Precision Asteroseismology Iau S301

IAU Symposium 301 highlights the recent advances in the field of asteroseismology and was the twenty-first in a series of pulsation meetings started in Los Alamos in 1971 and held every two years. Topics discussed centred around seismic studies of all types of pulsating stars, which - in the era of space observations made by MOST, CoRoT and Kepler - use data of unprecedented precision. The Symposium was also the opportunity to honour Wojtek Dziembowski, one of the world's leaders in the study of solar and stellar pulsations. Highlights include contributions on observing from space and the ground, techniques of analysis and mode identification, astrophysical applications of pulsations, pulsation-convection interaction, mass loss, microphysics, pulsations in main-sequence stars, compact stars and supergiants, and solar-like oscillations. Containing many excellent reviews, this volume is an important reference source for researchers on solar and stellar pulsations.

Develops a fresh mathematical approach to coronal seismology, explaining oscillatory phenomena by drawing upon original research and complex modelling techniques.

I have felt the need for a book on the theory of solar magnetic fields for some time now. Most books about the Sun are written by observers or by theorists from other branches of solar physics, whereas those on magnetohydrodynamics do not deal extensively with solar applications. I had thought of waiting a few decades before attempting to put pen to paper, but one summer Josip Kleczek encouraged an im mediate start 'while your ideas are still fresh'. The book grew out of a postgraduate lecture course at St Andrews, and the resulting period of gestation or 'being with monograph' has lasted several years. The Sun is an amazing object, which has continued to reveal completely unexpected features when observed in greater detail or at new wavelengths. What riches would be in store for us if we could view other stars with as much precision! Stellar physics itself is benefiting greatly from solar discoveries, but, in tum, our understanding of many solar phenomena (such as sunspots, sunspot cycles, the corona and the solar wind) will undoubtedly increase in the future due to their observation under different conditions in other stars. In the 'old days' the solar atmosphere was regarded as a static, plane-parallel structure, heated by the dissipation of sound waves and with its upper layer expanding in a spherically symmetric manner as the solar wind. Outside of sunspots the magnetic field was thOUght to be unimportant with a weak uniform value of a few gauss.

In the history books, the Italo-Ethiopian War will doubtless be entered as one of the strangest wars ever waged. History will record the spectacle of a primitive people—haphazardly armed and lacking in modern military technique—seeking to resist Mussolini’s modern war machine by tribal cunning on the battlefield and up-to-date intrigue in the diplomatic councils of Europe. But what the history books will not record, W.W. (“Bill”) Chaplin tells in this fascinating volume. It is behind the scenes of politics and bloodshed in this curious conflict that Mr. Chaplin takes the reader in a vivid diary of his day-by-day experiences and observations at the Italo-Ethiopian War front. Written with the dramatic simplicity of a newspaperman trained in the art of brevity, Mr. Chaplin’s account of the thousand and one quixotic incidents in a war correspondent’s life in Ethiopia sparkles with interest and amusement. From the beginning when he describes his departure on an Italian troop-ship at Naples to the very end when he returns to the same port as the approaching rainy season slows down the pace of the war, Mr. Chaplin records an odyssey as strange as the war itself. The reader is led through picturesque by-ways into the heart of the Ethiopian war zone and shown not only what war has wrought on the battlefield but what it has wrought in the hearts of fighting men. This and much more that is of human texture, Mr. Chaplin tells in a diary that reflects undiluted curiosity and a subtle sense of the dramatic.

"Four hundred years after Kepler discovered his third law of planetary motion, disproving the Pythagorean notion of 'the music of the spheres', music was discovered in the Sun. With this discovery the science of helioseismology was born." "In Music of the Sun, renowned helioseismologist William Chaplin tells the story of this discipline's origins and gives us invaluable insight into its implications - not only for better understanding the distant sun and stars - but for climate change, particle physics, and the very relationship between the Sun and the Earth."--BOOK JACKET.

The reconnection of magnetic fields is one of the most fascinating processes in plasma physics, responsible for phenomena such as solar flares and magnetospheric substorms. The concept of reconnection has developed through recent advances in exploring the magnetospheres of the Sun and Earth through theory, computer simulations and spacecraft observations. The great challenge in understanding it stems from balancing the large volumes of plasma and magnetic fields involved with the energy release with the physical mechanism which relies on the strongly localized behavior of charged particles. This book, edited by and with contributions from leading scientists in the field, provides a comprehensive overview of recent theoretical and observational findings concerning the physics of reconnection and the complex structures that may give rise to, or develop from, reconnection. It is intended for researchers and graduate students interested in the dynamics of plasmas.

This work has been selected by scholars as being culturally important and is part of the knowledge base of civilization as we know it. This work is in the public domain in the United States of America, and possibly other nations. Within the United States, you may freely copy and distribute this work, as no entity (individual or corporate) has a copyright on the body of the work. Scholars believe, and we concur, that this work is important enough to be preserved, reproduced, and made generally available to the public. To ensure a quality reading experience, this work has been proofread and republished using a format that seamlessly blends the original graphical elements with text in an easy-to-read typeface. We appreciate your support of the preservation process, and thank you for being an important part of keeping this knowledge alive and relevant.