The Flux of Open and Torroidal Interplanetary Magnetic Field as a Function of Heliolatitude and Solar Cycle

Details The Flux of Open and Torroidal Interplanetary Magnetic Field as a Function of Heliolatitude and Solar Cycle The Flux of Open and Torroidal Interplanetary Magnetic Field as a Function of Heliolatitude and Solar Cycle

Publishing date

Dec 2008

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh44a..07c&link_type=abstract

Journals

American Geophysical Union, Fall Meeting 2008, abstract #SH44A-07

Science

Physics

Additional info 3

2101 Coronal Mass Ejections (7513), 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 7524 Magnetic Fields

Type

Scientific paper

Abstract

Analyses performed during the previous 11-year phase of the solar cycle attempted to measure the flux of open and toroidal magnetic field lines [Bieber and Rust, ApJ, 453, 911, 1995] and associate the toroidal flux with coronal mass ejections (CMEs) [Smith and Phillips, JGR, 102, 249, 1997]. Since that time Ulysses has made three polar passes and spent at least eight years at polar latitudes, enabling us to examine the underlying assumption of the earlier studies that using near-ecliptic latitude measurements could serve as a proxy for polar-latitude observations. We find confirmation of the claims that the present solar minimum has experienced a strong decrease in open flux, but we also find evidence of past conditions at this same level. We find that torroidal flux is virtually negligable at higher latitudes as measured by the Ulysses spacecraft, even during times of solar maximum, and attribute this to the sub-photospheric winding of the Sun's magnetic field as illustrated by the familiar butterfly diagram. Our observations of the rate of toroidal flux ejection, 7 × 1022 Mx/year, sets a lower limit on the amount of magnetic flux that can be ejected by CMEs near solar maximum.

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