Influence of large-scale interplanetary structures on the propagation of solar energetic particles: The multi-spacecraft event on 2021 October 9
| Autor: | D. Lario, N. Wijsen, R. Y. Kwon, B. Sánchez-Cano, I. G. Richardson, D. Pacheco, E. Palmerio, M. L. Stevens, A. Szabo, D. Heyner, N. Dresing, R. Gómez-Herrero, F. Carcaboso, A. Aran, A. Afanasiev, R. Vainio, E. Riihonen, S. Poedts, M. Brüden, Z. G. Xu, A. Kollhoff |
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| Přispěvatelé: | European Space Agency, National Aeronautics and Space Administration (US), European Commission, Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España) |
| Rok vydání: | 2022 |
| Předmět: | |
| Zdroj: | Dipòsit Digital de la UB Universidad de Barcelona |
| Popis: | An intense solar energetic particle (SEP) event was observed on 2021 October 9 by multiple spacecraft distributed near the ecliptic plane at heliocentric radial distances R ≲ 1 au and within a narrow range of heliolongitudes. A stream interaction region (SIR), sequentially observed by Parker Solar Probe (PSP) at R = 0.76 au and 48° east from Earth (ϕ = E48°), STEREO-A (at R = 0.96 au, ϕ = E39°), Solar Orbiter (SolO; at R = 0.68 au, ϕ = E15°), BepiColombo (at R = 0.33 au, ϕ = W02°), and near-Earth spacecraft, regulated the observed intensity-time profiles and the anisotropic character of the SEP event. PSP, STEREO-A, and SolO detected strong anisotropies at the onset of the SEP event, which resulted from the fact that PSP and STEREO-A were in the declining-speed region of the solar wind stream responsible for the SIR and from the passage of a steady magnetic field structure by SolO during the onset of the event. By contrast, the intensity-time profiles observed near Earth displayed a delayed onset at proton energies ≳13 MeV and an accumulation of ≲5 MeV protons between the SIR and the shock driven by the parent coronal mass ejection (CME). Even though BepiColombo, STEREO-A, and SolO were nominally connected to the same region of the Sun, the intensity-time profiles at BepiColombo resemble those observed near Earth, with the bulk of low-energy ions also confined between the SIR and the CME-driven shock. This event exemplifies the impact that intervening large-scale interplanetary structures, such as corotating SIRs, have in shaping the properties of SEP events. Solar Orbiter is a space mission of international collaboration between ESA and NASA, operated by ESA. The STEREO SECCHI data are produced by a consortium of RAL (UK), NRL (USA), LMSAL (USA), GSFC (USA), MPS (Germany), CSL (Belgium), IOTA (France), and IAS (France). SOHO is a mission of international cooperation between ESA and NASA. The SDO/AIA data are provided by the Joint Science Operations Center (JSOC) Science Data Processing (SDP). Parker Solar Probe was designed, built, and is now operated by the Johns Hopkins University Applied Physics Laboratory as part of NASA's LWS program (contract NNN06AA01C). We thank the German Federal Ministry for Economic Affairs and Energy and the German Space Agency (Deutsches Zentrum für Luft- und Raumfahrt, e.V., (DLR)) for their unwavering support of STEP, EPT, and HET under grants Nos. 50OT0901, 50OT1202, 50OT1702, and 50OT2002. N.W. acknowledges funding from the Research Foundation—Flanders (FWO–Vlaanderen, fellowship No. 1184319N). This project has received funding from the European Union's Horizon 2020 research and innovation programs under grant agreement No. 870405 (EUHFORIA 2.0). These results were also obtained in the framework of the ESA project "Heliospheric modeling techniques" (contract No. 4000133080/20/NL/CRS) and the projects C14/19/089 (C1 project Internal Funds KU Leuven), G.0D07.19N (FWO–Vlaanderen), SIDC Data Exploitation (ESA Prodex-12), and Belspo project B2/191/P1/SWiM. E.P. acknowledges support from NASA's PSP-GI (grant No. 80NSSC22K0349) and O2R (grant No. 80NSSC20K0285) programs. B.S.-C. acknowledges support through UK-STFC Ernest Rutherford Fellowship ST/V004115/1 and STFC grants ST/W00089X/1 and ST/V000209/1. R.G.H. acknowledges the financial support by the Spanish MICIU (project PID2019-104863RB-I00/AEI/10.13039/501100011033). R.V. and N.D. acknowledge funding from the European Union's Horizon 2020 research and innovation program under grant agreement No. 101004159 (SERPENTINE). N.D. also acknowledges support from the Turku Collegium for Science, Medicine and Technology of the University of Turku, Finland. A.A. acknowledges the support by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019-105510GB-C31 and through the "Centre of Excellence María de Maeztu 2020-2023" award to the ICCUB (CEX2019-000918-M). D.L. and I.G.R. acknowledge support from NASA Living With a Star (LWS) programs NNH17ZDA001N-LWS and NNH19ZDA001N-LWS, the Goddard Space Flight Center Internal Scientist Funding Model (competitive work package) program, and the Heliophysics Innovation Fund (HIF) program. I.G.R. also acknowledges support from the ACE mission. The data used in this paper can be downloaded from spdf.gsfc.nasa.gov, www.srl.caltech.edu/ACE/ASC/, soar.esac.esa.int/soar/, stereo.gsfc.nasa.gov, gong.nso.edu/data/magmap/, sdo.gsfc.nasa.gov/data/aiahmi/. See also 10.48322/7gr7-1791, 10.48322/97te-0132, 10.48322/wpk2-yq48, and 10.48322/c0zj-xf76. BepiColombo data used in Figures 11 and 12 can be downloaded from 10.25392/leicester.data.19447259.v1. |
| Databáze: | OpenAIRE |
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