Design study of the heliospheric imager

对一种新的成像系统的研究，以用于透视图（三维成像仪）和相关研究已经完成。（1）在第一年，我们设计了一个Heliospheric Imager。Very large effective area at least 3000 m-D12-D1 and reducing urban noise about 30 dB are for observe weak radio sources。因为这些原因。一个相位阵列天线环绕着金属围栏，高度为10米，用于三维成像仪。Thus we designed a phased array which consists of 16384/2-dipole elements （256 E-W）x64（N-S），3500 m-D12-D1。天线的敏感性预计将成为0.2 Jy将是我们实验室中当前IPS网络中最高的一个。各种部分是作为双极元件、一个schpertop balun和连接器正在开发和测试的电气性能。特别是，这些是为削减成本而设计的。我们成功地使用了一个低ohmic-loss （-0.02 dB）连接器。而且还发现了一种合适的电缆（MFH-8AC），它具有足够的强度和低速度因素。在第二年，我们建造了一个小相位阵列天线（16（E-W）x8（N-S），32米D12 D1来检查我们的设计。天线的撞击可以测量到大约170Ω，以设计计算的方式同意。太阳和QSO（3C 273、3C 405）观察到波束大小、系统温度和海拔区域，它们为6.5度（FWHP）、290 K和17米D12米D1相应地。这些价值观也是用计算的。在包容性中，设计可以应用于空间图像。（2）相关研究起源紧凑，速度非常慢，太阳风和传播的行星间干扰测量了IPS在这两年内研究了。这些分析技术将被应用到新的观测中，并将其应用到三维图像中。我们希望，新的数据将为我们提供对太阳圈中动态现象的更进一步的见解。

Research of a new instrument for imaging heliosphere (heliospheric imager) and related studies have been done.(1) Heliospheric ImagerIn the first year, we designed the heliospheric imager. Very large effective area at least 3000mィイD12ィエD1 and reducing urban noise about 30dB are required to observe weak radio sources. For these reasons. a phase array antenna surrounded by metallic-fence with 10m height was adopted for the heliospheric imager. Thus we designed a phased array which consists of 16384 λ/2-dipole elements (256E-W) x 64(N-S), 3500mィイD12ィエD1). The sensitivity of the antenna is expected to be 0.2 Jy which will be the highest one among those of the current IPS network in our laboratory.Various parts such as a dipole element, a schpertop balun and connectors are developed and tested electric performance. Especially these are designed for mass production to cut down the cost. We success to develop a low ohmic-loss (-0.02dB) connector which can be used in the heliospheric imager. And also suitable cable (MFH-8AC) was found which have enough strength and low velocity factor.In the second year, we built a small phased array antenna (16(E-W) x 8(N-S), 32mィイD12ィエD1 to check our design. The antenna impedance is measured to be about 170Ω which well agrees with design calculation. The Sun and QSOs (3C273, 3C405) were observed to measure beam size, system temperature and aperture area, and they are 6.5 degree (FWHP), 290 K and 17mィイD12ィエD1 respectively. These values also agree with calculated ones. In conclusion, the design can be applied to the heliospheric imager.(2) Related StudiesOrigin compact very low speed solar wind and propagation of interplanetary disturbances measured with IPS were studied in these two years. These analysis techniques will be applied to new observations with the heliospheric imager. We expect that the new data will provide us further insights of dynamical phenomena in heliosphere.