The Astrophysical Journal (Jan 2024)

Properties of an Interplanetary Shock Observed at 0.07 and 0.7 au by Parker Solar Probe and Solar Orbiter

  • Domenico Trotta,
  • Andrea Larosa,
  • Georgios Nicolaou,
  • Timothy S. Horbury,
  • Lorenzo Matteini,
  • Heli Hietala,
  • Xochitl Blanco-Cano,
  • Luca Franci,
  • C. H. K Chen,
  • Lingling Zhao,
  • Gary P. Zank,
  • Christina M. S. Cohen,
  • Stuart D. Bale,
  • Ronan Laker,
  • Nais Fargette,
  • Francesco Valentini,
  • Yuri Khotyaintsev,
  • Rungployphan Kieokaew,
  • Nour Raouafi,
  • Emma Davies,
  • Rami Vainio,
  • Nina Dresing,
  • Emilia Kilpua,
  • Tomas Karlsson,
  • Christopher J. Owen,
  • Robert F. Wimmer-Schweingruber

DOI
https://doi.org/10.3847/1538-4357/ad187d
Journal volume & issue
Vol. 962, no. 2
p. 147

Abstract

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The Parker Solar Probe (PSP) and Solar Orbiter (SolO) missions opened a new observational window in the inner heliosphere, which is finally accessible to direct measurements. On 2022 September 5, a coronal mass ejection (CME)-driven interplanetary (IP) shock was observed as close as 0.07 au by PSP. The CME then reached SolO, which was radially well-aligned at 0.7 au, thus providing us with the opportunity to study the shock properties at different heliocentric distances. We characterize the shock, investigate its typical parameters, and compare its small-scale features at both locations. Using the PSP observations, we investigate how magnetic switchbacks and ion cyclotron waves are processed upon shock crossing. We find that switchbacks preserve their V–B correlation while compressed upon the shock passage, and that the signature of ion cyclotron waves disappears downstream of the shock. By contrast, the SolO observations reveal a very structured shock transition, with a population of shock-accelerated protons of up to about 2 MeV, showing irregularities in the shock downstream, which we correlate with solar wind structures propagating across the shock. At SolO, we also report the presence of low-energy (∼100 eV) electrons scattering due to upstream shocklets. This study elucidates how the local features of IP shocks and their environments can be very different as they propagate through the heliosphere.

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