Heating in coronal funnels by ion cyclotron waves

Xing Li*

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

16 Citations (SciVal)

Abstract

Plasma heating by ion cyclotron waves in rapidly expanding flow tubes in the transition region, referred to as coronal funnels, is investigated in a three-fluid plasma consisting of protons, electrons, and a-particles. Ion - cyclotron waves are able to heat the plasma from 6 × 104 to 106 K over a distance range of 104 km by directly heating a-particles. Although only a-particles dissipate the waves, the strong Coulomb coupling between aparticles and protons and between protons and electrons makes it possible for protons and electrons to be heated also to more than 10 6 K. However, owing to the extreme heating of the α-particles, the particles are not in thermal equilibrium: α-particles can be much hotter and faster than protons. Beyond 1.02Rs, the particles return to thermal equilibrium when the electrons reach about 106 K, which is canonically defined as the base of the corona. These results lead to the following implications: (1) If spectral lines formed at Te < 1066 are observed at different heights, the inferred outflow velocities may vary by a factor of 5-6. (2) If minor ions are indeed much faster than protons and electrons at Te < 106 K, one cannot reliably determine the bulk outflow velocity of the solar wind in that region by using minor ion outflow velocities.

Original languageEnglish
Pages (from-to)L67-L70
JournalAstrophysical Journal
Volume571
Issue number1 II
DOIs
Publication statusPublished - 20 May 2002

Keywords

  • Solar wind
  • Sun: corona
  • Sun: transition region

Fingerprint

Dive into the research topics of 'Heating in coronal funnels by ion cyclotron waves'. Together they form a unique fingerprint.

Cite this