Figure 1. PAS 1s mode except for Sep 23 – 25 in STP 328, where PAS was on 2s mode (see operation table). High correction factor (lower data quality) for slow wind streams. High solar activities with several ICMEs detected. PSP was also in the vicinity of SO during this perihelion.

Figure 2. An ICME-like structure. PAS 1s data. Good data quality throughout apart from the slow wind. Velocity jump > 400 km/s. Hot and dense ion stream (sheath) behind the velocity jump. The jump contains two-step-like shocks. Interesting non-thermal proton and alpha interval.

Figure 3. A shock at the perihelion (_{0.3 AU). PAS 1s data. Good data quality throughout apart from the slow wind. A shock with \Delta 𝑉} 400 km/s with a very dense interval behind the shock (sheath?).

Figure 4. Interesting structure at the perihelion (0.3 AU). PAS 1s data. Good data quality throughout apart from the slow wind. Either a stream interface (transition from slow- to high-speed stream) or an ICME with cold materials containing clear alpha particles. Featured by spiky structures (time scale of hours).

Figure 5. Slow, dense, and hot solar wind featured by spiky features (~ timescale of hours) in energy, velocity, temperature. A transition to intermediate/high-speed stream after Sep 30th.

Figure 6. Slow/intermediate fast wind intervals. Clear small-scale (hours) spiky features. Very dense SW interval after Sep 24.

Figure 7. Slow, dense, and hot solar wind featured by spiky features (~ timescale of hours) in energy, velocity, temperature. A transition to intermediate/high-speed stream after Sep 30th.

Figure 8. ICME with max H+ speed~ 700 km/s. Clear presence of non-thermal H+/He2+ populations (complex distribution functions).

Figure 9. Clear shock and sheath on Sep 4 followed by cold, tenuous H+ and He2+ streams on Sep 5. Another ICME with two-step shocks on Sep 6 followed by alternating cold and hot intervals. Data contamination by photoelectrons on September 4 - 6 visible as uniform energy flux across all energies in green.

Figure 10. Shock-ICME sampled with PAS 1s cadence.

Figure 11. Detected with PAS 1s data. Shock with V jump of 400 km/s. Clear sheath behind the shock. Proton speed in ICME ~ 1000 km/s. Secondary electron contamination on 23rd and 27th July.

Figure 12. Fast and hot stream (correlated velocity and temperature).

Figure 13. ICME detected at 0.94 AU with clear alpha particles and some additional ion species. Cold materials.

Figure 14. Two-step shocks on 13 - 14 June 2024.

Figure 15. An ICME preceded by a shock. Velocity jump > 200 km/s. Photoelectron contamination visible as uniform energy flux at all energies.

Figure 16. An ICME preceded by a shock. Velocity jump ~ 200 km/s. Plausibly clear flux rope structure. Clear alpha energy flux throughout.

Figure 17. An ICME at 0.45 AU with a shock and plausibly a flux rope with cold prominence materials. An additional species above He2+ omnidirectional energy flux.

Figure 18. Slow (V~ 350 km/s) and dense (200 /cc) wind with multiple populations and additional species.

Figure 19. Fast-/intermediate-speed wind on April 8th – 12th at 0.35 AU with a presence of jets throughout.

Figure 20. Dense wind interval preceding a high-speed stream. Presence of jets and sub-populations.

Figure 21. March – April 2024 Perihelion data (0.29 AU).

Figure 22. Slow and high-speed streams with broad energy flux. Presence of strong non-thermal H+ population.

Figure 23. Overview.

Figure 24. Zoom-in.

Figure 25. Note: the new PAS high cadence tests (1s or 2s) were running from Nov 2023 – 10 March 2024. There are several intervals with partial VDFs. PAS is on 2s cadence from March 11, 2024.

Figure 26. PAS was in 1s cadence, some partial VDF with 5 elevations. Nice wave activities upstream of the shocks seen by MAG.

Figure 27. IP shock or shock/ICME in moderate speed wind, calm upstream conditions.

