2006/11/14 by D. Orozco Suárez, D. Orozco Suarez, L. R. Bellot Rubio +13
Engineering · Physics and Astronomy · #Adaptive optics and wavefront sensing #Astrophysics (astro-ph) #FOS: Physical sciences #Optical Polarization and Ellipsometry #Solar and Space Plasma Dynamics #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0611443
6 pages, 7 figures. Submitted to the proceedings of the conference "The Second Solar Orbiter Workshop", 2006 October 16-20, Athens. To be published by the ESA Publications conference Proceedings
arxiv created 2006/11/14 · openalex publication_date 2006/11/14 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The Visible-light Imager and Magnetograph (VIM) proposed for the ESA Solar Orbiter mission will observe a photospheric spectral line at high spatial resolution. Here we simulate and interpret VIM measurements. Realistic MHD models are used to synthesize "observed" Stokes profiles of the photospheric Fe I 617.3 nm line. The profiles are degraded by telescope diffraction and detector pixel size to a spatial resolution of 162 km on the solar surface. We study the influence of spectral resolving power, noise, and limited wavelength sampling on the vector magnetic fields and line-of-sight velocities derived from Milne-Eddington inversions of the simulated measurements. VIM will provide reasonably accurate values of the atmospheric parameters even with filter widths of 120 mA and 3 wavelength positions plus continuum, as long as the noise level is kept below 10-3 Ic.