The Role of Type II Spicules in the Upper Solar Atmosphere

TL;DR

This study evaluates the hypothesis that type II spicules significantly contribute to the solar corona's hot plasma, finding that their contribution is minimal and supporting traditional coronal heating models.

Contribution

The paper provides observational evidence that limits the role of type II spicules in coronal plasma supply, favoring established coronal heating mechanisms.

Findings

Spicules contribute less than 8% of hot plasma in the corona.

Predicted spectral asymmetries from spicule models are much larger than observed.

Most hot emission originates from non-spicule strands explained by traditional heating models.

Abstract

We examine the suggestion that most of the hot plasma in the Sun's corona comes from type II spicule material that is heated as it is ejected from the chromosphere. This contrasts with the traditional view that the corona is filled via chromospheric evaporation that results from coronal heating. We explore the observational consequences of a hypothetical spicule dominated corona and conclude from the large discrepancy between predicted and actual observations that only a small fraction of the hot plasma can be supplied by spicules (<2% in active regions, <5% in the quiet Sun, and <8% in coronal holes). The red-blue asymmetries of EUV spectral lines and the ratio of lower transition region (LTR; T<0.1 MK) to coronal emission measures are both predicted to be 2 orders of magnitude larger than observed. Furthermore, hot spicule material would cool dramatically by adiabatic expansion as it rises into the corona, so substantial coronal heating would be needed to maintain the high temperatures that are seen at all altitudes. We suggest that the corona contains a mixture of thin strands, some of which are populated by spicule injections, but most of which are not. A majority of the observed hot emission originates in non-spicule strands and is explained by traditional coronal heating models. However, since these models predict far too little emission from the LTR, most of this emission comes from the bulk of the spicule material that is only weakly heated and visible in He II (304 A) as it falls back to the surface.