A Study of the Global Heliospheric Magnetic Flux Using In-Situ Data and the SAIC MHD Model

Details A Study of the Global Heliospheric Magnetic Flux Using In-Situ Data and the SAIC MHD Model A Study of the Global Heliospheric Magnetic Flux Using In-Situ Data and the SAIC MHD Model

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh13b..08l&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH13B-08

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7511 Coronal Holes, 7524 Magnetic Fields, 7537 Solar And Stellar Variability (1650)

Scientific paper

There has been considerable controversy in recent years over the slow evolution of the Sun's open field, which extends out to become the heliospheric magnetic field. In the standard solar model (e.g., Wang and Sheeley [1993]) the open flux can increase or decrease in response to the emergence or cancellation of magnetic flux at the photosphere in relation to coronal holes. In the Fisk et al. [1999a, 1999b] model, on the other hand, the open flux is conserved and evolves primarily via interchange reconnection with closed fields. This model predicts no long-term variations in the amount of heliospheric flux. We compare and test these theories by measuring the behavior of the open magnetic flux in the global heliospheric magnetic field. Using multi-point measurements from the VHM instrument on the Ulysses spacecraft and from the MAG instrument on the ACE spacecraft, we analyze in-situ radial magnetic field data and compare the behavior to that predicted by the updated SAIC MHD model. During solar maximum, ICMEs significantly disturb the heliospheric magnetic field, making our comparisons difficult. We examine the radial component of the magnetic field in data from 1991 though the present in order to determine the variability of the open flux and hence the evolution of corona holes.

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