Abstract
Continuous accumulation of IPS (interplanetary scintillation) observations of the solar wind since 1972 enables us to follow solar-cycle variations of large-scale solar wind stream structures. The longitude/latitude structure of the solar wind speed is largely determined by the geometry of the heliospheric neutral sheet; the low-speed solar wind tends to be observed along the neutral sheet, whereas large, predominantly unipolar magnetic regions on the source surface (coronal holes) are the sources of high-speed streams. Large-scale configuration of a transient interplanetary disturbance has been shown to be distorted by the solar wind stream structures. In some cases, strong deceleration of the shock speed will take place along the heliospheric neutral sheet.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
