Synopses & Reviews
This volume presents a selection of papers on the state of the art of image enhancement, automated feature detection, machine learning, and visualization tools in support of solar physics that focus on the challenges presented by new ground-based and space-based instrumentation. The articles and topics were inspired by the Third Solar Image Processing Workshop, held at Trinity College Dublin, Ireland but contributions from other experts have been included as well. This book is mainly aimed at researchers and graduate students working on image processing and compter vision in astronomy and solar physics.
Synopsis
This title collects refereed papers submitted to the Third Solar Image Processing Workshop, (6-8 September, 2006, Trinity College Dublin, Ireland). The workshop brought together researchers in image processing and solar physics to focus on the challenges presented by new ground-based and space-based instrumentation. Topics covered include image enhancement, automated feature detection, machine learning and visualization tools in support of solar physics.
Synopsis
The SECCHI A and B instrument suites (Howard et al., 2006) onboard the two STEREO mission spacecraft (Kaiser, 2005) are each composed of: one Extreme Ultra-Violet Imager (EUVI), two white-light coronagraphs (COR1 and COR2), and two wide-angle heliospheric imagers (HI1 and HI2). Technical descriptions of EUVI, COR1 and the HIs can be found in Wuelser et al. (2004), Thompson et al. (2003), and De?se et al. (2003), respectively. The images produced by SECCHI represent a data visualization challenge: i) the images are 20482048 pixels (except for the HIs, which are usually binned onboard 22), thus the vast majority of computer displays are not able to display them at full frame and full r- olution, and ii) more importantly, the ?ve instruments of SECCHI A and B were designed to be able to track Coronal Mass Ejections from their onset (with EUVI) to their pro- gation in the heliosphere (with the HIs), which implies that a set of SECCHI images that covers the propagation of a CME from its initiation site to the Earth is composed of im- ?1 ages with very different spatial resolutions - from 1. 7 arcsecondspixel for EUVI to 2. 15 ?1 arcminutespixel for HI2, i. e. 75 times larger. A similar situation exists with the angular scales of the physical objects, since the size of a CME varies by orders of magnitude as it expands in the heliosphere.
Synopsis
This volume contains papers from the Third Solar Image Processing Workshop, held in Dublin, Ireland in September, 2006. Topics covered include image enhancement, automated feature detection, machine learning and visualization tools in support of solar physics.
Table of Contents
Preface: A Topical Issue on Solar Image Analysis and Visualization.- FESTIVAL: A Multiscale Visualization Tool for Solar Imaging Data.- Visualization of Distributed Solar Data and Metadata with the Solar Weather Browser.- Widespread Occurrence of Trenching Patterns in the Granulation Field: Evidence for Roll Convection?.- Principal Components and Independent Component Analysis of Solar and Space Data.- Automatic Recognition and Characterisation of Supergranular Cells from Photospheric Velocity Fields.- Automated McIntosh-Based Classification of Sunspot Groups Using MDI Images.- Multifractal Properties of Evolving Active Regions.- Multiscale Analysis of Active Region Evolution.- A Comparison of Feature Classification Methods for Modeling Solar Irradiance Variation.