Period Change of the Contact Binary AH Tauri
New BVRI photometric observations of the contact binary AH Tau were performed with the 61 cm reflector and a 2K CCD camera at the Sobaeksan Optical Astronomy Observatory during seven nights from September to December, 2001. A total of 144 times of minima observed up to date, including three times of...
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| Format: | Article |
| Language: | English |
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The Korean Space Science Society
2004-12-01
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| Series: | Journal of Astronomy and Space Sciences |
| Subjects: | |
| Online Access: | http://ocean.kisti.re.kr/downfile/volume/kosss/OJOOBS/2004/v21n4/OJOOBS_2004_v21n4_283.pdf |
| _version_ | 1797333034087743488 |
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| author | Dongjoo Lee Chung-Uk Lee Jae Woo Lee Seung-Lee Kim Kyu-Dong Oh Chun-Hwey Kim |
| author_facet | Dongjoo Lee Chung-Uk Lee Jae Woo Lee Seung-Lee Kim Kyu-Dong Oh Chun-Hwey Kim |
| author_sort | Dongjoo Lee |
| collection | DOAJ |
| description | New BVRI photometric observations of the contact binary AH Tau were performed with the 61 cm reflector and a 2K CCD camera at the Sobaeksan Optical Astronomy Observatory during seven nights from September to December, 2001. A total of 144 times of minima observed up to date, including three times of minima obtained from our observation, were analyzed. It is found that the orbital period of AH Tau has varied in a cyclic way superposed on a secular period decrease. The rate of the secular period decrease is calculated to be 1^s.04 per century, implying that a mass of about 3.8 × 10-8 M⊙/yr from the more massive primary flows into the secondary if a conservative mass transfer is assumed. Assuming that the sinusoidal period variation is produced by a light-time effect due to an unseen third body, the resultant semi-amplitude, period, and eccentricity for the deduced light-time orbit are obtained as 35.4 years, 0.014 day and 0.52, respectively. The mass of the third-body is calculated as about 0.24 M⊙ when the third body is assumed to be coplanar with AH Tau system. |
| first_indexed | 2024-03-08T07:58:00Z |
| format | Article |
| id | doaj.art-ba88f333ccef41628bdce9ffbe337ad0 |
| institution | Directory Open Access Journal |
| issn | 2093-5587 2093-1409 |
| language | English |
| last_indexed | 2024-03-08T07:58:00Z |
| publishDate | 2004-12-01 |
| publisher | The Korean Space Science Society |
| record_format | Article |
| series | Journal of Astronomy and Space Sciences |
| spelling | doaj.art-ba88f333ccef41628bdce9ffbe337ad02024-02-02T13:23:22ZengThe Korean Space Science SocietyJournal of Astronomy and Space Sciences2093-55872093-14092004-12-0121428329410.5140/JASS.2004.21.4.283Period Change of the Contact Binary AH TauriDongjoo Lee0Chung-Uk Lee1Jae Woo Lee2Seung-Lee Kim3Kyu-Dong Oh4Chun-Hwey Kim5Korea Astronomy Observatory, Daejeon 305-348, KoreaKorea Astronomy Observatory, Daejeon 305-348, KoreaKorea Astronomy Observatory, Daejeon 305-348, KoreaKorea Astronomy Observatory, Daejeon 305-348, KoreaDepartment of Earth Science Education, Chonnam National University, Kwangju 500-757, KoreaDept. of Astronomy & Space Science, College of Natural Science and Institute for Basic Science Research, Chungbuk National University, Cheongju 361-763, KoreaNew BVRI photometric observations of the contact binary AH Tau were performed with the 61 cm reflector and a 2K CCD camera at the Sobaeksan Optical Astronomy Observatory during seven nights from September to December, 2001. A total of 144 times of minima observed up to date, including three times of minima obtained from our observation, were analyzed. It is found that the orbital period of AH Tau has varied in a cyclic way superposed on a secular period decrease. The rate of the secular period decrease is calculated to be 1^s.04 per century, implying that a mass of about 3.8 × 10-8 M⊙/yr from the more massive primary flows into the secondary if a conservative mass transfer is assumed. Assuming that the sinusoidal period variation is produced by a light-time effect due to an unseen third body, the resultant semi-amplitude, period, and eccentricity for the deduced light-time orbit are obtained as 35.4 years, 0.014 day and 0.52, respectively. The mass of the third-body is calculated as about 0.24 M⊙ when the third body is assumed to be coplanar with AH Tau system.http://ocean.kisti.re.kr/downfile/volume/kosss/OJOOBS/2004/v21n4/OJOOBS_2004_v21n4_283.pdfbinary starAH Tauperiod changethird body |
| spellingShingle | Dongjoo Lee Chung-Uk Lee Jae Woo Lee Seung-Lee Kim Kyu-Dong Oh Chun-Hwey Kim Period Change of the Contact Binary AH Tauri Journal of Astronomy and Space Sciences binary star AH Tau period change third body |
| title | Period Change of the Contact Binary AH Tauri |
| title_full | Period Change of the Contact Binary AH Tauri |
| title_fullStr | Period Change of the Contact Binary AH Tauri |
| title_full_unstemmed | Period Change of the Contact Binary AH Tauri |
| title_short | Period Change of the Contact Binary AH Tauri |
| title_sort | period change of the contact binary ah tauri |
| topic | binary star AH Tau period change third body |
| url | http://ocean.kisti.re.kr/downfile/volume/kosss/OJOOBS/2004/v21n4/OJOOBS_2004_v21n4_283.pdf |
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