為推動變星觀測風氣與研究水準，建立天文觀測網路學習平台，期望未來能建立台灣變星觀測網。國立臺灣師範大學地球科學系和臺北市立天文科學教育館特別舉辦此次研討會，會中演講者將會講述變星觀測和資料分析，並發表其觀測結果。歡迎對變星觀測與光度資料分析有興趣者來參與研討。
講題和演講者如下：
The photometric calibration of DSLR using Lyrae and Big Dipper
field - 傅學海
Program of VS observation for high school students - 黃晟庭
The V photometry of BP Peg - 李奇欣
Find the variables in the field of M35 - 黃冠夫
CCD變星觀測 - 林宏欽
DY Peg的光度研究 - 王為
時間：2005年10月29日上午9時至12時 (時程表)
地點：臺北市立天文科學教育館三樓第二演講室
報名方式：採網路報名，以20名為限（免費）。
聯絡電話：(02) 2831-4551 分機303
註：本計畫為國科會科教處的「頂尖創新計畫：從數位宇宙推廣台灣的天文教育—數位天文台」計畫（e-Observatory）下的活動。
演講摘要
The photometric calibration of DSLR using Lyrae
and Big Dipper field
Hsieh-Hai Fu (傅學海)
The Department of Earth Sciences, NTNU
Abstract
T effective magnitude of DSLC is an important parameter for the variable
stars observation. Beta Lyr, Algol and delta Cep are chosen for DSLC and
the fields
of these targets are suitable for magnitude calibration. The standard error
of magnitude is about 0.1-0.3, and under 0.1 is expected. The best accuracy
of stellar magnitude with naked eye of an experience observer is about 0.1,
and the digitized images with DSLC are encouraged for variable stars observation
if the magnitude accuracy is about or under 0.1. (全文)
Program of VS Observation for High School Students
Shang-Ting Huang (黃晟庭)
Department of Earth Sciences, NTNU
Abstract
The program of VS Observation for High School Students has been holding at
NTNU in the past two years. There are high-school students selected from
the program, astronomy workshop at Taipei Nan-Kang high school. After they
were
familiar with the manipulation of the remote telescope at NTNU campus, they
can control the telescope at their home via ADSL. These students increase
their knowledge of astronomy, astrophysics, and mathematics; improve their
ability
on computer and system control of telescopes in our education programs in
terms of observing the variable stars. (全文)
The V Photometry of BP Peg
Chi-Shin Lee (李奇欣)
Department of Earth Sciences, NTNU
Abstract
BP Peg is a delta Scuti star with a period of 0.10954357 days (Kim, et al., 1989).
The light curve shows two pulsation modes. The observation was made at NTNU
campus during October 08 - 15, 2005. The data were obtained using RC 16 telescope
equipped with SBIG ST-10XME CCD plus Johnson V filter for seven nights. The
model of light
curve of BP Peg will be analyzed. (全文)
Find the variables in the field of M35
Kuan-Fu Huang (黃冠夫)
Department of Earth Sciences, NTNU
Abstract
There are few suspected variable stars found in the M35 field, using RC-16”
telescope on campus of NTNU and 63-cm telescope of NTU observatory on Mt. Phoenix.
The BV CCD images of three epoch, Nov 8, 11, and Dec 14, 2004 are used in
searching for variable stars. The standard error of V magnitude is about 0.05
for RC-16” and 0.07 for 63-cm telescope. The stars, whose magnitude variation
is more than 3σ, are thought to be the suspected variable stars.
CCD變星觀測
Hung-Chin Lin (林宏欽)
Lulin Observatory, Institute of Astronomy, NCU
摘要
隨著CCD相機的普及及相關軟硬體的發展，利用CCD進行變星觀測已不是遙不可及的事。本
次講題將介紹CCD變星觀測所需的器材準備、觀測方法及資料處理、週期分析等工具，供有志
於變星觀測者參考。 (全文)
DY Peg的光度研究
Wei Wang (王為)、岑易臻、蕭旭清、羅卓延駿
麗山High School
摘要
本研究的主要任務是觀測變星的光度變化。在研究初期我們首先做的是資料的蒐集，對變星的種類、光度變化的原因以及周期的特殊變化作全面性的了解，其次根據GCVS中尋找適合觀測的目標DY
Peg，因為受到天氣影響，直至八月下旬才開始進行影像拍攝工作。主要觀測器材包含天文望遠鏡FS-152、冷卻CCD ST-10、道儀SBIG GT1100ME。整個攝影時間約四小時，藉由MaxIm
DL軟體控制CCD，使用V濾鏡共拍攝約100張星場影像，每張曝光100秒。另外同時拍攝Dark、Bias及Flat以做雜訊修正，最後求得DY Peg的光變曲線。
研究結果得知DY Peg的光變週期為0.07243天，光度最大為9.978，最小為10.543，其光變幅度為0.565星等。而光度變化是略為急升緩降，其光變曲線與SXPHE型及DSCT型的變星極為相似。
整個研究製作的過程中，我們學到了許多有關天文的學問，對天文觀測器材的使用也有了深入的了解，這些多對我們未來繼續對天文方面發展有很大的幫助。 (全文)