caa a22 4500 445346302 CHVBK 20180317142830.0 cr unu---uuuuu 170323e20110801xx s 000 0 eng 10.1007/s11207-011-9809-3 doi (NATIONALLICENCE)springer-10.1007/s11207-011-9809-3 Solar Magnetic Carpet I: Simulation of Synthetic Magnetograms [Elektronische Daten] [K. Meyer, D. Mackay, A. van Ballegooijen, C. Parnell] This paper describes a new 2D model for the photospheric evolution of the magnetic carpet. It is the first in a series of papers working towards constructing a realistic 3D non-potential model for the interaction of small-scale solar magnetic fields. In the model, the basic evolution of the magnetic elements is governed by a supergranular flow profile. In addition, magnetic elements may evolve through the processes of emergence, cancellation, coalescence and fragmentation. Model parameters for the emergence of bipoles are based upon the results of observational studies. Using this model, several simulations are considered, where the range of flux with which bipoles may emerge is varied. In all cases the model quickly reaches a steady state where the rates of emergence and cancellation balance. Analysis of the resulting magnetic field shows that we reproduce observed quantities such as the flux distribution, mean field, cancellation rates, photospheric recycle time and a magnetic network. As expected, the simulation matches observations more closely when a larger, and consequently more realistic, range of emerging flux values is allowed (4×1016 - 1019Mx). The model best reproduces the current observed properties of the magnetic carpet when we take the minimum absolute flux for emerging bipoles to be 4×1016Mx. In future, this 2D model will be used as an evolving photospheric boundary condition for 3D non-potential modeling. Springer Science+Business Media B.V., 2011 Sun: magnetic fields nationallicence Sun: magnetic carpet nationallicence Meyer K. School of Mathematics and Statistics, University of St Andrews, North Haugh, KY16 9SS, St Andrews, Fife, Scotland, UK aut Mackay D. School of Mathematics and Statistics, University of St Andrews, North Haugh, KY16 9SS, St Andrews, Fife, Scotland, UK aut van Ballegooijen A. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, 02138, Cambridge, MA, USA aut Parnell C. School of Mathematics and Statistics, University of St Andrews, North Haugh, KY16 9SS, St Andrews, Fife, Scotland, UK aut Solar Physics Springer Netherlands 272/1(2011-08-01), 29-58 0038-0938 272:1<29 2011 272 11207 https://doi.org/10.1007/s11207-011-9809-3 text/html Onlinezugriff via DOI 1 research-article jats NATIONALLICENCE 856 40 https://doi.org/10.1007/s11207-011-9809-3 text/html Onlinezugriff via DOI NATIONALLICENCE 700 1- Meyer K. School of Mathematics and Statistics, University of St Andrews, North Haugh, KY16 9SS, St Andrews, Fife, Scotland, UK aut NATIONALLICENCE 700 1- Mackay D. School of Mathematics and Statistics, University of St Andrews, North Haugh, KY16 9SS, St Andrews, Fife, Scotland, UK aut NATIONALLICENCE 700 1- van Ballegooijen A. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, 02138, Cambridge, MA, USA aut NATIONALLICENCE 700 1- Parnell C. School of Mathematics and Statistics, University of St Andrews, North Haugh, KY16 9SS, St Andrews, Fife, Scotland, UK aut NATIONALLICENCE 773 0- Solar Physics Springer Netherlands 272/1(2011-08-01), 29-58 0038-0938 272:1<29 2011 272 11207 Metadata rights reserved Springer special CC-BY-NC licence nationallicence BK010053 XK010053 XK010000 NATIONALLICENCE NATIONALLICENCE NL-springer