The solar magnetic field

By S. Solanki, B. Inhester, M. Schüssler. 2006

256 citations recorded by the source corpus.

The magnetic field of the Sun is the underlying cause of the many diverse phenomena combined under the heading of solar activity. Here we describe the magnetic field as it threads its way from the bottom of the convection zone, where it is built up by the solar dynamo, to the solar surface, where it manifests itself in the form of sunspots and faculae, and beyond into the outer solar atmosphere and, finally, into the heliosphere. On the way it transports energy from the surface and the subsurface layers into the solar corona, where it heats the gas and accelerates the solar wind.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/68d612450118570a310dc28f2bdfd52f4cf0a1e9

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Citations in the corpus

Observations of Cool-Star Magnetic Fields (2012, background): “Interestingly, the fields appear in groups consisting of at least two areas in close proximity and of opposite polarity (for an overview of the solar magnetic field, see, e.g., Solanki et al., 2006).”
Solar Surface Magnetism and Irradiance on Time Scales from Days to the 11-Year Cycle (2009, background): “D models need to be invoked (see, e.g. Solanki et al. 2006 for a review, see also the discussion in Sect.”
Fluctuation dynamo and turbulent induction at low magnetic Prandtl numbers (2007, background): “…magnetic fluctuations pervade the solar photosphere (e.g., Domı́nguez Cerdeña et al. 2003, Socas-Navarro & Lites 2004, Trujillo Bueno et al. 2004, Solanki et al. 2006), the numerical evidence used to argue that the turbulent fluctuation dynamo is responsible has thus far been based on…”
The Solar Optical Telescope for the Hinode Mission: An Overview (2007, background): “Recent progress of the groundbased observations show that the solar magnetic fields consist of an ensemble of fine (≈0”.1−0”.2) scale magnetic fields in addition to sunspots and pores (Solanki, Inhester, and Schüssler, 2006).”
Solar Dynamo Theory (2014, background): “Numerous good reviews are available on the observational side of solar magnetism (e.g., Solanki et al. 2006, de Wijn et al. 2009); consequently, the following overview focuses on aspects most pertinent to solar dynamo theory.”
The standard flare model in three dimensions II: upper limit on solar flare energy (2012, methodology): “They are respectively 700 G in the penumbra, and 3500 G in the umbra (Solanki et al. 2006; Pevtsov et al. 2011).”
The magnetic field in the solar atmosphere (2014, background): “field lines seemingly not connecting back to the solar surface (Schrijver et al. 1999; Solanki et al. 2006).”
Chromospheric activity catalogue of 4454 cool stars (2018, background): “The Sun also exhibits several cycles that are not as dominant as the 11-year cycle (see Solanki et al. 2006, for more details on solar activity).”