SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 335, 691-702 (1998)

Next Section Table of Contents

Element fractionation in the solar chromosphere driven by ionization-diffusion processes

Hardi Peter

Max-Planck-Institut für Aeronomie, D-37191 Katlenburg-Lindau, Germany (hPeter@linmpi.mpg.de)

Received 11 August 1997 / Accepted 24 March 1998

Abstract

An ionization-diffusion mechanism is proposed to understand the first ionization potential (FIP) fractionation as observed in the solar corona and the solar wind. The enrichment of the low-FIP elements ([FORMULA]10 eV) compared to the high-FIP elements in a large variety of phenomena, as e.g. slow and fast wind or polar plumes, is explained. Also the special behaviour of the heavy noble gases becomes perceptive and the absolute fractionation, i.e. in relation to hydrogen, can be calculated and fits well to the measurements. Additionally the theoretical velocity-dependence of the fractionation will be used to determine the velocities of the solar wind in the chromosphere. The main achievement of this paper is the explanation of a great variety of fractionation-related phenomena on the basis of one single model.

Key words: Sun: abundances – Sun: chromosphere – solar wind

Present address: High Altitude Observatory/NCAR, P.O. Box 3000, Boulder, CO 80307-3000, USA

SIMBAD Objects

Contents

Next Section Table of Contents

© European Southern Observatory (ESO) 1998

Online publication: June 18, 1998
helpdesk.link@springer.de