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This book describes the design and development of an instrument called the Solar Vector Magnetograph or SVM. This instrument maps the magnetic field of the solar active regions. The magnetic field of solar active regions is responsible for the eruptive phenomena on the sun which expel large amounts of high-energy particles and radiation in the interplanetary space posing danger for human activities in space. The careful measurement of solar magnetic field is very important to track its evolution which may be useful for forecasting the solar eruptive events. The instrument SVM was developed by Dr. Sanjay Gosain during his Ph.D. at Udaipur Solar Observatory, India for which he received best thesis award by Astronomical Society of India. This book describes how the high-cadence magnetic field measurements can be done by using a tunable Fabry-Perot etalon and a polarimeter. This book is useful for any solar astronomer who wishes to develop an instrument for measuring solar magnetic fields or wishes to understand how solar magnetic field is measured using Zeeman-effect diagnostics. The techniques of optical polarimetry is also discussed in depth.
Annotation This proceedings volume of the September 2000 workshop presents recent developments in spectropolarimetry and the measurement of solar magnetic fields using the Zeeman and Hanle effects. The 67 papers address new instrumentation for telescopes, weak polarization and coronal magnetic fields, infrared polarimetry and the physics of active regions, magnetohydrodynamic (MHD) simulations, high resolutions polarimetry and the physics of flux tubes, and the analysis of Stokes profiles. No subject index. Annotation c. Book News, Inc., Portland, OR (booknews.com)
Written by an experienced teacher and author, this must-have source for work with polarimetric equipment and polarimetry in astronomy conveys the knowledge of the technology and techniques needed to measure and interpret polarizations. As such, this monograph offers a brief introduction and refresher, while also covering in detail statistics and data treatment as well as telescope optics. For astronomers, physicists and those working in the optical industry.
Summarising the striking advances of the last two decades, this reliable introduction to modern astronomical polarimetry provides a comprehensive review of state-of-the-art techniques, models and research methods. Focusing on optical and near-infrared wavelengths, each detailed, up-to-date chapter addresses a different facet of recent innovations, including new instrumentation, techniques and theories; new methods based on laboratory studies, enabling the modelling of polarimetric characteristics for a wide variety of astronomical objects; emerging fields of polarimetric exploration, including proto-planetary and debris discs, icy satellites, transneptunian objects, exoplanets, and the search for extraterrestrial life; and unique results produced by space telescopes, and polarimeters aboard exploratory spacecraft. With contributions from an international team of accomplished researchers, this is an ideal resource for astronomers and researchers working in astrophysics, earth sciences, and remote sensing keen to learn more about this valuable diagnostic tool. The book is dedicated to the memory of renowned polarimetrist Tom Gehrels.
"The polarization study of celestial objects is a valuable part of optical astronomy, and the author has done exceptionally well in bringing to gether contributions treating all aspects of the polarimetry field. . . . The first section contains a fine introduction and an excellent and definitive history of the subject. . . . The volume is well illustrated. . . . Highly recommended."ÑChoice "The high quality of this book is clearly due to strict editorial attention to each paper and the discussions. Gehrel's book will surely stand for many years as the fundamental reference source for polarization studies in astronomy as well as in atmospheric physics."ÑJournal of the Assoc. of Lunar and Planetary Observers
Novel instruments for high-precision imaging polarimetry have opened new possibilities, including for exploring effects in radiative scattering, atomic physics, spectral line formation, and radiative transfer. This volume gives a comprehensive and up-to-date account of this rapidly evolving and interdisciplinary field of science.
Spectropolarimetry embraces the most complete and detailed measurement and analysis of light, as well as its interaction with matter. This book provides an introductory overview of the area, which plays an increasingly important role in modern solar observations. Chapters include a comprehensive description of the polarization state of polychromatic light and its measurement, an overview of astronomical (solar) polarimetry, the radiative transfer equation for polarized light, and the formation of spectral lines in the presence of a magnetic field. Most topics are dealt with within the realm of classical physics, although a small amount of quantum mechanics is introduced where necessary. This text will be a valuable reference for graduates and researchers in astrophysics, solar physics and optics.
This thesis is devoted to the development and the application of novel instrument systems and measuring techniques in the field of solar polarimetry. The work is split into three parts, each part addressing an independent project in terms of scientific objectives and implementation. In the first part I describe the development and implementation of a tunable narrow-band filter system to be used in combination with the Zurich Imaging Polarimeter for quasi-monochromatic imaging vector polarimetry. Its working range covers the visible spectrum between 390 nm and 660 nm. The bandwidth varies between 2 pm and 12 pm, depending on wavelength and optical setup. The main filter components are two lithium-niobate Fabry-Pérot interferometers which can be tuned by applying a voltage or by changing the temperature. In the current version of the instrument the interferometers are used in series in a single-pass tandem configuration. The filter system will allow us to explore the spatial structuring of the polarized solar spectrum, including vector mapping of the Hanle and Zeeman effects in any spectral line. First polarimetric images recorded at the SST and at IRSOL in the spectral lines of Ca I 422.7 nm, Sr I 460.7 nm and Hα 656.3 nm show that the instrumentation and its operation is technically mature. The filter system is now available for scientific observations. The second part deals with a laboratory experiment linked to a solar polarization anomaly that has remained an unresolved enigma for many years. While scattering processes usually produce polarized radiation, certain spectral lines, in particular the Fraunhofer D1line of neutral sodium at 589.6 nm should be intrinsically unpolarizable according to the standard quantum mechanical scattering theory. In contrast, observations in quiet regions on the Sun reveal a polarization peak centered in the D1 line core. As the solar atmosphere is a complex environment with an optically thick medium permeated by a tangled and fractal-like magnetic field, we have set up a laboratory experiment with a sodium vapor cell to obtain an answer to the question: Is the sodium D1 anomaly a problem for atomic or for solar physics? The experimental results are consistent with the theoretical null prediction of atomic physics. Furthermore the experiment gives an upper limit for the D1 polarization which is smaller than the signal observed on the Sun. Although this result does not provide the definitive answer to the problem, it permits to conclude that the clarification of the D1 anomaly has to involve solar physics. The third project included in this thesis is the development of a dedicated instrument to capture the polarization of the chromospheric emission spectrum (flash spectrum) during the total solar eclipse of March 29, 2006. The whole visible range and small overlaps with near UV and near IR have been covered with a spectral resolution of 3000. The minimum sampling period was chosen to be 20 ms, which corresponds to a height resolution of some 10 km in the solar atmosphere, along the direction of the lunar movement. The flash spectrum has been successfully recorded during the above-mentioned eclipse in the Sahara desert in southern Libya. For several spectral lines the noise level in the degree of polarization is of order 1% which allows us to compare with theoretical predictions. However, it is tricky to correct for the systematic errors because of optical aberrations in the observed spectra.