Evolution of the large-scale magnetic field on the solar surface: a parameter study

By I. Baumann, D. Schmitt, M. Schüssler, S. Solanki. 2004

142 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/6eb83a12406cfb82e9cc39a6951c57952af5e7d2

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In Astronomy and Astrophysics

Citations in the corpus

The Case for a Distributed Solar Dynamo Shaped by Near-Surface Shear (2005, background): “[The poleward branch could also be due poleward flows – as demonstrated convincingly by flux transport models; see Baumann et al. (2004) and Schüssler (2005).]”
Solar Surface Magnetism and Irradiance on Time Scales from Days to the 11-Year Cycle (2009, methodology): “Instead of magnetograms, it is also possible to use flux transport simulations, such as those of Schrijver et al. (2003), or Baumann et al. (2004, 2006).”
Sunspot Group Tilt Angles and the Strength of the Solar Cycle (2010, background): “Obviously, the total amount of magnetic flux emerging over a cycle,φtot, is another central parameter influencing the polar flux (Baumann et al., 2004).”
Solar Cycle Prediction Using Precursors and Flux Transport Models (2006, background): “Two-dimensional versions of such models have successfully reproduced the observed evolution of the solar surface field (e.g., Wang et al. 1989a,b; van Ballegooijen et al. 1998; Schrijver 2001; Durrant et al. 2004; Baumann et al. 2004).”
Flux-Transport Dynamos with Lorentz Force Feedback on Differential Rotation and Meridional Flow: Saturation Mechanism and Torsional Oscillations (2006, background): “…is the essential ingredient in models describing the evolution of the surface magnetic field assimilating real observations (Schrijver et al. 2002; Baumann et al. 2004, 2006; Wang et al. 2005)) this is of secondary concern for the model presented here; it is however of primary interest for…”
Dynamo Models of the Solar Cycle (2005, background): “, 2002; Baumann et al., 2004, and references therein). The key question is whether this is an active component of the dynamo cycle, or a mere side-effect of active region decay. Likewise, the buoyant instability of magnetic flux tubes (Section 4.7) is, in some sense, unavoidable; here again the ques”
ON THE WEAKENING OF THE POLAR MAGNETIC FIELDS DURING SOLAR CYCLE 23 (2009, background): “The mechanism of polar field formation and reversal, as it occurs at the photosphere, may be summarized as follows (see, e.g., Wang & Sheeley 1991; Baumann et al. 2004; Cameron & Schüssler 2007; Schrijver & Liu 2008).”
Magnetic Flux Transport at the Solar Surface (2014, methodology): “The other method was initiated by van B llegooijen et al. (1998) and was adopted by others (Mackay et al. 2002a,2002b;Baumann et al. 2004; Schüssler and Baumann 2006; Cameron et al. 2010; Jiang et al. 2011b; Upton and Hathaway 2014).”
Solar Dynamo Theory (2014, background): “…the MHD induction equation on a spherical shell subjected to the advective and shearing action of surface differential rotation, poleward meridional flow, diffusion, and injection of tilted bipolar sunspot pairs (Wang et al. 1989, Wang & Sheeley 1991, Baumann et al. 2004, Jiang et al. 2013).”