Polarized Radiation Diagnostics of Magnetohydrodynamic Models of the Solar Atmosphere

Details Polarized Radiation Diagnostics of Magnetohydrodynamic Models of the Solar Atmosphere Polarized Radiation Diagnostics of Magnetohydrodynamic Models of the Solar Atmosphere

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996soph..164..223s&link_type=abstract

Solar Physics, Volume 164, Issue 1-2, pp. 223-242

Physics

34

Magnetohydrodynamics, Polarization, Solar Atmosphere

Scientific paper

Solar magnetic elements and their dynamical interaction with the convective surface layers of the Sun are numerically simulated. Radiation transfer in the photosphere is taken into account. A simulation run over 18.5 minutes real time shows that the granular flow is capable of moving and bending a magnetic flux sheet (the magnetic element). At times it becomes inclined by up to 30° with respect to the vertical around the level τ 5000 = 1 and it moves horizontally with a maximal velocity of 4 km/s. Shock waves form outside and within the magnetic flux sheet. The latter cause a distinctive signature in a time series of synthetic Stokes V-profiles. Such shock events occur with a mean frequency of about 2.5 minutes. A time resolution of at least 10 seconds in Stokes V recordings is needed to reveal an individual shock event by observation.

Affiliated with

Also associated with

No associations

Rating

Polarized Radiation Diagnostics of Magnetohydrodynamic Models of the Solar Atmosphere does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Polarized Radiation Diagnostics of Magnetohydrodynamic Models of the Solar Atmosphere, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Polarized Radiation Diagnostics of Magnetohydrodynamic Models of the Solar Atmosphere will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1618005