Simulations of the Photospheric Magnetic Activity and Outer Atmospheric Radiative Losses of Cool Stars Based on Characteristics of the Solar Magnetic Field

By C. Schrijver. 2001

152 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/a6272f8054e1e715620577f261e68737dda5924f

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In Astronomy and Astrophysics

Citations in the corpus

Modeling the Sun’s Magnetic Field and Irradiance since 1713 (2005, methodology): “…pole separation to every BMR, we plan in subsequent work to employ an observationally based distribution of sizes, as in the simulations of Schrijver (2001) or ofWang et al. (2002b), where the source term comprised 3000 bipoles whose properties were determined individually from…”
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).”
Evolution of the large-scale magnetic field on the solar surface: a parameter study (2004, methodology): “More recently, flux transport models have been used to simulate the spreading of single bipoles (Mackay et al. 2002a; Wang et al. 2000) and whole activity cycles (Schrijver 2001; Mackay et al. 2002b).”
What Is Missing from Our Understanding of Long-Term Solar and Heliospheric Activity? (2002, methodology): “The model was demonstrated to accurately reproduce both geometric and quantitative properties of the last sunspot cycles (Schrijver 2001), including the polar regions (Schrijver & Title 2001).”
Magnetic Flux Transport at the Solar Surface (2014, methodology): “One approach, adopted by Schrijver (2001) and Upton and Hathaw y (2014), is to include in the advection velocities and small-scale cellular flows or random motions corresponding to, e.g., supergranulation.”
On the Formation of Polar Spots in Sun-like Stars (2001, methodology): “An e†ective Ñux-weighted Ñux dispersal coefficient for our nonlinear model can be deÐned by D*(r) 4 /0= 'N(')D0C2(') d' /0= 'N(') d' , (4) where the function C(') \ 1.7 exp (['/3 ] 1019) reÑects the changing rms velocity of concentrations with Ñux ' (Schrijver 2001), and km2 s~1.”