TY - JOUR
T1 - CME Magnetic Structure and IMF Preconditioning Affecting SEP Transport
AU - Palmerio, Erika
AU - Kilpua, Emilia K.J.
AU - Witasse, Olivier
AU - Barnes, David
AU - Sánchez-Cano, Beatriz
AU - Weiss, Andreas J.
AU - Nieves-Chinchilla, Teresa
AU - Möstl, Christian
AU - Jian, Lan K.
AU - Mierla, Marilena
AU - Zhukov, Andrei N.
AU - Guo, Jingnan
AU - Rodriguez, Luciano
AU - Lowrance, Patrick J.
AU - Isavnin, Alexey
AU - Turc, Lucile
AU - Futaana, Yoshifumi
AU - Holmström, Mats
N1 - Funding Information:
E. Palmerio acknowledges the Doctoral Programme in Particle Physics and Universe Sciences (PAPU) at the University of Helsinki, the Emil Aaltonen Foundation, and the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by UCAR's Cooperative Programs for the Advancement of Earth System Science (CPAESS) under award no. NNX16AK22G. E. Kilpua acknowledges the SolMAG project (ERC-COG 724391) funded by the European Research Council (ERC) in the framework of the Horizon 2020 Research and Innovation Programme, Academy of Finland project SMASH (grant no. 310445), and the Finnish Centre of Excellence in Research of Sustainable Space (Academy of Finland grant no. 312390). B. S?nchez-Cano acknowledges support through UK-STFC grant ST/S000429/1. A. Weiss and C. M?stl thank the Austrian Science Fund (FWF): P31521-N27. M. Mierla, A. Zhukov, and L. Rodriguez thank the European Space Agency (ESA) and the Belgian Federal Science Policy Office (BELSPO) for their support in the framework of the PRODEX Programme. J. Guo thanks the Strategic Priority Program of the Chinese Academy of Sciences (grant no. XDB41000000 and XDA15017300), and the CNSA preresearch Project on Civil Aerospace Technologies (grant no. D020104). The work of L. Turc is supported by the Academy of Finland (grant no. 322544). We thank two anonymous reviewers, whose comments and suggestions have significantly improved this article. We acknowledge support from the European Union FP7-SPACE-2013-1 programme for the HELCATS project (grant no. 606692). The HI instruments on STEREO were developed by a consortium that comprised the Rutherford Appleton Laboratory (UK), the University of Birmingham (UK), Centre Spatial de Li?ge (CSL, Belgium) and the Naval Research Laboratory (NRL, USA). The STEREO/SECCHI project, of which HI is a part, is an international consortium led by NRL. We recognize the support of the UK Space Agency for funding STEREO/HI operations in the UK. The WSA model was developed by C. N. Arge (currently at NASA/GSFC), and the Enlil model was developed by D. Odstrcil (currently at GMU). We thank the model developers, M. L. Mays, R. Colaninno, and the CCMC staff. We acknowledge the NMDB, founded under the European Union's FP7 programme (contract no. 213007), for providing neutron monitor data. We thank the WDC for Geomagnetism, Kyoto, and the geomagnetic observatories for their cooperation to make the final Dst indices available. This work is based (in part) on archival data obtained with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by an award issued by JPL/Caltech. Finally, we thank the instrument teams of all the spacecraft involved in this study.
Funding Information:
E. Palmerio acknowledges the Doctoral Programme in Particle Physics and Universe Sciences (PAPU) at the University of Helsinki, the Emil Aaltonen Foundation, and the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by UCAR's Cooperative Programs for the Advancement of Earth System Science (CPAESS) under award no. NNX16AK22G. E. Kilpua acknowledges the SolMAG project (ERC‐COG 724391) funded by the European Research Council (ERC) in the framework of the Horizon 2020 Research and Innovation Programme, Academy of Finland project SMASH (grant no. 310445), and the Finnish Centre of Excellence in Research of Sustainable Space (Academy of Finland grant no. 312390). B. Sánchez‐Cano acknowledges support through UK‐STFC grant ST/S000429/1. A. Weiss and C. Möstl thank the Austrian Science Fund (FWF): P31521‐N27. M. Mierla, A. Zhukov, and L. Rodriguez thank the European Space Agency (ESA) and the Belgian Federal Science Policy Office (BELSPO) for their support in the framework of the PRODEX Programme. J. Guo thanks the Strategic Priority Program of the Chinese Academy of Sciences (grant no. XDB41000000 and XDA15017300), and the CNSA preresearch Project on Civil Aerospace Technologies (grant no. D020104). The work of L. Turc is supported by the Academy of Finland (grant no. 322544). We thank two anonymous reviewers, whose comments and suggestions have significantly improved this article. We acknowledge support from the European Union FP7‐SPACE‐2013‐1 programme for the HELCATS project (grant no. 606692). The HI instruments on STEREO were developed by a consortium that comprised the Rutherford Appleton Laboratory (UK), the University of Birmingham (UK), Centre Spatial de Liège (CSL, Belgium) and the Naval Research Laboratory (NRL, USA). The STEREO/SECCHI project, of which HI is a part, is an international consortium led by NRL. We recognize the support of the UK Space Agency for funding STEREO/HI operations in the UK. The WSA model was developed by C. N. Arge (currently at NASA/GSFC), and the Enlil model was developed by D. Odstrcil (currently at GMU). We thank the model developers, M. L. Mays, R. Colaninno, and the CCMC staff. We acknowledge the NMDB, founded under the European Union's FP7 programme (contract no. 213007), for providing neutron monitor data. We thank the WDC for Geomagnetism, Kyoto, and the geomagnetic observatories for their cooperation to make the final Dst indices available. This work is based (in part) on archival data obtained with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by an award issued by JPL/Caltech. Finally, we thank the instrument teams of all the spacecraft involved in this study.
