The Behavior of the Open Magnetic Field of the Sun

By L. Fisk, N. Schwadron. 2001

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In Astronomy and Astrophysics

Citations in the corpus

The Heliospheric Magnetic Field (2013, background): “Fisk and Schwadron (2001) suggest HCS rotation is driven by a diffusive process involving reconnection between open and closed flux (interchange reconnection, Crooker et al., 2002), which is thought to continually operate at the coronal hole boundaries (Nash et al., 1988; Wang and Sheeley Jr, 2004).”
What Is Missing from Our Understanding of Long-Term Solar and Heliospheric Activity? (2002, background): “This likely has implications for the behavior of the heliospheric field (see Fisk & Schwadron 2001).”
Observations of discrete, global magnetospheric oscillations directly driven by solar wind density variations (2003, background): “[35] A possible mechanism for the generation of the periodic solar wind density variations is interchange reconnection, which reconnects open flux tubes with closed flux tubes, leading to an influx of new plasma [Fisk, 1996; Fisk and Schwadron, 2001; Wang, 1998; Crooker et al., 2002].”
Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus (2015, background): “…of the importance of interchange reconnection, a model that aims to jointly explain coronal heating and solar wind formation by proposing that open magnetic field lines are present all over the Sun, including regions that are predominantly closed (Fisk and Schwadron 2001; Crooker et al. 2002).”
MAGNETOHYDRODYNAMIC WAVES AND CORONAL HEATING: UNIFYING EMPIRICAL AND MHD TURBULENCE MODELS (2012, background): “n Eq.(2) applied to the radial components of the Poynting ux, P R, and the magnetic eld, B R, is a keystone of the Fisk theory for the solar wind (see Fisk (1996); Fisk et al. (1999b,a); Fisk (2001); Fisk and Schwadron (2001). Then, Farrugia et al. (1997) (and the works cited therein) formulated an ”
Flux tube texture of the solar wind: Strands of the magnetic carpet at 1 AU?: FLUX TUBE TEXTURE OF SOLAR WIND (2008, background): “Also, it might be possible to measure the timescales and spatial scales needed to calculate open-flux diffusion coefficients [cf. Fisk and Schwadron, 2001; Cohen et al., 2006].”
Global distribution of the solar wind during solar cycle 23: ACE observations (2009, result): “And our result is also consistent with models for the global transport of the magnetic field of the Sun that have been developed by Fisk and colleagues [Fisk et al., 1999; Fisk and Schwadron, 2001; Fisk, 2005].”
Acceleration of the solar wind as a result of the reconnection of open magnetic flux with coronal loops (2003, background): “…for the configuration of the heliospheric magnetic field and offers an explanation for the formation of coronal holes and the apparent rotation of the large-scale current sheet that separates opposite polarities of the heliospheric magnetic field during the solar cycle [Fisk and Schwadron, 2001].”
Solar Orbiter (2012, background): “The magnetic connection between the solar wind and the solar source therefore hinges on understanding what determines the amount of open flux from the Sun, how open field lines are distributed at the solar surface at any given time, and how these open field lines reconnect and change their connectio”