Evidence of a complex structure within the 2013 August 19 coronal mass ejection. Radial and longitudinal evolution in the inner heliosphere
- 1Universidad de Alcalá, Space Research Group, Alcalá de Henares, Madrid, Spain (l.rodriguezgarcia@edu.uah.es, raul.gomezh@uah.es, fernando.carcaboso@edu.uah.es, fsrodriguez@uah.es)
- 2Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA (teresa.nieves-chinchil-1@nasa.gov, lan.jian@nasa.gov, m.leila.mays@nasa.gov)
- 3European Space Astronomy Center, European Space Agency, Villanueva de la Cañada, Madrid, Spain (yannis.zouganelis@esa.int)
- 4Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA (angelos.vourlidas@jhuapl.edu)
- 5George Mason University, Fairfax, VA, USA (lbalmace@gmu.edu)
- 6Hvar Observatory, Faculty of Geodesy, University of Zagreb, Croatia (mateja.dumbovic@geof.unizg.hr)
- 7The Catholic University of America, Washington, DC, USA
- 8Cooperative Institute for Research in Environmental Sciences, University of Colorado Boulder, Boulder, CO, USA (luizfernando.guedesdossantos@colorado.edu)
Context. Late on 2013 August 19, a coronal mass ejection (CME) erupted from an active region located near the far-side central meridian from Earth’s perspective. The event and its accompanying shock were remotely observed by the STEREO-A, STEREO-B and SOHO spacecraft. The interplanetary (IP) counterpart (ICME) was intercepted by MESSENGER near 0.3 au, and by both STEREO-A and STEREO-B, near 1 au, which were separated by 78 degrees in heliolongitude.
Aims. The main objective of this study is to follow the radial and longitudinal evolution of the ICME throughout the inner heliosphere, and to examine possible scenarios for the different magnetic flux-rope (MFR) configuration observed on the solar disk, and measured in-situ at the locations of MESSENGER and STEREO-A, separated by 15 degrees in heliolongitude, and at STEREO-B, which detected the ICME flank.
Methods. Solar disk observations are used to estimate the ‘MFR type’, namely, the magnetic helicity, axis orientation and axial magnetic field direction of the MFR. The graduated cylindrical shell model is used to reconstruct the CME in the corona. The analysis of in-situ data, specifically, plasma and magnetic field, is used to estimate the global IP shock geometry and to derive the MFR type at different in-situ locations, which is compared to the type estimated from solar disk observations. The elliptical cylindrical analytical model is used for the in-situ MFR reconstruction.
Results. Based on the CME geometry and on the spacecraft configuration, we find that the MFR structure detected at STEREO-B belongs to the same ICME detected at MESSENGER and STEREO-A. The opposite helicity deduced at STEREO-B, might be due to the spacecraft intercepting one of the legs of the structure far from the MFR axis, while STEREO-A and MESSENGER are crossing through the core of the MFR. The different MFR orientations measured at MESSENGER and STEREO-A arise probably because the two spacecraft measure a curved, highly distorted and rather complex MFR topology. The ICME may have suffered additional distortion in its evolution in the inner heliosphere, such as the west flank is traveling faster than the east flank when arriving near 1 au.
How to cite: Rodríguez-García, L., Nieves-Chinchilla, T., Gómez-Herrero, R., Zouganelis, I., Vourlidas, A., Balmaceda, L., Dumbovic, M., Jian, L., Mays, L., Carcaboso, F., Guedes-Dos Santos, L. F., and Rodríguez-Pacheco, J.: Evidence of a complex structure within the 2013 August 19 coronal mass ejection. Radial and longitudinal evolution in the inner heliosphere, EGU General Assembly 2022, Vienna, Austria, 23–27 May 2022, EGU22-1017, https://doi.org/10.5194/egusphere-egu22-1017, 2022.
