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Inferences of Plasma Parameters from Coronal Hole Observations

Published online by Cambridge University Press:  12 April 2016

Shadia Rifai Habbal
Shadia Rifai Habbal*
Affiliation:
Harvard-Smithsonian Center for Astrophysics

Abstract

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The temperature in the acceleration region of the solar wind remains one of the most elusive parameters to measure. Knowledge of the temperature as well as its gradient in the inner corona is fundamental for placing constraints on physical mechanisms thought to be responsible for the coronal heating process, as well as for understanding the flow properties of the solar wind. Estimates of the helium abundance is essential for understanding the puzzling behavior of heavier ions in the solar wind. As an illustration of the difficulties and uncertainties involved in the inferences of plasma parameters in the solar wind acceleration region, the inference of electron temperature and helium abundance will be described. Prospects for future observations will be briefly discussed.

Keywords

TemperatureHelium AbundanceSolar Wind
Type
Coronal Heating and Solar Wind Acceleration
Information
International Astronomical Union Colloquium , Volume 154: Solar and Interplanetary Transients , 1996 , pp. 49 - 56
Copyright
Copyright © Kluwer 1997

References

Bame, S.T., et al.: 1977, J. Geophys. Res., 82, 1487.CrossRefGoogle Scholar
Bürgi, A., and Geiss, J.: 1986, Sol. Phys., 103, 347.Google Scholar
Domingo, V. (ed.): 1989, The SOHO Mission - Scientific and Technical Aspects of the Instruments, ESA SP-1104.Google Scholar
Habbal, S.R. and Withbroe, G.L.: 1981, Solar Phys. 69, 77.Google Scholar
Habbal, S.R., Esser, R., and Arndt, M.B.: 1993, Ap. J., 413, 435.Google Scholar
Habbal, S.R., and Esser, R.: 1994, Ap. J., 421, L59.Google Scholar
Koutchmy, S.: 1977, Solar Phys., 51, 399.Google Scholar
Joselyn, J.A. and Holzer, T.E.: 1978, J. Geophys. Res. 83, 1019.Google Scholar
Mariska, J.T.: 1992, The Solar Transition Region, Cambridge University Press.Google Scholar
Parkinson, J.H. and Gabriel, A.H.: 1986, Adv. Space Res. 6 (8), 243.CrossRefGoogle Scholar
Reeves, E.M., et al.: 1977, Appi. Optics, 16, 849.Google Scholar
Thieme, K.M., Marsch, E., and Schwenn, R.: 1989, Adv. Space Res., 9, 127.Google Scholar
Tsuneta, S.,et al.: 1991, Solar Phys., 136, 37.Google Scholar
Woo, R.: 1995, this volume.Google Scholar