Figure 28. Shock/ICME in slow wind with high alpha density in the trailing edge.

Figure 29. Dense ICME. Only partial VDF at the beginning of the interval.

Figure 30. Hot, slow streams at 0.3 AU. Some visible reflected ions upstream of the shock.

Figure 31. Mostly slow-intermediate speed wind with a few ICMEs. PAS static mode (window changes every 6h, 4s cadence). Distance 0.29 AU.

Figure 32. Possibly two ICMEs. 1st shock with \Delta V = 500 km/s, 2nd shock with \Delta V = 300 km/s. The ion energy flux of the 1st shock overshoots the PAS field of view. Alternate intervals of hot and cold materials.

Figure 33. A high density interval with clear He2+ (and possibly another ionized species above He2+?).

Figure 34. Alternating hot/cold intervals with clear He2+. There is possibly an IP shock on 20th of August at 4:00.

Figure 35. An IP shock, with some possible partial IP crossings.

Figure 36. An interval with the ion density enhancement.

Figure 37. An interplanetary (IP) shock in the slow wind.

Figure 38. An ICME on the 26th of July with maximum proton speed of 1130 km/s. There are two intervals of fast and dense protons. A cold trailing interval after the 2nd speed bump. There are some contaminations possibly due to photoelectrons across all the energies before the shock.

Figure 39. ICME with maximum proton speed of 800 km/s and intervals of cold H+ and He2+ (and some hot H+). A few hours interval with a very low density (0.02 cm-3).

Figure 40. ICME with maximum proton speed of 600 km/s and cold trailing interval (with a second proton peak, possibly a very fast beam, above the first peak).

Figure 41. A hot ion stream with intermediate/high speed wind, preceded by an intermediate/slow wind interval with clear He2+.

Figure 42. Slow, hot solar wind with some clear (dense) He2+.

Figure 43. Stream interaction region with clear H+ and He2+ in the trailing part (slow wind).

Figure 44. Cold stream of H+ and He2+ preceding hot stream (with a stream interface – like structure), followed by an ICME-like structure in intermediate – fast wind.

Figure 45. ICMEs in intermediate/slow wind with hot sheath and cold plasmas (0.5 AU).

Figure 46. A stream interface observed at 0.29 AU during the perihelion. The fast stream has a very high number density, reaching 1500 /cc. There is an intense He2+ energy flux with a clear separation from the cold protons in the fast stream.

Figure 47. An ICME with shock on the 20th and a cold/dense plasma with clear proton-alpha separation in the trailing part. This event was observed to have a strong Bz and it arrives at Earth.

Figure 48. A shock arrival.

Figure 49. A shock and/or stream interface with preceded cold plasma.

Figure 50. An interplanetary shock.

Figure 51. A potential Coronal Mass Ejection with a broaden shock region and a flux-rope structure at the trailing edge.

Figure 52. A drop of ion omnidirectional energy flux on the 24th December 2022, characterised by a 12-hr interval of a very low ion Eflux with n ~ 0.01 - 0.1 cm-3. Likely high uncertainties for moment calculations, seen as strong fluctuations of temperature and ion number density. SolO was located before Earth/MMS. Stereo-A was between SolO and Earth.

Figure 53. Slow and dense solar wind at 0.33 AU and high-speed streams plausibly containing switchback patches at 0.3 AU.

Figure 54. A shock/ICME arrival on the 6th of September 2022. High-speed protons up to 1100 km/s and high-temperature protons up to a few hundred eV in the shock. Cold protons in the magnetic cloud.

Figure 55. A stream interaction region / high-speed stream or an ICME arrival on the 3rd of September, 2022.

Figure 56. An ICME detected on the 1st of September 2022. Proton speed up to 1200 km/s in the shock. Cold plasma in the magnetic cloud. Data gap at the beginning STP 220, starting from 12:35 due to WOL and TCM.

Figure 57. Interplanetary shock. Warning - data quality factor exceeding the lower threshold before IP shock.

Figure 58. Shock/ICME arrival on 25/07/2022 with the proton bulk reaching ~1000 km/s.