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CME deflections due to magnetic forces from the Sun and Kepler-63

Published online by Cambridge University Press:  24 September 2020

F. Menezes Open the ORCID record for F. Menezes [Opens in a new window] ,
Y. Netto ,
C. Kay ,
M. Opher  and
A. Valio
F. Menezes
Affiliation:
Universidade Presbiteriana Mackenzie, CRAAM, São Paulo, Brazil email: [email protected]
Y. Netto
Affiliation:
Universidade Presbiteriana Mackenzie, CRAAM, São Paulo, Brazil email: [email protected] Osservatorio Astrofisico Di Catania, Catania, Italy
C. Kay
Affiliation:
NASA, Goddard Space Flight Center, Greenbelt, USA
M. Opher
Affiliation:
Boston University, Department Of Astronomy, Boston, USA
A. Valio
Affiliation:
Universidade Presbiteriana Mackenzie, CRAAM, São Paulo, Brazil email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

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The stellar magnetic field is the driver of activity in the star and can trigger energetic flares, CMEs and ionized wind. These phenomena, specially CMEs, may have an important impact on the magnetosphere and atmosphere of the orbiting planets. To predict whether a CME will impact a planet, the effects of the background on the CME's trajectory must be taken into account. We used the MHD code ForeCAT – a model for CME deflection due to magnetic forces – to perform numerical simulations of CMEs being launched from both the Sun and Kepler-63, which is a young, solar-like star with high activity. Comparing results from Kepler-63 and the Sun gives us a panorama of the distinct activity level and star-planet interactions of these systems due to the difference of stellar ages and star-planet distances.

Keywords

Sun: coronal mass ejections (CMEs)stars: activitystars: magnetic fieldsstars: spots, MHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S354: Solar and Stellar Magnetic Fields: Origins and Manifestations , June 2019 , pp. 421 - 425
Copyright
© International Astronomical Union 2020

References

Estrela, R. & Valio, A. 2018, Astrobiology, 18, 1414CrossRefGoogle Scholar
Jakosky, B. M. 2015, Science, 350, 643CrossRefGoogle Scholar
Kay, C., Opher, M., & Evans, R. M. 2013, ApJ, 775, 5CrossRefGoogle Scholar
Kay, C., Opher, M., & Evans, R. M. 2015, ApJ, 805, 168CrossRefGoogle Scholar
Kay, C., Opher, M., & Kornbleuth, M. 2016, ApJ, 826, 195CrossRefGoogle Scholar
Netto, Y. & Valio, A. 2019, A&A (accepted)Google Scholar
Sanchis-Ojeda, R., Winn, J. N., Marcy, G. W., et al. 2013, ApJ, 775, 54CrossRefGoogle Scholar
Silva, A. V. R. 2003, ApJ, 585, L147CrossRefGoogle Scholar
Valio, A., Spagiari, E., Marengoni, M., & Selhorst, C. 2019, Manuscript in preparationGoogle Scholar