Selected animations show a hypothetic global context for PUNCH spacecraft on August 2022. Historic observations are used to calculate the radial magnetic field and solar wind velocity at 21.5 Rs by the GONGz-WSA_2.2 model and to fit geometric and kinematic parameters of coronal mass ejections (CMEs) at CCMC/DONKI. (Click on an image to launch the animation.)

• Boundary conditions at 21.5 Rs from 2011-07-19 to 2011-08-31 used to drive a heliospheric simulation from 2022-07-19 to 2022-08-31 (i.e., within the same period of the 11-year solar activity cycle).

• Space weather monitors: PUNCH (at near-Earth), Solar Orbiter (SOL), and STEREO-A (STA) and heliospheric disturbances at the ecliptic from 2022-08-01 to 2022-08-31. Left: solar wind density together with the heliospheric imagers' field of view. Right: solar wind radial velocity together with the interplanetary magnetic field lines.

• Detail view of heliospheric disturbances at the ecliptic from 2022-08-01 to 2022-08-31. Solar wind density together with the interplanetary magnetic field line passing through geospace.

• Synthetic white-light images at PUNCH (right) and solar wind density at ecliptic (left) from 2022-08-01 to 2022-08-31. Running differencing has 2-hour cadence. Dashed-green lines show an extent of the combined FOV (elongations: 2.5-47.5 degs) and the solid green lines show elongations at 20, 40, and 60 degs.

• Alternative animations with synthetic white-light images at PUNCH and solar wind density at ecliptic:
  • Running difference - 1-hour cadence
  • Running difference - 4-hour cadence
  • Ambient difference
  • Absolute values

• Acronyms for the displayed spacecraft positions:
BEP=BepiColombo, KEP=Kepler, INS=InSight, HAY=Hayabusha-2, PSP=Parker Solar Probe, SOLO=Solar Orbiter, SPI=Spitzer, STA=STEREO-A.

Acknowledgments: This work has been supported by NASA/LWS-SC Program.