The Role of Reconnection in Controlling Interplanetary Magnetic Flux Depletion in Forming the Heliospheric Solar Cycle

Details The Role of Reconnection in Controlling Interplanetary Magnetic Flux Depletion in Forming the Heliospheric Solar Cycle The Role of Reconnection in Controlling Interplanetary Magnetic Flux Depletion in Forming the Heliospheric Solar Cycle

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh33c..03c&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH33C-03

Physics

[2162] Interplanetary Physics / Solar Cycle Variations, [2723] Magnetospheric Physics / Magnetic Reconnection

Scientific paper

We examine the Omni data set of 1 AU observations over the past 15 years that constitute the latest solar cycle. We show that the interplanetary magnetic field continues to be depleted at low latitudes throughout the protracted solar minimum reaching levels below previously predicted minima. We obtain a rate of flux removal resulting in magnetic field reduction by 0.5 nT/yr at 1 AU when averaged over the years 2005--09 that reduces to 0.3 nT/yr for 2007-09 and show that the flux removal operates on field lines that follow the nominal Parker spiral orientation. We argue that the field line reduction can only be accomplished by ongoing reconnection of nominally open field lines. We develop a model for the levels of magnetic flux in the heliosphere, which represents a balance between new flux created by CMEs and flux lost through reconnection near the Sun. This magnetic flux balance is a fundamental property that regulates the plasma and radiation environment of our solar system.

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