The Properties of Small Magnetic Regions on the Solar Surface and the Implications for the Solar Dynamo(s)

By H. Hagenaar, C. Schrijver, A. Title. 2002

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In Astronomy and Astrophysics

Citations in the corpus

Modeling the Sun’s Magnetic Field and Irradiance since 1713 (2005, background): “Ephemeral regions are small bipoles having pole separations sP 15;000 km, total fluxes f0 1019 Mx, and lifetimes < 1 day (see Harvey-Angle 1993; Hagenaar 2001; Hagenaar et al. 2003).”
Dynamo Models of the Solar Cycle (2005, background): “Ample observational evidence now exists that a substantial portion of the Sun’s surface magnetic flux is continuously being reprocessed on a timescale commensurate with convective motions (see Schrijver et al., 1997; Hagenaar et al., 2003).”
The magnetic field in the solar atmosphere (2014, background): “Their number varies much less over a solar cycle than that of ARs and there are inconsistent results regarding whether their number varies in phase or in anti-phase with the solar cycle (Martin and Harvey 1979; Martin 1988; Hagenaar et al. 2003).”
A solar surface dynamo (2007, background): “On the other hand, the increasing flux replenishment rates towards smaller scales (Hagenaar et al., 2003) and the absence of a significant variation of the QS flux between solar minimum ⋆ Present address: Sterrekundig Instituut, Utrecht University, Postbus 80 000, 3508 TA Utrecht, The Netherlands…”
The solar magnetic field (2006, background): “Magnetic flux appears at the solar surface in the form of bipolar magnetic regions with a wide range of values for the (unsigned) magnetic flux and lifetimes [13, 14].”
Reconstruction of solar total irradiance since 1700 from the surface magnetic flux (2007, background): “Hagenaar et al. (2003) found, however, that the number density of emerging ER decreased by about a factor of 1.5 from 1997 (i.e. right after the sunspot minimum in 1996) to a minimum in 2000 (when the sunspot number reached its maximum).”
SIMULATION OF THE FORMATION OF A SOLAR ACTIVE REGION (2010, background): “Observations of active regions on the solar surface indicate that, in terms of magnetic flux content, there is a continuous spectrum of active region sizes (Zwaan 1978, 1987; Harvey & Martin 1973; Schrijver & Zwaan 2000; Hagenaar 2001; Hagenaar et al. 2003).”
Magnetic flux emergence in granular convection: radiative MHD simulations and observational signatures (2007, background): “In terms of the amount of magnetic flux in each polarity, there is a continuous spectrum of active region sizes (Hagenaar et al., 2003).”