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Investigation of mass flows in the transition region and corona in a three-dimensional numerical model approach

机译:三维数值模型方法研究过渡区和电晕中的质量流

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Context. The origin of solar transition region redshifts is not completely understood. Current research is addressing this issue by investigating three-dimensional magneto-hydrodynamic models that extend from the photosphere to the?corona. Aims. By studying the average properties of emission line profiles synthesized from the simulation runs and comparing them to observations with present-day instrumentation, we investigate the origin of mass flows in the solar transition region and corona. Methods. Doppler shifts were determined from the emission line profiles of various extreme-ultraviolet emission lines formed in the range of T?=?104?106?K. Plasma velocities and mass flows were investigated for their contribution to the observed Doppler shifts in the model. In?particular, the?temporal evolution of plasma flows along the magnetic field lines was analyzed. Results. Comparing observed vs. modeled Doppler shifts shows a good correlation in the temperature range log?(T/[K])?= 4.5?5.7, which is the basis of our search for the origin of the line shifts. The vertical velocity obtained when weighting the velocity by the density squared is shown to be almost identical to the corresponding Doppler shift. Therefore, a?direct comparison between Doppler shifts and the model parameters is allowed. A?simple interpretation of Doppler shifts in terms of mass flux leads to overestimating the mass flux. Upflows in the model appear in the form of cool pockets of gas that heat up slowly as they rise. Their low temperature means that these pockets are not observed as blueshifts in the transition region and coronal lines. For?a?set of magnetic field lines, two?different flow phases could be identified. The coronal part of the field line is intermittently connected to subjacent layers of either strong or weak heating, leading either to mass flows into the loop (observed?as a blueshift) or to the draining of the loop (observed as a?redshift).
机译:上下文。太阳过渡区红移的起源尚不完全清楚。当前的研究通过研究从光球延伸到电晕的三维磁流体动力学模型来解决这个问题。目的通过研究由模拟运行合成的发射谱线轮廓的平均特性,并将其与当前仪器的观测值进行比较,我们研究了太阳过渡区和日冕中质量流的起源。方法。从在T 1 =≤104≤106≤K范围内形成的各种极紫外发射线的发射线轮廓确定多普勒频移。研究血浆速度和质量流量对模型中观察到的多普勒频移的影响。特别地,分析了沿磁场线的等离子体流的时间演变。结果。比较观察到的多普勒频移与模型多普勒频移,在温度范围log?(T / [K])?= 4.5?5.7时显示出良好的相关性,这是我们寻找线偏移起点的基础。当通过密度平方加权速度时获得的垂直速度显示为几乎与相应的多普勒频移相同。因此,允许在多普勒频移和模型参数之间进行直接比较。根据质量通量对多普勒频移的简单解释会导致高估质量通量。模型中的上升流以冷气袋的形式出现,随着上升,其加热缓慢。它们的低温意味着在过渡区域和冠状线中没有观察到这些袋的蓝移。对于一组磁场线,可以确定两个不同的流相。磁力线的冠状部分间歇性地与强热或弱热的下层相连,从而导致质量流入环路(观察为蓝移)或引流环路(观察为红移)。

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