CRISP Spectropolarimetric Imaging of Penumbral Fine Structure
By G. Scharmer, G. Narayan, T. Hillberg, J. Rodríguez, Mats G. Lofdahl, D. Kiselman, P. Sutterlin, M. Noort, A. Lagg. 2008
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We discuss penumbral fine structure in a small part of a pore, observed with the CRISP imaging spectropolarimeter at the Swedish 1-m Solar Telescope (SST), close to its diffraction limit of 0.16″. Milne-Eddington inversions applied to these Stokes data reveal large variations of field strength and inclination angle over dark-cored penumbral intrusions and a dark-cored light bridge. The mid-outer part of this penumbra structure shows ~0.3″ wide spines, separated by ~1.6″ (1200 km) and associated with 30° inclination variations. Between these spines, there are no small-scale magnetic structures that easily can be identified with individual flux tubes. A structure with nearly 10° more vertical and weaker magnetic field is seen midway between two spines. This structure is cospatial with the brightest penumbral filament, possibly indicating the location of a convective upflow from below.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics
View Paper: https://www.semanticscholar.org/paper/1e95e95218b2d7c74cd2577321bd2748716a1c8a
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Citations in the corpus
- CRISPRED: A data pipeline for the CRISP imaging spectropolarimeter (2014, methodology): “…of a relatively large field-of-view (FOV) with very high cadence, very high spatial resolution, and an acceptable wavelength coverage (e.g., Tritschler et al. 2004; Cauzzi et al. 2008; Bello González & Kneer 2008; Scharmer et al. 2008; Steiner et al. 2010; De Pontieu et al. 2012, among others).”
- THE FORMATION OF THE Hα LINE IN THE SOLAR CHROMOSPHERE (2012, methodology): “The observations were obtained with the CRisp Imaging SpectroPolarimeter (CRISP, Scharmer et al. 2008) at the Swedish 1-m Solar Telescope (SST, Scharmer et al. 2003a) on La Palma on May 5,2011 at 7:53UT.”
- ON-DISK COUNTERPARTS OF TYPE II SPICULES IN THE Ca ii 854.2 nm AND Hα LINES (2009, methodology): “The observations were obtained with the CRisp Imaging SpectroPolarimeter (CRISP, Scharmer et al. 2008) installed at the Swedish 1-m Solar Telescope (SST, Scharmer et al. 2003a) on La Palma (Spain).”
- Alfvén Waves in the Solar Atmosphere (2012, methodology): “High-cadence imagers, such as the ROSA (Jess et al. 2010) instrument, will need to be employed with high spatial, temporal, and spectral resolution facilities, such as the IBIS (Cavallini 2006) and CRISP (Scharmer et al. 2008) two-dimensional spectro-polarimeters.”
- Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, methodology): “This has only been made possible through; (i) seeing-free, space-based chromospheric observations provided by Hinode/SOT; (ii) advances in reducing atmospheric distortion through both instrumental (e.g., adaptive optics) and image reconstruction techniques such as speckle (Wöger et al. 2008) and Mul”