The long‐term variation of the Sun's open magnetic flux

By Y. Wang, J. Lean, N. R. Sheeley. 2000

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In Astronomy and Astrophysics

Citations in the corpus

The Behavior of the Open Magnetic Field of the Sun (2001, background): “The fact that CMEs could add to the open magnetic Ñux is then a potential puzzle, since the heliospheric magnetic Ñux is observed to be relatively constant in time (Wang et al. 2000a ; Balogh & Smith 2001).”
Secular variation of the Sun's magnetic flux (2002, background): “…latter, which comprises between roughly 10% (solar maximum) and up to 30% (solar minimum) of the unsigned photospheric magnetic flux measured on scales larger than about 10 arcsec (Harvey 1994b; Wang et al. 2000), the question arises whether there is a secular variation of the total flux as well.”
The Heliospheric Magnetic Field (2013, background): “Bottom: 1-AU open solar flux (OSF), in the same format.”
Modeling the Sun’s Magnetic Field and Irradiance since 1713 (2005, background): “At least on timescales on the order of or less than a solar cycle, the open flux is rather poorly correlated with sunspot activity, unlike the closed flux that controls the solar irradiance (see Wang et al. 2000).”
Topological Methods for the Analysis of Solar Magnetic Fields (2005, background): “As a consequence Φopen tends to reach its maximum when the dipole moment is largest some time near solar minimum (Wang et al., 2000).”
Solar cycle changes in coronal holes and space weather cycles (2002, background): “The interplanetary magnetic field magnitude cycle coincides with the latter part of the sunspot maximum and declining phase when the total coronal hole area is greatest [Wang, 1993; Wang et al., 2000], with active regions contributing to their fields.”
An Antarctic view of Beryllium-10 and solar activity for the past millennium (2011, methodology): “Further, calculations by Webber and Higbie (2003) show that the 10Be production increase due to the same modulation parameter decrease (700–500 MV) is about 20% at high latitudes ([60 ), and 9% at middle latitudes (40 ).”
Sources of geomagnetic activity during nearly three solar cycles (2002, background): “The calculated open flux tends to decline more slowly during the declining phase of the solar cycle (in particular in 1985-88) though this may be an instrumental effect caused by the difficulty of measuring fields at high latitudes [Wang et al., 2000].”
Solar radiative output and its variability: evidence and mechanisms (2004, background): “Furthermore, it is the open coronal ux, not the total ux, that extends into the heliosphere and controls geomagnetic activity and cosmic ray uxes (Cane et al., 1999; Wang et al., 2000; Arge et al., 2002).”
Extreme Ultraviolet Variability Experiment (EVE) on the Solar Dynamics Observatory (SDO): Overview of Science Objectives, Instrument Design, Data Products, and Model Developments (2010, background): “…EUV sources are properly connected to surface magnetic fields, the EUV irradiance variations become amenable to study in terms of source emergence, meridional transport and diffusion, as encapsulated in current flux-transport models (Wang, Lean, and Sheeley, 2000; Wang, Sheeley, and Lean, 2000).”
The effect of increasing solar activity on the Sun's total and open magnetic flux during multiple cycles: Implications for solar forcing of climate (2002, background): “Increasing solar cycle amplitudes produce a secular increase in open flux and IMF, and can therefore explain variations like the cosmogenic isotope decrease from 1922 to 1965.”