Abstract
The small-scale interplanetary magnetic flux ropes (SIMFRs) are common magnetic structures in the interplanetary space, yet their origination is still an open question. In this article, we surveyed 63 SIMFRs found within 6-day window around the heliospheric current sheet (HCS) and investigated their axial direction, as well as the local normal direction of the HCS. Results showed that the majority (48/63) of the SIMFRs were quasi-parallel to the associated HCS (i.e., the axial direction of SIMFRs was quasi-perpendicular to the normal direction of the associated HCS). They also showed that the SIMFRs quasi-parallel to the associated HCS statistically had shorter duration than the cases quasi-perpendicular. The results indicate that most of these SIMFRs may be generated in the nearby HCSs.
Highlights
Magnetic flux ropes (MFRs) are a helical magnetic structure that is very common in solar corona, the interplanetary space, planetary ionosphere, and earth magnetosphere [1]
We surveyed the axial distribution of SIMFRs detected within 6-day window around HCS and found that most of the ropes (76.2%) was quasi-parallel to the HCS
All authors contributed to the interpretation of the results and helped draft the manuscript
Summary
Magnetic flux ropes (MFRs) are a helical magnetic structure that is very common in solar corona, the interplanetary space, planetary ionosphere, and earth magnetosphere [1]. As solar wind and structures embedded in it mainly move in the Sun–Earth line direction, assuming that the magnetic field points from the Sun to the Earth in the upper hemisphere and points from the Earth to the Sun on the bottom hemisphere, as illustrated, the spacecraft should detect negative to positive variation of the z component of the magnetic field. The SIMFRs studied in this article were detected by Wind from 1995 to 2013 in the vicinity of HCSs. The crossing of an HCS is identified by a flip in at least one component of the magnetic field, and the polarity of the magnetic field should be kept several hours or more before and after the flip. BThe duration of the SIMFR (MIN). cThe longitude and latitude of the axis of SIMFR and the normal direction of HCS with respect to the ecliptic plane. dThe time of HCS crossing (UT). eThe time between the beginning of the SIMFR and the HCS crossing. fThe angle between the axial direction of SIMFR and the normal direction of HCS
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