Resonant Heating of Ions by Parallel Propagating Alfvén Waves in Solar Coronal Holes

作     者：Tian-XiZhang Jing-XiuWang Chi-JieXiao 

作者机构：NationalAstronomicalObservatoriesChineseAcademyofSciencesBeijing100012／／CenterforSpacePlasmaandAeronomicResearchTheUniversityofAlabamainHuntsvilleHuntsvilleAL35899USA NationalAstronomicalObservatoriesChineseAcademyofSciencesBeijing100012 

出 版 物：《Chinese Journal of Astronomy and Astrophysics》 (中国天文和天体物理学报（英文版）)

年 卷 期：2005年第5卷第3期

页      面：285-294页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：Supported by the National Natural Science Foundation of China 

主　　题：acceleration of particles   plasmas   waves   solar wind   Sun: corona 

摘      要：Resonant heating of H, O+5, and Mg+9 by parallel propagating ion cyclotron Alfven waves in solar coronal holes at a heliocentric distance is studied using the heating rate derived from the quasilinear theory. It is shown that the particle-AlfVen-wave interaction is a significant microscopic process. The temperatures of the ions are rapidly increased up to the observed order in only microseconds, which implies that simply inserting the quasilinear heating rate into the fluid/MHD energy equation to calculate the radial dependence of ion temperatures may cause errors as the time scales do not match. Different species ions are heated by Alfven waves with a power law spectrum in approximately a mass order. To heat O+5 over Mg+9 as measured by the Ultraviolet Coronagraph Spectrometer (UVCS) in the solar coronal hole at a region ≥ 1.9.R, the energy density of Alfven waves with a frequency close to the O+5-cyclotron frequency must be at least double of that at the Mg+9-cyclotron frequency. With an appropriate wave-energy spectrum, the heating of H, O+5 and Mg+9 can be consistent with the UVCS measurements in solar coronal holes at a heliocentric distance.