On the Contribution of Coronal Mass Ejections to the Heliospheric Magnetic Flux Budget on Different Time Scales

Coronal mass ejections (CMEs) contribute closed magnetic flux to the heliosphere while they are connected at both ends to the Sun and play a key role in adding magnetic flux to the heliosphere. Here, we discuss how the type of magnetic reconnection that opens CME field lines in the inner heliosphere, i.e., interchange (IC) and/or interplanetary (IP) reconnection, determines the length of time CMEs contribute to the heliospheric flux budget. This distinction has not been taken into account in past studies that estimate the CME flux opening timescale. We outline key criteria to aid in distinguishing IC reconnection from IP reconnection based on in situ spacecraft data and highlight these through two example events. Studying the manner in which CMEs reconnect and open in the inner heliosphere yields important insights not only into CMEs' role in the heliospheric flux budget but also the evolution of CME complexity, connectivity, and topology.

Automated summary

This study discusses how the type of magnetic reconnection in the inner heliosphere affects the contribution time of CMEs to the heliospheric flux budget, and proposes criteria to distinguish between different types of reconnection. The validity of these criteria is verified through example events. Studying the reconnection and opening of CMEs in the inner heliosphere provides important insights into their role in the heliospheric flux budget and the evolution of their complexity, connectivity, and topology.