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首页> 外文期刊>Plasma physics reports >Evolution of the Solar Wind Speed with Heliocentric Distance and Solar Cycle. Surprises from Ulysses and Unexpectedness from Observations of the Solar Corona
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Evolution of the Solar Wind Speed with Heliocentric Distance and Solar Cycle. Surprises from Ulysses and Unexpectedness from Observations of the Solar Corona

机译：天线距离和太阳循环太阳风速的演变。 从太阳能电晕的观察结果中，尤利西斯和意外意外意外的惊喜

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An extensive analysis of Ulysses observations of the solar wind speed V from 1990 to 2008 is undertaken. It is shown that the evolution of V with heliocentric distance r depends substantially on both the heliolatitude and the solar activity cycle. Deviations from the predicted Parker's profile of V(r) are so considerable that cannot be explained by a scarcity of measurements or other technical effects. In particular, the expected smooth growth of the solar wind speed with r is typical only for the solar activity maximum and for low heliolatitudes (lower than +/- 40 degrees), while at high latitudes, there are two V(r) branches: growing and falling. In the solar activity maximum, V increases toward the solar pole in the North hemisphere only; however, in the South hemisphere, it decreases with heliolatitude. In the minimum of solar activity, the profile of V(r) at low heliolatitudes has a local minimum between 2 and 5 AU. This result is confirmed by the corresponding data from other spacecraft (Voyager 1 and Pioneer 10). Unexpected spatial variations in V at low heliolatitudes can be explained by the impact of coronal hole flows on the V(r) profile since the flows incline to the ecliptic plane. To reproduce the impact of spatial variations of V in the polar corona on the behavior of V at low heliolatitudes, a stationary one-fluid ideal MHD-model is developed with account of recent results on imagery of the solar wind speed in the corona up to 5.5 solar radii obtained on the basis of combined observations from SOHO/UVCS, LASCO, and Mauna Loa.
机译：对1990年至2008年的太阳风速V的尤利索观察进行了广泛的分析。结果表明，具有皮层距离R的v的演化基本上取决于热性和太阳能循环。从预测的帕克的v（r）的偏差是如此可观，这不能通过测量或其他技术效果的稀缺来解释。特别是，对于太阳能的预期平滑增长，R是典型的，仅适用于太阳能活动最大值和低热量（低于+/- 40度），而在高纬度地区，有两种V（R）分支：生长和跌倒。在太阳能活动最大值中，V仅增加了北半球的太阳能杆;然而，在南半球，它随着HelioStity减少。在太阳能活性的最小值中，低热溶解的V（R）的轮廓具有2至5AU之间的局部最小值。该结果由来自其他航天器（Voyager 1和Pioneer 10）的相应数据确认。由于流量倾斜到黄光平面，因此可以通过冠状孔流量的影响来解释低热孔的v的意外空间变化。为了在低直升机处的v的行为中再现V在极性电晕中的空间变化的影响，通过近期结果的太阳风速的成果来制定静止的单流体理想MHD模型5.5基于Soho / UVCS，Lasco和Mauna Loa的组合观察获得的太阳能线索。

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  • 来源
    《Plasma physics reports》 |2018年第9期|共14页
  • 作者

    Khabarova O. V.; Obridko V. N.; Kislov R. A.; Malova H. V.; Bemporad A.; Zelenyi L. M.; Kuznetsov V. D.; Kharshiladze A. F.;

  • 作者单位

    Russian Acad Sci Pushkov Inst Terr Magnetism Ionosphere &

    Radio Wa Moscow 108840 Russia;

    Russian Acad Sci Pushkov Inst Terr Magnetism Ionosphere &

    Radio Wa Moscow 108840 Russia;

    Russian Acad Sci Pushkov Inst Terr Magnetism Ionosphere &

    Radio Wa Moscow 108840 Russia;

    Russian Acad Sci Space Res Inst Moscow 117997 Russia;

    Osservatorio Astrofis Torino Ist Nazl Astrofis INAF I-10025 Turin Italy;

    Russian Acad Sci Space Res Inst Moscow 117997 Russia;

    Russian Acad Sci Pushkov Inst Terr Magnetism Ionosphere &

    Radio Wa Moscow 108840 Russia;

    Russian Acad Sci Pushkov Inst Terr Magnetism Ionosphere &

    Radio Wa Moscow 108840 Russia;

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  • 正文语种 eng
  • 中图分类 等离子体物理学;
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  • 入库时间 2022-08-20 06:25:55

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