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Coronal Mass Ejections travel time

Published online by Cambridge University Press:  12 September 2017

Carlos Roberto Braga ,
Rafael Rodrigues Souza de Mendonça Open the ORCID record for Rafael Rodrigues Souza de Mendonça [Opens in a new window] ,
Alisson Dal Lago  and
Ezequiel Echer
Carlos Roberto Braga
Affiliation:
National Institute for Space Research, Av. Dos Astronautas 1758, Jd. Granja, São José dos Campos, SP, Brazil email: carlos.braga@inpe.br
Rafael Rodrigues Souza de Mendonça
Affiliation:
National Institute for Space Research, Av. Dos Astronautas 1758, Jd. Granja, São José dos Campos, SP, Brazil email: carlos.braga@inpe.br
Alisson Dal Lago
Affiliation:
National Institute for Space Research, Av. Dos Astronautas 1758, Jd. Granja, São José dos Campos, SP, Brazil email: carlos.braga@inpe.br
Ezequiel Echer
Affiliation:
National Institute for Space Research, Av. Dos Astronautas 1758, Jd. Granja, São José dos Campos, SP, Brazil email: carlos.braga@inpe.br
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Abstract

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Coronal mass ejections (CMEs) are the main source of intense geomagnetic storms when they are earthward directed. Studying their travel time is a key-point to understand when the disturbance will be observed at Earth. In this work, we study the CME that originated the interplanetary disturbance observed on 2013/10/02. According to the observations, the CME that caused the interplanetary disturbance was ejected on 2013/09/29. We obtained the CME speed and estimate of the time of arrival at the Lagrangian Point L1 using the concept of expansion speed. We found that observed and estimated times of arrival of the shock differ between 2 and 23 hours depending on method used to estimate the radial speed.

Keywords

coronal mass ejections (CMEs)halo CMEsinterplanetary disturbancesmagnetic clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S328: Living Around Active Stars , October 2016 , pp. 218 - 220
Copyright
Copyright © International Astronomical Union 2017 

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