Study of Planetary Magnetospheres Using Infrared / Radio Data

使用红外/无线电数据研究行星磁层

• 批准号: 11694097
• 负责人: SATOH Takehiko
• 金额: $ 2.05万
• 依托单位: Science University of Tokyo
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (B).
• 财政年份: 1999
• 资助国家: 日本
• 起止时间: 1999 至 2000
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-11694097/
• 关键词: Jupiter; Magnetosphere; Infrared; Radio; Aurora; Satellite; Plasma

A comprehensive planning meeting was held in August 1999 with all investigators. Discussed the Jovian magnetospheric phenomena observed in the infrared/radio wavelengths, the data, and future "coordinated" observing plans. Observations in the infraed (Satoh and Connerney) and in the radio (Imai, Reyes, and Carr) were made accordingly.By analyzing these data, we've obtained extraordinary details of Jupiter's northern aurora, and very precise positions of the IFT footprints. Imai's modulation lane model has been proven to be very powerful determining precise location of Jovian decametric radio source. Our success owes much on the tilt of Jupiter's rotation axis (3 degrees max) during 1999-2000, justifying our choise of research period.The results have been published in several papers, as well as many meeting presentations, such as the one at the American Geophysical Union (Satoh, Dec 1999), the Royal Society (Connerney, Feb 2000), European Geophysical Society (Imai, Apr 2000), etc.Our future plan is : (1) to improve the VIP4 jovimagnetic field model, (2) to develop the precipitation flux model for the aurora, (3) to refine the modulation lane model and apply it to many data, and (4) to combine infrared/ultraviolet/radio data to further understand the fundamentals in the magnetospheric physics.

1999年8月与所有调查员举行了一次全面规划会议。讨论了在红外线/无线电波段观测到的木星磁层现象、数据和未来“协调”观测计划。据此，我们进行了红外线（Satoh和Connerney）和无线电（Imai，Reyes和卡尔）观测，通过分析这些数据，我们获得了木星北方极光的非凡细节，以及IFT足迹的非常精确的位置。Imai的调制通道模型已被证明是非常强大的确定木星十米波射电源的精确位置。我们的成功很大程度上归功于木星自转轴的倾斜研究结果已发表在多篇论文和许多会议报告中，如美国地球物理联合会的报告（Satoh，1999年12月），皇家学会（Connerney，2000年2月），欧洲地球物理学会（今井，2000年4月）等。我们未来的计划是：（1）改进VIP 4木星磁场模型;（2）发展极光降水通量模型;（3）改进调制通道模型并将其应用于许多数据，以及（4）结合联合收割机红外/紫外/无线电数据以进一步理解磁层物理学的基本原理。

项目成果

J.E.P.Connerney,and T.Satoh: "The H^+_3 Ion:A Remote Diagnostic of the Jovian Magnetosphere"Philosophical Transaction of the Royal Society. (in press). (2000)

J.E.P.Connerney 和 T.Satoh：“H^_3 离子：木星磁层的远程诊断”英国皇家学会哲学汇刊。

T.Satoh, and J.E.P.Connerney: "Spatial and Temporal Variations of Jupiter's H^+_3 Emission Deduced from Image Analysis"Geophysical Research Letters. 26. 1789-1792 (1999)

T.Satoh 和 J.E.P.Connerney：“从图像分析推导出木星 H^ _3 发射的空间和时间变化”地球物理研究快报。

J.E.P.Connerney, and T.Satoh: "The H3+ ion : A remote diagnostic of the Jovian magnetosphere"Philosophical Transactions of the Royal Society. 358. 2471-2483 (2000)

J.E.P.Connerney 和 T.Satoh：“H3 离子：木星磁层的远程诊断”英国皇家学会哲学汇刊。

T.Satoh, S.Itoh, K.Kawabata, T.Tenma, and T.Akabane: "A universal phase function for Jovian clouds from the visible to near-IR wavelength region : I.Zone phase function"Publications of the Astronomical Society of Japan. 52. 363-374 (2000)

T.Satoh、S.Itoh、K.Kawabata、T.Tenma 和 T.Akabane：“从可见光到近红外波长区域的木星云的通用相位函数：I.Zone 相位函数”天文学会出版物

T.Satoh, and J.E.P.Connerney: "Jupiter's H^+_3 Emissions Viewed in Corrected Jovimagnetic Coordinates"Icarus. 141. 236-252 (1999)

T.Satoh 和 J.E.P.Connerney：“木星的 H^ _3 在校正的木磁坐标中观察到的发射”伊卡洛斯。