Coronal and heliospheric magnetic flux circulation and its relation to open solar flux evolution

This work utilizes data from the National Solar Observatory Integrated Synoptic Program, which is operated by the Association of Universities for Research in Astronomy, under a cooperative agreement with the National Science Foundation and with additional financial support from the National Oceanic and Atmospheric Administration, the National Aeronautics and Space Administration, and the United States Air Force. The GONG network of instruments is hosted by the Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofísica de Canarias, and Cerro Tololo Interamerican Observatory. (http://gong2.nso.edu/). The authors are also grateful to staff and funders of National Space Science Data Center for the provision of the OMNI2 data set (http://omniweb.gsfc.nasa.gov/html/ow_data.html). We also thank David Hathaway and the staff of the Solar Physics Group at NASA's Marshall Space Flight Center for maintaining the online database of SOON sunspot data (http://solarscience.msfc.nasa.gov/greenwch.shtml) and the staff of the Wilcox Solar Observatory (WSO) for the solar polar field data (http://http://wso.stanford.edu/Polar.html). The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to the Johns Hopkins Applied Physics Laboratory. The data used in this study are available from the Planetary Data Center (https://pds.nasa.gov/). The work at Reading has been funded by the UK Science and Technology Facilities Council (STFC) consolidated grant ST/M000885/1. The work at Leicester has been funded by STFC consolidated grant ST/N000749/1. S.I. is also funded by a Leverhulme Research Fellowship.