On the Generation of Flux-Tube Waves in Stellar Convection Zones. IV. Longitudinal Wave Energy Spectra and Fluxes for Stars with Nonsolar Metallicities

Z. E. Musielak; R. Rosner; P. Ulmschneider

摘要

In the previous papers of this series, we developed an analytical method describing the generation of longitudinal tube waves in stellar convection zones and used it to compute the wave energy spectra and fluxes for late-type stars with the solar metal abundance (Population I). We now extend these calculations to Population II stars with effective temperatures ranging from Teff = 2500 to 10,000 K, gravities log g = 3-5, and with three different metal abundances: 1/10, 1/100, and 1/1000 of solar metallicity. The obtained results are valid for a single magnetic flux, and they show that the effects of metallicity are important only for cool stars with Teff 6000 K and that the amount of the generated wave energy decreases roughly by an order of magnitude for every decrease of the metallicity by an order of magnitude. The maximum wave energy flux generated in Population II stars is 7 × 108 ergs cm-2 s-1, and it is practically the same for stars of different gravities and metallicities. The computed spectra and fluxes can be used to construct theoretical models of magnetic regions in chromospheres of Population II stars.

机译：在本系列的前几篇论文中，我们开发了一种分析方法，该方法描述了恒星对流区中的纵向管波的产生，并用它来计算具有太阳金属丰度的后型恒星的波能谱和通量（种群I）。现在，我们将这些计算扩展到有效温度范围从Teff = 2500到10,000 K，重力log g = 3-5以及具有三种不同金属丰度的II类恒星：太阳的1 / 10、1 / 100和1/1000金属性。所获得的结果对于单个磁通量是有效的，并且它们表明，金属性的影响仅对Teff <6000 K的冷星很重要，并且每减小1埃，所产生的波能的数量大约减少一个数量级。金属性一个数量级。在种群II恒星中产生的最大波能通量为7×108 ergs cm-2 s-1，对于不同重力和金属性的恒星，实际上是相同的。计算出的光谱和通量可用于构建种群II星色球中磁区的理论模型。

On the Generation of Flux-Tube Waves in Stellar Convection Zones. IV. Longitudinal Wave Energy Spectra and Fluxes for Stars with Nonsolar Metallicities

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