. V/n for Ne. S and Fe boxes. 3

st almost disappears above 80 ke. V ! 4

• gray – counts from both bursts periods; red – Dec 9 2007 CIR • count excess in 6 -12 & 12 -20 amu in slide 1 is due to counts in 40 -80 ke. V/n range; in CIRs there are many counts in range 60 -160 ke. V/n which masks this excess in histograms on slide 1 • the shape of the 1 st excess (6 -12 amu) is due to energy threshold and contains likely 4 He ions • the 2 nd excess (12 -20 amu) should be due 16 O • there is also small 3 rd peak due to Ne. S ions • since these bursts are low-energy phenomena we luckily see O and Ne. S peaks! Therefore the claiming in Opitz paper that enhancements in bursts are seen in C-O range was correct. • for 40 -80 ke. V/n the CIR and bursts histograms are quite similar - implying common seed population (solar wind)? • at higher energies (see last histogram which is almost above threshold energy for hydrogen ) the H/He ratio in bursts is much different than in the CIR – implying different acceleration processes ? 5

• previous CIR histograms in log scale 12 C 16 O 20 Ne-32 S no ‘so’ obvious peaks? 6

BACKGROUND • ~20 min periodic bckg. feature, where: • 80 -160 ke. V/n 4 He counts shifted to higher amu (to C-O range) & • at higher energies (see 320 -640 ke. V/n) when H counts start to appear, their counts also shifted to higher amu (like 3 He) • such bckg. is not visible above 20 amu and for 40 -80 ke. V/n – but not sure because counts are low (next slide checks this for a stronger event) 7

• now there are two periods in the background • also this stronger event shows that Ne. S, Fe & 40 -80 ke. V/n are not much affected by this bckg. 8

SIT-B bursts on top of CIR event 40 -57 57 -80 80 -113 113 -160 etc. 160 -226 226 -320 320 -453 453 -640 640 -905 • why these bursts coincide with the periodic bckg. increases? But they are not bckg. , otherwise they appear always and it’s not the case! Would we see these bursts if SIT-B is working without these periodic failures? 9

… back to the G. Mason ‘s report on contamination < 80 ke. V/n • in this event, counts in gray area (40 -57 ke. V) behave differently than rest energy ranges (especially at ~20 -40 amu) • Fe peak is not well separated at 40 -57 but at 57 -80 ke. V/n is separated well 10

sunward pointing s anti-sunward poin • the bursts pattern on STA until ~300 Re (20 Jan) is similar to ST STEREO-B pattern similar to STB STEREO-A 101 -110 ke. V SEPT ions

#2 #3 sunward pointing anti-sunward poin #4 • STB shows more isotropic pattern while STA shows strong an in anti-sunward direction; strong simultaneous spikes #1, 2, 3, 4 a direction on STA but from sunward (or are more isotropic) on ST the bow shock? STB almost at the bow-shock ? STA far (300 Re) from the bow shock #1