A Determination of the Value and Variability of the Sun's Open Magnetic Flux using a Global MHD Model

Details A Determination of the Value and Variability of the Sun's Open Magnetic Flux using a Global MHD Model A Determination of the Value and Variability of the Sun's Open Magnetic Flux using a Global MHD Model

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh44a..03r&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SH44A-03

Physics

2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma, 7509 Corona, 7524 Magnetic Fields, 7536 Solar Activity Cycle (2162)

Scientific paper

The underlying value and variation of the Sun's open, unsigned magnetic flux is of fundamental scientific importance, yet its properties remain poorly known. For example, do long term (on the time-scale of ~ 100 years) changes in the strength of the solar magnetic field exist and do they persist through the heliosphere? If present, they may have a direct impact on space climate, including implications for the transport of cosmic rays (CRs), and as such, may affect technology, space, and even terrestrial climate. Global MHD models are capable of reproducing the structure of the large-scale solar and interplanetary magnetic field (at least in the absence of transient phenomena such as Coronal Mass Ejections), and should, in principle, be able to address this topic. However, they rely - and depend crucially - on boundary conditions derived from observations of the photospheric magnetic field. In spite of ~ 40 years of measurements, accurate estimates of the radial component of the photospheric magnetic field remain difficult to make. In this study, we attempt to find a "ground truth" estimate of the photospheric magnetic field by carefully comparing both disk magnetograms and diachronic (previously known as synoptic) maps from 6 different observatories (KPVT, SOLIS, GONG, MDI, WSO, and MWO). We find that although there is a general consensus between several of them, there are also some significant discrepancies. Using data from these observatories, we compute global heliospheric solutions for a selection of epochs during the last 3 solar cycles and compare the results with in situ observations. We apply these results to several topics related to the Sun's open flux.

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