1,2,3,4,3,5,6,7,9,10,8,- 1San Antonio, United States of America (mdesai@swri.edu)
- 2Department of Physics and Astronomy, University of Texas at San Antonio, San Antonio, TX 78249, USA
- 3Department of Physics, the Institute for Physical Science and Technology and the Joint Space Institute, University of Maryland, College Park, MD, USA
- 4Institute for Research in Electronics and Applied Physics, University of Maryland, College Park, MD, USA
- 5Department of Astrophysical Sciences, Princeton University, NJ 08544, USA
- 6Space Sciences Laboratory, University of California, Berkeley, CA
- 7Physics Department, University of California, Berkeley,
- 8Johns Hopkins University/Applied Physics Laboratory, Laurel, MD 20723, USA
- 9California Institute of Technology, Pasadena, CA 91125, USA
- 10NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
- 11University of New Hampshire, 8 College Road, Durham NH 03824, USA
- 12University of Delaware, Newark, DE 19716, USA
Magnetic reconnection at the near-Sun heliospheric current sheet (HCS) dissipates the Parker spiral and converts magnetic energy into kinetic energy of the plasma constituents. Observations at a radial distance of ~16.25 Rs by Parker Solar Probe associated with the encounter 14 (E14) HCS crossing have shown that reconnection-driven particle acceleration mechanisms, likely facilitated by the merging of large-scale flux tubes, are able to accelerate protons up to ~400 keV, which is ≈1000 times greater than the available magnetic energy per particle during this crossing (Desai et al. 2025; Phan et al. 2024). In this paper, we present a detailed analysis of the pitch-angle distributions, differential energy spectra, and maximum energies and spectra of protons and heavy ions (He, O, and Fe) in conjunction with observations of local wave activity during the E14 HCS crossing. Our results show the following: 1) First direct observations of the energization of protons and heavy ions during reconnection. 2) First direct observations that the power-law spectral slopes of heavy ions differ from that of protons, which contradicts previous simulation results where the spectral indices of all ion species are essentially identical. 3) First demonstration that the anisotropies and beams of ions produced during reconnection drive waves in the ion cyclotron range of frequencies. 4) First evidence that the pitch angle scattering of protons is stronger than that of the other ion species and that this might be responsible for the harder spectral slopes of the heavy ions compared with protons. In summary, PSP observations during the E14 HCS crossing provide strong evidence for in-situ reconnection-driven acceleration of protons and heavy ions at the near-Sun HCS that will need to be fully accounted for by contemporary reconnection-driven energization models.
How to cite: Desai, M., Drake, J., Swisdak, M., Fitzmaurice, A., McComas, D., Bale, S., Phan, T., Berland, G., Mitchell, D., Cohen, C., Hill, M., Christian, E., Schwadron, N., McNutt, R., Matthaeus, W., Rahmati, A., Whittlesey, P., Livi, R., and Larson, D.: Proton and Heavy Ion Acceleration by Magnetic Reconnection at the near-Sun Heliospheric Current Sheet, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-3589, https://doi.org/10.5194/egusphere-egu26-3589, 2026.
