Abstract
Bu çalışmada, KIC7542091 sisteminin Kepler Uzay Teleskobu ile alınmış yüksek duyarlıklı fotometrik verileri kullanılarak çevrimsel aktivitenin yapısı ortaya konulmuştur.
Sistemin toplam 18 ayrı çeyrekte (quarter) alınmış ışık eğrileri dikkate alınarak maksimum ve minimum parlaklıkları ile bu parlaklıklar arasındaki farklar incelenmiş ve yaklaşık 150 gün dönemli çevrimsel değişimin bulunduğu gösterilmiştir. Bu değişimin, sistemin tayf türüyle (G1V; Frasca vd., 2016) uyumlu bir şekilde aktivite kaynaklı olacağı önerilmektedir. W UMa türü bir değişen olan bu sistemin fiziksel ve geometrik parametrelerine ilişkin çalışmalar hem Kepler Uzay Teleskobu, hem de TESS gözlemlerine dayalı olarak sürdürülmektedir.
References
- Borucki W., Koch D., Dunham E., Jenkins J., 1997, in Planets beyond the solar system and the next generation of space missions. p. 153
- Debosscher J., Blomme J., Aerts C., De Ridder J., 2011, Astronomy & Astrophysics, 529, A89
- Frasca A., ve diğ., 2016, Astronomy & Astrophysics, 594, A39
- Gilliland R. L., ve diğ., 2010, The Astrophysical Journal Letters, 713, L160
- Koch D. G., ve diğ., 2010, The Astrophysical Journal Letters, 713, L79
- Lenz P., Breger M., 2005, Communications in Asteroseismology, 146, 53
- Pigulski A., Pojmanski G., Pilecki B., Szczygiel D., 2009, arXiv preprint arXiv:0903.4921
- Press W. H., Teukolsky S. A., Vetterling W. T., Flannery B. P., 2007, Numerical recipes 3rd edition: The art of scientific computing. Cambridge university press
- Slawson R. W., ve diğ., 2011, The Astronomical Journal, 142, 160
- Tran K., Levine A., Rappaport S., Borkovits T., Csizmadia S., Kalomeni B., 2013, The Astrophysical Journal, 774, 81
- Zhang J., Qian S.-B., Wu Y., Zhou X., 2019, The Astrophysical Journal Supplement Series, 244, 43
Abstract
In this study, the cyclic structure of the activity is revealed by using high-precision photometric data of the KIC7542091 system taken with the Kepler Space Telescope.
Considering the light curves of the system taken in a total of 18 different quarters, the maximum and minimum brightnesses and the differences between these brightnesses were examined and it was shown that there was a cyclic variation with a period of about 150 days. It is suggested that this variaton is originated from activity which is corresponding with the spectral type of the system (G1V; Frasca et al. 2016). Studies on the physical and geometric parameters of this system, which is a W UMa type variable, are carried out based on both Kepler Space Telescope and TESS observations.
References
- Borucki W., Koch D., Dunham E., Jenkins J., 1997, in Planets beyond the solar system and the next generation of space missions. p. 153
- Debosscher J., Blomme J., Aerts C., De Ridder J., 2011, Astronomy & Astrophysics, 529, A89
- Frasca A., ve diğ., 2016, Astronomy & Astrophysics, 594, A39
- Gilliland R. L., ve diğ., 2010, The Astrophysical Journal Letters, 713, L160
- Koch D. G., ve diğ., 2010, The Astrophysical Journal Letters, 713, L79
- Lenz P., Breger M., 2005, Communications in Asteroseismology, 146, 53
- Pigulski A., Pojmanski G., Pilecki B., Szczygiel D., 2009, arXiv preprint arXiv:0903.4921
- Press W. H., Teukolsky S. A., Vetterling W. T., Flannery B. P., 2007, Numerical recipes 3rd edition: The art of scientific computing. Cambridge university press
- Slawson R. W., ve diğ., 2011, The Astronomical Journal, 142, 160
- Tran K., Levine A., Rappaport S., Borkovits T., Csizmadia S., Kalomeni B., 2013, The Astrophysical Journal, 774, 81
- Zhang J., Qian S.-B., Wu Y., Zhou X., 2019, The Astrophysical Journal Supplement Series, 244, 43
Details
| Primary Language | Turkish |
|---|---|
| Subjects | Astronomical Sciences (Other) |
| Journal Section | Articles |
| Authors | |
| Publication Date | June 30, 2023 |
| Submission Date | December 26, 2022 |
| Acceptance Date | June 14, 2023 |
| Published in Issue | Year 2023 Volume: 4 Issue: 1 |
TJAA is a publication of Turkish Astronomical Society (TAD).