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首页> 外文期刊>Journal of Geophysical Research. Biogeosciences >An empirically-driven global MHD model of the solar corona and inner heliosphere
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An empirically-driven global MHD model of the solar corona and inner heliosphere

机译：由太阳驱动的日冕和内部太阳圈的经验驱动的全球MHD模型

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In this study we describe a three-dimensional MHD model of the solar corona and heliosphere. We split the modeling region into two distinct parts: the solar corona (1 solar radius, R-S, to 30 R-S) and the inner heliosphere (30 Rs to 5 AU). This combined model is driven solely by the observed line-of-sight photospheric magnetic field and call thus provide a realistic global picture of the corona and heliosphere for specific time periods of interest. We use the model to illustrate heliospheric structure during three different phases of the solar cycle: (1) Carrington rotation (CR) 1913 (August 22, 1996, to September 18, 1996), which occurred near solar minimum and overlapped the "Whole Sun Month'' campaign; (2) CR 1892 (January 27, 1995, to February 23, 1995), which occurred during the declining phase of cycle 22 and coincided with the so-called "Ulysses rapid latitude scan"; and (3) CR 1947 (March 7, 1999, to April 4, 1999), which occurred approximately 15 months before the predicted maximum of solar cycle 23. We compare Ulysses and Wind observations with the simulation for CR 1913 and compare Ulysses observations during its traversal from pole to pole with CR 1892. We find that the simulations reproduce the overall large-scale features of the observations. We use the near-solar-maximum results to speculate on the structure of the high-latitude solar wind that Ulysses will encounter during its traversal of the southern and northern solar poles in 2000 and 2001, respectively. In particular, the results suggest that because of the presence of equatorial coronal holes the ordered pattern of corotating interaction region tilts and their associated shocks, which was observed during Ulysses' initial southward excursion in 1992, will likely disappear completely as Ulysses moves toward the south pole. We anticipate that Ulysses will encounter fast streams but will not remain within them fur more than a fraction of a solar rotaton. Finally, the simulations suggest that crossings of the heliospheric cm rent sheet will persist up to at least similar to 70 degrees heliographic latitude. [References: 40]
机译：在这项研究中，我们描述了太阳日冕和日光层的三维MHD模型。我们将建模区域分为两个不同的部分：太阳日冕（1个太阳半径，R-S，至30 R-S）和内部太阳圈（30 Rs至5 AU）。该组合模型仅由观察到的视线光球磁场驱动，因此可以在特定的特定时间段内提供有关电晕和日光层的真实全局图像。我们使用该模型来说明太阳周期三个不同阶段的日球结构：（1）卡林顿旋转（CR）1913（1996年8月22日至1996年9月18日），发生在太阳最小附近，与“全太阳”重叠月”广告系列;（2）CR 1892（1995年1月27日至1995年2月23日），发生在周期22的下降阶段，与所谓的“尤利西斯快速纬度扫描”同时进行;以及（3） CR 1947（1999年3月7日至1999年4月4日），发生在太阳周期23的预计最大值之前约15个月。我们将Ulysses和Wind观测值与CR 1913的模拟进行了比较，并将Ulysses观测值从极点横穿时进行了比较。到CR 1892年的极点。我们发现模拟重现了观测的整体大规模特征，我们使用近太阳极大值的结果推测了尤利西斯在穿越过程中会遇到的高纬度太阳风的结构。南部和北部的在2000年和2001年分别有n个太阳极。特别是，这些结果表明，由于存在赤道冠状孔，相互作用的相互作用区域倾斜的有序模式及其相关的震荡（在1992年尤利西斯最初向南偏移期间观察到）可能会随着尤利西斯向南移动而完全消失。极。我们预计，尤利西斯将遇到快速流，但不会停留在它们中超过太阳旋转子的一小部分。最后，模拟表明，日球厘米租片的穿越将持续到至少类似于70度的纬度。 [参考：40]

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