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Convective Lineshifts in the Infrared Region of the Solar Spectrum

Published online by Cambridge University Press:  12 April 2016

Devon Hamilton  and
J. B. Lester
Devon Hamilton
Affiliation:
Department of Astronomy, University of Toronto, 60 St. George St., Toronto, Ont., M5S 3H8
J. B. Lester
Affiliation:
Erindale College, University of Toronto

Abstract

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Convective motions in the photospheres of the Sun and solar-type stars can be studied using spectral line asymmetries via line bisectors and line shifts. Over the past few years there has been an improvement in the precision of the line positions for Fe I, CO and OH. These improved positions can be combined with recent high resolution infrared spectra of the Sun to examine how their convective line asymmetries behave with respect to observable line parameters, such as wavenumber and depth. We have completed a survey of convective line shifts for over 650 Fe I lines, 1320 CO lines and 80 OH lines, between 0.9 and 11 μm. The behavior of the distributions of these features, with respect to observed characteristics, is examined. The use of different species allows for an exploration of convective motions at different levels in the solar atmosphere. The large size of the sample allows for a more complete statistical understanding of the distributions. This work complements surveys of line asymmetries in the visible region of the Solar spectrum, and provides a foundation for further studies of convective motions in the spectra of other stars.

Type
Part 7. Convection, Line Asymmetry
Information
International Astronomical Union Colloquium , Volume 170: Precise Stellar Radial Velocities , 1999 , pp. 291 - 296
Copyright
Copyright © Astronomical Society of the Pacific 1999

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