Reconnection between pairs of solar magnetic flux elements, one open and the other a closed loop, is theorised to be a crucial process for both maintaining the structure of the corona and producing the solar wind. This 'interchange reconnection' is expected to be particularly active at the open-closed boundaries of coronal holes (CHs). Previous analysis of solar wind data at 1AU indicated that peaks in the flux of suprathermal electrons at slow-fast stream interfaces may arise from magnetic connection to the CH boundary, rather than dynamic effects such as compression. Further, offsets between the peak and stream interface locations are suggested to be the result of interchange reconnection at the source. As a preliminary test of these suggestions, we analyse two solar wind streams observed during the first Parker Solar Probe (PSP) perihelion encounter, each associated with equatorial CH boundaries (one leading and one trailing with respect to rotation). Each stream features a peak in suprathermal electron flux, the locations and associated plasma properties of which are indicative of a solar origin, in agreement with previous suggestions from 1AU observations. Discrepancies between locations of the flux peaks and other features suggest these peaks may too be shifted by source region interchange reconnection. Our interpretation of each event is compatible with a global pattern of open flux transport, although random footpoint motions or other explanations remain feasible. These exploratory results highlight future opportunities for statistical studies regarding interchange reconnection and flux transport at CH boundaries with modern near-Sun missions.
On the role of solar wind expansion as a source of whistler waves: scattering of suprathermal electrons and heat flux regulation in the inner heliosphere
Sunward Streaming 3He-rich SEP Events Observed by Solar Orbiter and Parker Solar Probe during Perihelion Passage
Southwest Research Institute（西南研究所）；Center for Astrophysics—Harvard & Smithsonian（天体物理学中心——哈佛与史密森尼学会）；Space Radiation Laboratory, California Institute of Technology（加州理工学院空间辐射实验室）；Applied Physics Laboratory, Johns Hopkins University（约翰斯·霍普金斯大学应用物理实验室）；The University of Texas at San Antonio（得克萨斯大学圣安东尼奥分校）
The Wave-Regulated Precursor of a Near-Parallel Interplanetary Shock Observed by Parker Solar Probe
University of Turku（图尔库大学）；Space Sciences Laboratory, University of California, Berkeley（加州大学伯克利分校空间科学实验室）；National Taras Shevchenko University of Kyiv（基辅塔拉斯舍甫琴科国立大学）；Ben Gurion University of the Negev（内盖夫本古里安大学）；University of California, San Diego（加州大学圣地亚哥分校）；Eureka Scientific（尤里卡科学公司）；The Johns Hopkins University Applied Physics Laboratory（约翰斯·霍普金斯大学应用物理实验室）；Queen Mary University of London（伦敦大学玛丽女王学院）；KU Leuven（荷语鲁汶大学）
Correlation of the sunspot number and the waiting time distribution of solar flares, coronal mass ejections, and solar wind switchback events observed with the Parker Solar Probe
Kinetic-based macro-modeling of the solar wind at large heliocentric distances: Kappa electrons at the exobase
KU Leuven（荷语鲁汶大学）；European Space Agency (ESA), European Space Astronomy Centre (ESAC)（欧洲航天局（ESA）欧洲航天天文中心（ESAC））；Ruhr-University Bochum（波鸿鲁尔大学）；Royal Belgian Institute for Space Aeronomy (BIRA-IASB)（比利时皇家空间气动力学研究所（BIRA-IASB））；Université Catholique de Louvain（天主教鲁汶大学）；University of Maria Curie-Skłodowska（玛丽亚·居里-斯可罗多夫斯卡大学）
Energetic Particle Acceleration and Transport: Interplanetary Coronal Mass Ejections and Shocks
National Observatory of Athens, IAASARS（雅典国家天文台）；California Institute of Technology（加州理工学院）；University of Arizona（亚利桑那大学）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理科学系）；European Space Agency (ESA), European Space Astronomy Centre (ESAC)（欧洲空间局（ESA），欧洲空间天文中心（ESAC））；Universidad de Alcalá, Space Research Group (SRG-UAH)（阿尔卡拉大学，空间研究小组（SRG-UAH））；The Johns Hopkins University, Applied Physics Laboratory（约翰斯·霍普金斯大学，应用物理实验室）；Institut für Experimentelle und Angewandte Physik, Christian-Albrechts-Universität zu Kiel（基尔大学实验与应用物理研究所）；National Key Laboratory of Deep Space Exploration/School of Earth and Space Sciences, University of Technology and Science of China（中国科学技术大学深空探测全国重点实验室/地球与空间科学学院）；Institute of Physics, University of Graz（格拉茨大学物理研究所）；NASA, Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；Los Alamos National Laboratory（洛斯阿拉莫斯国家实验室）；University of New Hampshire（新罕布什尔大学）；Southwest Research Institute（西南研究院）；CAS Center for Excellence in Comparative Planetology, University of Science and Technology of China（中国科学院比较行星学卓越创新中心，中国科学技术大学）
本综述利用多航天器多点多仪器观测，结合Solar Orbiter与Parker Solar Probe的近太阳高能粒子测量，研究行星际日冕物质抛射和激波对高能粒子加速与传输的作用，以解决相关未决问题。
