Abstract
One of the grand challenges in heliophysics is the characterization of coronal mass ejection (CME) magnetic structure and evolution from eruption at the Sun through heliospheric propagation. At present, the main difficulties are related to the lack of direct measurements of the coronal magnetic fields and the lack of 3D in-situ measurements of the CME body in interplanetary space. Nevertheless, the evolution of a CME magnetic structure can be followed using a combination of multi-point remote-sensing observations and multi-spacecraft in-situ measurements as well as modeling. Accordingly, we present in this work the analysis of two CMEs that erupted from the Sun on April 28, 2012. We follow their eruption and early evolution using remote-sensing data, finding indications of CME–CME interaction, and then analyze their interplanetary counterpart(s) using in-situ measurements at Venus, Earth, and Saturn. We observe a seemingly single flux rope at all locations, but find possible signatures of interaction at Earth, where high-cadence plasma data are available. Reconstructions of the in-situ flux ropes provide almost identical results at Venus and Earth but show greater discrepancies at Saturn, suggesting that the CME was highly distorted and/or that further interaction with nearby solar wind structures took place before 10 AU. This work highlights the difficulties in connecting structures from the Sun to the outer heliosphere and demonstrates the importance of multi-spacecraft studies to achieve a deeper understanding of the magnetic configuration of CMEs.
Originalsprache | englisch |
---|---|
Aufsatznummer | e2021JA029770 |
Fachzeitschrift | Journal of Geophysical Research: Space Physics |
Jahrgang | 126 |
Ausgabenummer | 11 |
DOIs | |
Publikationsstatus | Veröffentlicht - Nov. 2021 |
ASJC Scopus subject areas
- Astronomie und Planetologie
- Geophysik
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in: Journal of Geophysical Research: Space Physics, Jahrgang 126, Nr. 11, e2021JA029770, 11.2021.
Publikation: Beitrag in einer Fachzeitschrift › Artikel › Begutachtung
}
TY - JOUR
T1 - Magnetic Structure and Propagation of Two Interacting CMEs From the Sun to Saturn
AU - Palmerio, Erika
AU - Nieves-Chinchilla, Teresa
AU - Kilpua, Emilia K.J.
AU - Barnes, David
AU - Zhukov, Andrei N.
AU - Jian, Lan K.
AU - Witasse, Olivier
AU - Provan, Gabrielle
AU - Tao, Chihiro
AU - Lamy, Laurent
AU - Bradley, Thomas J.
AU - Mays, M. Leila
AU - Möstl, Christian
AU - Roussos, Elias
AU - Futaana, Yoshifumi
AU - Masters, Adam
AU - Sánchez-Cano, Beatriz
N1 - Funding Information: E. Palmerio is supported by the NASA Living With a Star (LWS) 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 310445, and the Finnish Centre of Excellence in Research of Sustainable Space (Academy of Finland grant no. 312390). A. Zhukov 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 no. 4000117262. L. Jian acknowledges support from the NASA LWS and Heliophysics Supporting Research (HSR) programs. G. Provan and B. S?nchez-Cano acknowledge support through UK-STFC Grant ST/S000429/1. L. Lamy acknowledges support from CNES and CNRS/INSU programs of planetology and heliophysics. C. M?stl thanks the Austrian Science Fund (FWF): P31521-N27. A. Masters was supported by a Royal Society University Research Fellowship. 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 recognise 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, 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. Finally, we thank the instrument teams of all the spacecraft involved in this study. Funding Information: E. Palmerio is supported by the NASA Living With a Star (LWS) 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 310445, and the Finnish Centre of Excellence in Research of Sustainable Space (Academy of Finland grant no. 312390). A. Zhukov 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 no. 4000117262. L. Jian acknowledges support from the NASA LWS and Heliophysics Supporting Research (HSR) programs. G. Provan and B. Sánchez‐Cano acknowledge support through UK‐STFC Grant ST/S000429/1. L. Lamy acknowledges support from CNES and CNRS/INSU programs of planetology and heliophysics. C. Möstl thanks the Austrian Science Fund (FWF): P31521‐N27. A. Masters was supported by a Royal Society University Research Fellowship. 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 recognise 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, 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. Finally, we thank the instrument teams of all the spacecraft involved in this study. Publisher Copyright: © 2021. The Authors.
PY - 2021/11
Y1 - 2021/11
N2 - One of the grand challenges in heliophysics is the characterization of coronal mass ejection (CME) magnetic structure and evolution from eruption at the Sun through heliospheric propagation. At present, the main difficulties are related to the lack of direct measurements of the coronal magnetic fields and the lack of 3D in-situ measurements of the CME body in interplanetary space. Nevertheless, the evolution of a CME magnetic structure can be followed using a combination of multi-point remote-sensing observations and multi-spacecraft in-situ measurements as well as modeling. Accordingly, we present in this work the analysis of two CMEs that erupted from the Sun on April 28, 2012. We follow their eruption and early evolution using remote-sensing data, finding indications of CME–CME interaction, and then analyze their interplanetary counterpart(s) using in-situ measurements at Venus, Earth, and Saturn. We observe a seemingly single flux rope at all locations, but find possible signatures of interaction at Earth, where high-cadence plasma data are available. Reconstructions of the in-situ flux ropes provide almost identical results at Venus and Earth but show greater discrepancies at Saturn, suggesting that the CME was highly distorted and/or that further interaction with nearby solar wind structures took place before 10 AU. This work highlights the difficulties in connecting structures from the Sun to the outer heliosphere and demonstrates the importance of multi-spacecraft studies to achieve a deeper understanding of the magnetic configuration of CMEs.
AB - One of the grand challenges in heliophysics is the characterization of coronal mass ejection (CME) magnetic structure and evolution from eruption at the Sun through heliospheric propagation. At present, the main difficulties are related to the lack of direct measurements of the coronal magnetic fields and the lack of 3D in-situ measurements of the CME body in interplanetary space. Nevertheless, the evolution of a CME magnetic structure can be followed using a combination of multi-point remote-sensing observations and multi-spacecraft in-situ measurements as well as modeling. Accordingly, we present in this work the analysis of two CMEs that erupted from the Sun on April 28, 2012. We follow their eruption and early evolution using remote-sensing data, finding indications of CME–CME interaction, and then analyze their interplanetary counterpart(s) using in-situ measurements at Venus, Earth, and Saturn. We observe a seemingly single flux rope at all locations, but find possible signatures of interaction at Earth, where high-cadence plasma data are available. Reconstructions of the in-situ flux ropes provide almost identical results at Venus and Earth but show greater discrepancies at Saturn, suggesting that the CME was highly distorted and/or that further interaction with nearby solar wind structures took place before 10 AU. This work highlights the difficulties in connecting structures from the Sun to the outer heliosphere and demonstrates the importance of multi-spacecraft studies to achieve a deeper understanding of the magnetic configuration of CMEs.
KW - coronal mass ejections
KW - heliophysics
KW - heliosphere
KW - interplanetary magnetic field
KW - solar wind
UR - http://www.scopus.com/inward/record.url?scp=85118521407&partnerID=8YFLogxK
U2 - 10.1029/2021JA029770
DO - 10.1029/2021JA029770
M3 - Article
AN - SCOPUS:85118521407
SN - 2169-9380
VL - 126
JO - Journal of Geophysical Research: Space Physics
JF - Journal of Geophysical Research: Space Physics
IS - 11
M1 - e2021JA029770
ER -