A Research about the locations of Jupiter's decametric sources by VLBI

VLBI对木星十米源位置的研究

• 批准号: 06640573
• 负责人: IMAI Kazumasa
• 金额: $ 1.28万
• 依托单位: Kochi National College of Technology
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (C)
• 财政年份: 1995
• 资助国家: 日本
• 起止时间: 1995 至 1996
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-06640573/
• 关键词: Jupiter; Radio Emissions; Decametric wave; VLBI; Polarization

The investigation of Jupiter's decameter-wavelength radio source locations and emission beam structure is very important for the study of the emission mechanism (Carr and Desch, 1976 ; Carr et al., 1983). Jupiter's rediation occurring during the so-called Io-B and Io-A storms is right-hand (RH) circularly or elliptically polarized. The Io-C storms, however, are often left-hand (LH) circularly polarized when observed in the vicinity of 18 MHz. Often a storm of long duration will begin in the Io-A region of central meridian longitude (CML) and end in the Io-C region, in which case it is not uncommon for the polarization sense to fluctuate back and forth between RH and LH in the transition region. It is generally believed that the Io-B and Io-A radiations are emitted in the extraordinary (X) mode, from within successive Io-energized flux tubes at the altitudes above the cloud-tops at which the wave frequency is only slightly higher than the electron gyrofrequency.Since it is known that the field lines of Jupiter's nearly-dipolar magnetic field are directed from the northern to the southern Jovigraphic polar regions, it follows that the RH polarized Io-B and Io-A emissions come from near the northern rather than the southern foot of the Io-energized flux tube. The question is where do the LH polarized Io-C emissions come from? With our dual-polarization interferometer we expect to be able to measure the angular separation of the sources of the LH polarized and RH polarized bursts that occur within a few time seconds of each other with sufficient accuracy to determine whether they were located in the same or in opposite polar hemispheres.

对木星的dec仪波长无线电源位置和发射光束结构的研究对于研究发射机理非常重要（Carr and Desch，1976; Carr等，1983）。木星在所谓的IO-B和IO-A风暴中发生的木星重新次数是右（RH）循环或椭圆极化的。然而，当在18 MHz附近观察到IO-C风暴通常是左手（LH）圆形极化。通常持续时间的风暴通常会在中部子午线经度（CML）的IO-A地区开始，并在IO-C地区结束，在这种情况下，极化意义在RH和LH之间来回波动并不少见。在过渡区域。通常认为，IO-B和IO-A辐射以非凡的（x）模式发射，从连续的IO富集的通量管内部的高度上方的云端频率仅高于波频率略高于云端的高度，众所周知，木星几乎向二色磁场的田间线是从北部到南部的jovigraphic极地区域的，因此，RH Pallerized IO-B和IO-A的排放来自北部附近而不是富含IO的通量管的南部脚。问题是LH两极分化的IO-C排放来自哪里？使用我们的双偏振干涉仪，我们希望能够测量在几秒钟内彼此之间发生的LH极化和RH偏振爆发源的角度分离，以确定它们是否位于同一还是位于相同或在相对的极半球。

项目成果

Kazumasa Imai: "Observations of Jupiters Decametric Radio Sources by the Dual-Polarization Interferometer" Proceedings of Eights International Symposium on Solar Terrestial Physics. 49-49 (1994)

Kazumasa Imai：“双偏振干涉仪对木星十度射电源的观测”八人国际日地物理学研讨会论文集。

Kazumasa Imai, T.D.Carr^*, F.Reyes^*, Haruyori Matsuura^*: "Observations of Jupiter's Decametric Radio Sources by the Dudal-Polarization Interferometer" Proceedings of Eighth International Symposium on Solar Terrestrial Physics held at Sendai. 49 (1994)

Kazumasa Imai、T.D.Carr^*、F.Reyes^*、Haruyori Matsuura^*：“双偏振干涉仪对木星十米射电源的观测”在仙台举行的第八届国际日地物理学研讨会论文集。

今井一雅: "木星電波源のビーム構造" 地球惑星科学関連学会1995年合同大会予稿集. 262-262 (1995)

Kazumasa Imai：“木星射电源的光束结构”1995 年地球与行星科学相关学会联合会议记录 262-262 (1995)。

今井一雅: "UF50マイル干渉計による木星電波源の観測" 地球惑星科学関連学会1994年合同大会予稿集. 543-543 (1994)

Kazumasa Imai：“使用 UF50 英里干涉仪观测木星的射电源”1994 年地球与行星科学协会联合会议记录 543-543 (1994)。

今井一雅 他三名: "UF50マイル干渉計による木星電波源の観測" 地球惑星科学関連学会1994年合同大会予稿集. 543-543 (1994)

Kazumasa Imai 和其他三人：“使用 UF 50 英里干涉仪观测木星的无线电源”1994 年地球与行星科学协会联合会议论文集 543-543 (1994)。