S.L.Y. would like to thank STFC via the consolidated grant (STFC ST/V000497/1), NERC via the SWIMMR Aviation Risk Modeling (SWARM) project grant (NE/V002899/1), and the Donostia International Physics Center for their hospitality. D.M.L. is grateful to the Science Technology and Facilities Council for the award of an Ernest Rutherford Fellowship (ST/R003246/1). D.B. is funded under STFC consolidated grant No. ST/S000240/1. The work of D.H.B. was performed under contract to the Naval Research Laboratory and was funded by the NASA Hinode program. L.M.G. would like to thank NERC via the SWIMMR Aviation Modeling Risk (SWARM) project (grant No. NE/V002899/1). V.P. acknowledges support from NASA contract NNG09FA40C (IRIS) and NASA grant No. 80NSSC21K0623. L.v.D.G. acknowledges the Hungarian National Research, Development and Innovation Office grant OTKA K-131508. S.P. acknowledges funding by CNES through the MEDOC data and operations center. W.T.T. was funded under NASA Grant NNG06EB68C. Solar Orbiter is a space mission of international collaboration between ESA and NASA, operated by ESA. We are grateful to the ESA SOC and MOC teams for their support. The SO/EUI instrument was built by CSL, IAS, MPS, MSSL/UCL, PMOD/WRC, ROB, and LCF/IO with funding from the Belgian Federal Science Policy Office (BELSPO/PRODEX PEA 4000134088); the Centre National d'Etudes Spatiales (CNES); the UK Space Agency (UKSA); the Bundesministerium fuer Wirtschaft und Energie (BMWi) through the Deutsches Zentrum fuer Luft-und Raumfahrt (DLR); and the Swiss Space Office (SSO). The ROB team thanks the Belgian Federal Science Policy Office (BELSPO) for the provision of financial support in the framework of the PRODEX Programme of the European Space Agency (ESA) under contract numbers 4000134088, 4000112292, 4000136424, and 4000134474. Solar Orbiter magnetometer operations are funded by the UK Space Agency (grant ST/T001062/1). T.H. is supported by STFC grant ST/X002098/1. The German contribution to SO/PHI is funded by the BMWi through DLR and by MPG central funds. The Spanish contribution is funded by FEDER/AEI/MCIU (RTI2018-096886-C5), a "Center of Excellence Severo Ochoa" award to IAA-CSIC (SEV-2017-0709), and a Ramon y Cajal fellowship awarded to DOS. The French contribution is funded by CNES. J.C.T.I. and D.O.S. are supported by the Spanish Ministry of Economy and Competitiveness through projects ESP-2016-77548-C5-1-R, and by the Spanish Science Ministry "Centro de Excelencia Severo Ochoa" Program under grant SEV-2017-0709 and project RTI2018-096886-B-C51. D.O.S. also acknowledges financial support from a Ramon y Cajal fellowship. The development of the SPICE instrument was funded by ESA and ESA member states (France, Germany, Norway, Switzerland, United Kingdom). The SPICE hardware consortium was led by Science and Technology Facilities Council (STFC) RAL Space and included Institut d'Astrophysique Spatiale (IAS), Max-Planck-Institut fuer Sonnensystemforschung (MPS), Physikalisch-Meteorologisches Observatorium Davos and World Radiation Center (PMOD/WRC), Institute of Theoretical Astrophysics (University of Oslo), NASA Goddard Space Flight Center (GSFC), and Southwest Research Institute (SwRI). The in-flight commissioning of SPICE was led by the instrument team at UKRI/STFC RAL Space. A.F.'s and A.G.'s research is funded by UKRI STFC. SO/SWA data are derived from scientific sensors that have been designed, created, and operated under funding provided via numerous contracts from the UK Space Agency (UKSA), the UK Science and Technology Facilities Council (STFC), the Agenzia Spaziale Italiana (ASI), the Centre National d'Etudes Spatiales (CNES, France), the Centre National de la Recherche Scientifique (CNRS, France), the Czech contribution to the ESA PRODEX program, and NASA. Solar Orbiter SWA work at UCL/MSSL was funded under STFC grants ST/T001356/1, ST/S000240/1, ST/X002152/1 and ST/W001004/1. SDO data are courtesy of NASA/SDO and the AIA, EVE, and HMI science teams. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research Center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA), University of Cambridge (UK), and NASA Goddard Space Flight Center (USA). This work also utilizes data produced collaboratively between AFRL/ADAPT and NSO/NISP. For the purpose of open access, the author has applied a Creative Commons Attribution (CC BY) license (where permitted by UKRI, "Open Government License" or "Creative Commons Attribution No-derivatives (CC BY ND) license" may be stated instead) to any Author Accepted Manuscript version arising. Facilities: SolO, SDO, Hinode, IRIS. Software: JHelioviewer (Mueller et al. 2017), SunPy v4.1.0 (The SunPy Community et al. 2020; Mumford et al. 2022), AstroPy (Astropy Collaboration et al. 2022), SolarSoft IDL PFSS package (Schrijver & De Rosa 2003).

The Slow Solar Wind Connection Solar Orbiter Observing Plan (Slow Wind SOOP) was developed to utilize the extensive suite of remote-sensing and in situ instruments on board the ESA/NASA Solar Orbiter mission to answer significant outstanding questions regarding the origin and formation of the slow solar wind. The Slow Wind SOOP was designed to link remote-sensing and in situ measurements of slow wind originating at open-closed magnetic field boundaries. The SOOP ran just prior to Solar Orbiter’s first close perihelion passage during two remote-sensing windows (RSW1 and RSW2) between 2022 March 3-6 and 2022 March 17-22, while Solar Orbiter was at respective heliocentric distances of 0.55-0.51 and 0.38-0.34 au from the Sun. Coordinated observation campaigns were also conducted by Hinode and IRIS. The magnetic connectivity tool was used, along with low-latency in situ data and full-disk remote-sensing observations, to guide the target pointing of Solar Orbiter. Solar Orbiter targeted an active region complex during RSW1, the boundary of a coronal hole, and the periphery of a decayed active region during RSW2. Postobservation analysis using the magnetic connectivity tool, along with in situ measurements from MAG and SWA/PAS, showed that slow solar wind originating from two out of three of the target regions arrived at the spacecraft with velocities between ∼210 and 600 km s−1. The Slow Wind SOOP, despite presenting many challenges, was very successful, providing a blueprint for planning future observation campaigns that rely on the magnetic connectivity of Solar Orbiter. © 2023. The Author(s). Published by the American Astronomical Society.

Yardley, Stephanie L., et al.

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