臺師大雙星散斑觀測計畫
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2009
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Abstract
大氣擾動會使得我們觀測到的雙星影像產生變形，然而透過散斑干涉技術，我們可以去測量出雙星系統的角距和方向角。從2002開始，臺師大建立雙星系統的散斑干涉觀測技術。
商業用的CCD，DMK 31AF03是我們這次雙星系統的散斑干涉觀測技術所使用的CCD；由於C-14的主鏡會隨著望遠鏡移動時而變動，所以不適合作為雙星系統的散斑干涉觀測技術的工具。
在2009年的觀測計畫中，我們選定了24個雙星系統，而其中只有13個雙星系統被偵測出來，這些雙星的角距介在0.61到8角秒之間，主星的亮度介在1.93星等到5.64星等之間。
The binary image will be distorted by atmospheric turbulence, however the angular separation of a binary could be determined with speckle interferometry technology. The binary program with speckle interferometry at NTNU has been set up since 2002. The commercial CCD, DMK 31AF03 CCD, is suitable for the binary program with the method of speckle interferometry. Because C-14 is the telescope with a moving primary mirror, it is not suitable for speckle observations. There are 22 binaries chosen for our 2009 program, and the parameters of 13 binaries are determined. Their angular separations are between 0.61 ~ 8 arcsecs. The brightnesses of the primary stars fall between 1.93~5.64 mag.
The binary image will be distorted by atmospheric turbulence, however the angular separation of a binary could be determined with speckle interferometry technology. The binary program with speckle interferometry at NTNU has been set up since 2002. The commercial CCD, DMK 31AF03 CCD, is suitable for the binary program with the method of speckle interferometry. Because C-14 is the telescope with a moving primary mirror, it is not suitable for speckle observations. There are 22 binaries chosen for our 2009 program, and the parameters of 13 binaries are determined. Their angular separations are between 0.61 ~ 8 arcsecs. The brightnesses of the primary stars fall between 1.93~5.64 mag.
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雙星, 散斑觀測, binary, speckle interferometry