On the Origin of Alfven Waves Required for Heating in Solar Coronal Holes

太阳日冕洞加热所需的阿尔文波的起源

• 批准号: 9119580
• 负责人: Zdzislaw Musielak
• 金额: $ 9万
• 依托单位: University of Alabama in Huntsville
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 1992
• 资助国家: 美国
• 起止时间: 1992-04-01 至 1994-09-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9119580&HistoricalAwards=false
• 关键词: Origin; Alfven; Waves; Required; Heating

The Earth is situated in a solar wind, whose origins are unclear. The source of this is "coronal holes". This study deals with this plasma source. The fact that Alfven waves may play a significant role in the energy balance in solar coronal holes has been known for many years. The traditional view has been that these waves are generated in the convectively unstable subphotospheric layers. Just very recently Parker (1991, Astrophys. J., 372, 719) and Moore et al. (1991, Astrophys. J., 376, in press) have suggested that these waves can be generated by small-scale magnetic fields assoicated with the network and presented some qualitative arguments to support this idea. Because there are also other mechanisms of Alfven wave generation operating in the solar atmosphere, more detailed calculations are needed to estimate which mechanism dominates in the excitation of these waves. The PI propose to calculate the wave energy spectra and energy fluxes for three different mechanisms of Alfven wave generation: (1) excitation of transverse waves on magnetic flux tubes by the subphotospheric convection, (2) generation of transverse tube waves by the photospheric granulation, and (3) excitation of Alfven waves by the network microflaring. To find out which mechanism is dominant in supplying the wave energy into solar coronal holes, the PI will compare all three obtained wave energy fluxes with total heat input required by observations. This study will be important in ongoing efforts to understand the principal energy sources for solar coronal holes and the basic physical processes responsible for creating the heliosphere, in which the Earth resides.

地球位于太阳风中，其起源尚不清楚。 其来源是“日冕洞”。 本研究涉及 这个等离子源 阿尔芬波可能在 在太阳冕洞的能量平衡中起着重要作用， 已经知道很多年了。 传统的观点是， 这些波产生于对流不稳定的 亚光球层 就在最近，帕克（1991年， 占星术。J.，372，719）和摩尔等人（1991，Astrophys. J.， 376，在出版）提出，这些波可以产生 通过与网络相关的小规模磁场， 提出了一些定性的论据来支持这一观点。 因为阿尔芬波的产生还有其他机制 在太阳大气中运行，更详细的计算是 需要估计哪种机制在激发中占主导地位， 这些波浪。 PI建议计算波浪能谱 阿尔芬波的三种不同机制的能量通量 产生：（1）磁通量上的横波激发 （2）太阳辐射的产生， 横向管波的光球颗粒，和（3） 通过网络微耀斑激发阿尔芬波。 找到 哪一种机制在将波能提供给 太阳日冕洞，PI将比较所有三个获得的波 能量通量与观测所需的总热输入。 这项研究将是重要的，在不断努力了解 太阳冕洞的主要能量来源， 基本的物理过程， 太阳系，地球居住的地方。