Cecilia Payne-Gaposchkin – författare

Cecilia Payne-Gaposchkin became acclaimed in her lifetime as the greatest woman astronomer of all time. Her own story of her professional life, work and scientific achievements is augmented by the personal recollections of her daughter, Katherine Haramundanis, as well as a scientific appreciation by Jesse Greenstein, a historical essay by Peggy Kidwell and, in this new edition, an introduction by Virginia Trimble. Payne-Gaposchkin's overwhelming love for astronomy was her personal guiding light, and her attitude and approach have lessons for all. She received many prestigious awards for her outstanding contributions to science and in 1956 became the first woman to be advanced to the rank of Professor at Harvard University, as well as being the first woman departmental chair. This book will interest both astronomers and those studying the advancement of the position and status of women in society.

Cecilia Payne-Gaposchkin became acclaimed in her lifetime as the greatest woman astronomer of all time. Her own story of her professional life, work and scientific achievements is augmented by the personal recollections of her daughter, Katherine Haramundanis, as well as a scientific appreciation by Jesse Greenstein, a historical essay by Peggy Kidwell and, in this new edition, an introduction by Virginia Trimble. Payne-Gaposchkin's overwhelming love for astronomy was her personal guiding light, and her attitude and approach have lessons for all. She received many prestigious awards for her outstanding contributions to science and in 1956 became the first woman to be advanced to the rank of Professor at Harvard University, as well as being the first woman departmental chair. This book will interest both astronomers and those studying the advancement of the position and status of women in society.

Sects. 12, 13. 89 sequence and that subgiant and fainter stars in globular clusters have ultraviolet excesses. When dealing with stars whose physical properties are imperfectly under­ stood, such as in globular cluster stars, we cannot rely too heavily on the empiri­ cal calibration by the kinds of stars used to define Fig. 5, to determine their true, unreddened U-B, B-V curve. But if by a combination of arguments, principally the reddening in the region of the stars we do known about, we can assign a fairly probable unreddened U-B, B-V curve to a group of stars about which we know little, the argument may be turned around. In this case some information may be gained about the energy envelope of the stars by examining the differences between the normal two-color index curves for the unknown group of stars compared to the known. In general there seem to be two possible causes for different stars defining different normal sequences in the U-B, B-V plane. One, the relative energy distribution in the continuum in the U, B and V photometry bands are different. An example of this is the effect of the Balmer depression in supergiants. This, of course, requires deviation from black body radiation curves for one or both groups of stars. This cause seems to be the dominant effect for very blue, hot stars where the depression of the continuum by absorption lines is at a minimum.