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LOCATION:Foyer 2nd Floor
DTSTART;TZID=Europe/Stockholm:20220628T090000
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UID:submissions.pasc-conference.org_PASC22_sess181_pos149@linklings.com
SUMMARY:P31 - Methodology for Estimating the Effective Dissipation Coeffic
 ients in Magnetohydrodynamic Simulations of Stellar Plasmas
DESCRIPTION:Poster\n\nP31 - Methodology for Estimating the Effective Dissi
 pation Coefficients in Magnetohydrodynamic Simulations of Stellar Plasmas\
 n\nRiva, Steiner\n\nA crucial step in the post processing of astrophysical
  magnetohydrodynamic (MHD) numerical simulations is the accurate determina
 tion of the effective viscosity and magnetic diffusivity effecting the MHD
  flow. Once these are known, one can determine the dimensionless numbers t
 hat characterise the flow such as Reynolds and Prandtl numbers. These are 
 of particular significance for simulations of the solar and stellar small-
 scale dynamo. The proposed methodology relies on a post processing step ca
 rried out with numerical operators of higher order accuracy than the ones 
 in the simulation code. The poster explains the methodology and presents a
 pplication of it to a number of radiative MHD simulations of various effec
 tive viscosities and plasma resistivities. The proposed methodology provid
 es a solid estimate of the dissipation coefficients affecting the momentum
  and induction equations of MHD simulations. It is found that small-scale 
 dynamos are active and can amplify a small seed magnetic field up to signi
 ficant values in simulations of the solar convection zone with a grid spac
 ing better than 12 km, even at a magnetic Prandtl number as small as 0.65.
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