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Study on the precise observations of stellar and circum-stellar phenomena with the optical and infrared interferometer

光学、红外干涉仪精确观测恒星及环星现象的研究

基本信息

批准号：
10304015
负责人：
SATO Koichi
金额：
$ 21.56万
依托单位：
National Astronomical Observatory
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (A)
财政年份：
1998
资助国家：
日本
起止时间：
1998 至 2001
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-10304015/
关键词：
optical interferometer high angular resolution stellar physics stellar diameter binary circumstellar matter

项目摘要

This research project (MIRA-I.2) is aimed to develop the optical and infrared interferometer for observing stars with the very high angular resolution. The term of this project is 4 years (Apr. 1998 - Mar. 2002).In 1998, interferometer optics, detectors, and control system were investigated, partly made and tested. These parts were built into the former interferometer system, MIRA-I.1, which consists of two coude telescopes (250 mm aperture, 4 m baseline). Fringes of several bright stars were detected with this system. In 1999, the coude telescopes were replaced with the new element telescopes of siderostat (300 mm flat mirror, the test system of 6 m baseline). The construction of the new observing houses for the regular system of MIRA-I.2 (30 m baseline) was begun along with the setup of the test baseline system of 6 m. In 2000, we made the construction and the setup of new observing houses, vacuum pipes for optical path, optical parts in the observing house, interferometer optics, fringe detectors, quadrant sensors for tip-tilt mirrors, and vacuum chamber for delay line in the interferometer laboratory. In 2001, the interferometer system of 6 m test baseline was completed. At the end of June, 2001, fringes of several bright stars were detected with this system. In August, after this success, we started the construction of the regujar system of 30 m baseline in full-scale. Test observations of bright stars were begun in October, 2001. However, we could not detect the star fringes until March, 2002 (the end of 2001 fiscal year).Making improvements and regulations of the system, we succeeded to detect the fringes of Vega with the regular MIRA-I.2 system of 30 m baseline, in June, 2002. We will complete this interferometer, which is worth observing the physical parameters, such as radius and mass of stars.

本研究计画（MIRA-I.2）的目的是发展一种光学及红外线干涉仪，以达到极高的角解析度来观测恒星。本计画为期四年（1998年4月至2002年3月），于1998年完成了干涉仪光学系统、探测器及控制系统的研究、部分制作与测试。这些部件被安装在以前的干涉仪系统MIRA-I.1中，该系统由两个Coude望远镜（250毫米口径，4米基线）组成。这个系统探测到了几颗明亮恒星的边缘。1999年，Coude望远镜被新的铁磁仪单元望远镜（300 mm平面镜，6 m基线的测试系统）所取代。随着6米测试基线系统的建立，沿着开始为MIRA-I.2常规系统（30米基线）建造新的观测室。2000年，我们在干涉仪实验室建造并安装了新的观测室、光路真空管、观测室光学部件、干涉仪光学系统、条纹探测器、倾斜镜的象限传感器和延迟线真空室。2001年完成了6 m试验基线的干涉仪系统。2001年6月底，用该系统探测到了几颗亮星的条纹。8月，在这一成功之后，我们开始全面建设30米基线的regujar系统。2001年10月开始对亮星进行测试观测。但直到2002年3月（2001财政年度末）才探测到织女星的星星条纹，经过对系统的改进和调整，于2002年6月用30 m基线的常规MIRA-I.2系统成功地探测到织女星的条纹。我们将完成这个干涉仪，这是值得观察的物理参数，如半径和质量的恒星。