Publisher Copyright:
© 2021. The Authors.
PY - 2021/4
Y1 - 2021/4
N2 - Coronal mass ejections (CMEs) and solar energetic particles (SEPs) are two phenomena that can cause severe space weather effects throughout the heliosphere. The evolution of CMEs, especially in terms of their magnetic structure, and the configuration of the interplanetary magnetic field (IMF) that influences the transport of SEPs are currently areas of active research. These two aspects are not necessarily independent of each other, especially during solar maximum when multiple eruptive events can occur close in time. Accordingly, we present the analysis of a CME that erupted on May 11, 2012 (SOL2012-05-11) and an SEP event following an eruption that took place on May 17, 2012 (SOL2012-05-17). After observing the May 11 CME using remote-sensing data from three viewpoints, we evaluate its propagation through interplanetary space using several models. Then, we analyze in-situ measurements from five predicted impact locations (Venus, Earth, the Spitzer Space Telescope, the Mars Science Laboratory en route to Mars, and Mars) in order to search for CME signatures. We find that all in-situ locations detect signatures of an SEP event, which we trace back to the May 17 eruption. These findings suggest that the May 11 CME provided a direct magnetic connectivity for the efficient transport of SEPs. We discuss the space weather implications of CME evolution, regarding in particular its magnetic structure, and CME-driven IMF preconditioning that facilitates SEP transport. Finally, this work remarks the importance of using data from multiple spacecraft, even those that do not include space weather research as their primary objective.
AB - Coronal mass ejections (CMEs) and solar energetic particles (SEPs) are two phenomena that can cause severe space weather effects throughout the heliosphere. The evolution of CMEs, especially in terms of their magnetic structure, and the configuration of the interplanetary magnetic field (IMF) that influences the transport of SEPs are currently areas of active research. These two aspects are not necessarily independent of each other, especially during solar maximum when multiple eruptive events can occur close in time. Accordingly, we present the analysis of a CME that erupted on May 11, 2012 (SOL2012-05-11) and an SEP event following an eruption that took place on May 17, 2012 (SOL2012-05-17). After observing the May 11 CME using remote-sensing data from three viewpoints, we evaluate its propagation through interplanetary space using several models. Then, we analyze in-situ measurements from five predicted impact locations (Venus, Earth, the Spitzer Space Telescope, the Mars Science Laboratory en route to Mars, and Mars) in order to search for CME signatures. We find that all in-situ locations detect signatures of an SEP event, which we trace back to the May 17 eruption. These findings suggest that the May 11 CME provided a direct magnetic connectivity for the efficient transport of SEPs. We discuss the space weather implications of CME evolution, regarding in particular its magnetic structure, and CME-driven IMF preconditioning that facilitates SEP transport. Finally, this work remarks the importance of using data from multiple spacecraft, even those that do not include space weather research as their primary objective.
KW - coronal mass ejections
KW - heliophysics
KW - interplanetary magnetic field
KW - solar energetic particles
KW - solar wind
KW - space weather
UR - https://www.scopus.com/pages/publications/85105004492
U2 - 10.1029/2020SW002654
DO - 10.1029/2020SW002654
M3 - Article
AN - SCOPUS:85105004492
SN - 1542-7390
VL - 19
JO - Space Weather
JF - Space Weather
IS - 4
M1 - e2020SW002654
ER -