Abstract
The OVI resonance doublet is partly collisionally and partly radiatively excited in the solar corona. In the solar wind the OVI ions can attain sufficient outflow speed to cause excitation of the 2R½ level by the chromospheric CII λ1037.0 line. We show that this extends the diagnostic possibilities of the OVI resonance doublet. In particular, the determination of the intensity ratio of the doublet lines at several heights can be sufficient to yield the solar wind velocity at those heights and hence information on the mechanisms of solar wind acceleration.
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© 1986 D. Reidel Publishing Company
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Noci, G., Kohl, J.L., Withbroe, G.L. (1986). OVI Diagnostics of Solar Wind Generation. In: Marsden, R.G. (eds) The Sun and the Heliosphere in Three Dimensions. Astrophysics and Space Science Library, vol 123. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-4612-5_6
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DOI: https://doi.org/10.1007/978-94-009-4612-5_6
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-8549-6
Online ISBN: 978-94-009-4612-5
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