针状体是太阳大气中普遍存在的小尺度喷流。近期观测表明，针状体中部分色球气体可被加热至过渡区乃至日冕温度。此外，针状体常伴有被理解为快扭曲波的横向摆动，所估计的能流足供冕洞内日冕加热所需。但由于相关研究的理论基础偏离针状体现实甚远，快扭曲波能否及怎样加热冕洞针状体中太阳大气这一问题还远未解决。本项目拟在磁流体力学框架内，利用解析、线性数值计算及全三维非线性模拟手段，计入时变针状体中可观的流动及针状体内外介质的纵向分层，系统讨论这些真实物理因素如何影响针状体中快扭曲波的能量输运、衰减、向小尺度结构的转换及相应耗散，从而定量评估快扭曲波对冕洞针状体内太阳大气的加热效率。项目成果将有助于理解冕洞区日冕能量供应问题，考虑到横波在软X线喷流、网络喷流等小尺度喷流中广泛存在，项目成果还将具有普遍的应用价值。

Spicules abound in the solar atmosphere. Recent observations indicate that part of the chromospheric material in spicules can be heated to transition region or even coronal temperatures. Furthermore, spicules often undergo transverse motions generally accepted to be fast kink waves, which carry energy fluxes sufficient to account for coronal heating in solar coronal holes. However, the available theoretical studies are generally based on assumptions far from reality. It therefore remains an open question as to whether and how fast kink waves can heat the materials in spicules in coronal holes. In the framework of Magnetohydrodynamics, we will examine, in a systematic manner, the propagation, damping, and dissipation of fast kink waves in realistic temporally varying, dynamic, and longitudinally structured spicules. This will be done with a synergetic approach combining analytical methods together with time-dependent linear and fully non-linear computations. We will quantitatively assess the heating rates due to fast kink waves and their observational consequences. The outcome of this project will help understand the energy supply to the corona in coronal holes, and will also be applicable to soft X-ray jets and network jets, which are prevalent on the Sun and often accompanied by cyclic transverse motions as well.