Modeling of Two Low-amplitude Radially Pulsating δ Scuti Stars: KIC 12602250 and KIC 5768203
In this research, we conducted systematic photometric, spectroscopic, and theoretical modeling analyses of two δ Scuti stars—KIC 12602250 and KIC 5768203—that pulsate only in radial modes. We collected their relevant photometric and spectroscopic parameters from multiple catalogs and estimated the a...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/add406 |
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| author | Shuguo Ma A-Li Luo Peng Wei Chenglong Lv Ming Yang Fang Zuo Yingzhen Cui Shuo Li Gang Meng Wen Hou Yuji He Yinbi Li Zhongyang Liu Xiao-Xiao Ma Jun-Chao Liang Fei Dang Daoye Yang Ali Esamdin Hao Zeng Cai-Xia Qu |
| author_facet | Shuguo Ma A-Li Luo Peng Wei Chenglong Lv Ming Yang Fang Zuo Yingzhen Cui Shuo Li Gang Meng Wen Hou Yuji He Yinbi Li Zhongyang Liu Xiao-Xiao Ma Jun-Chao Liang Fei Dang Daoye Yang Ali Esamdin Hao Zeng Cai-Xia Qu |
| author_sort | Shuguo Ma |
| collection | DOAJ |
| description | In this research, we conducted systematic photometric, spectroscopic, and theoretical modeling analyses of two δ Scuti stars—KIC 12602250 and KIC 5768203—that pulsate only in radial modes. We collected their relevant photometric and spectroscopic parameters from multiple catalogs and estimated the absolute luminosities of both stars. Using high-precision time-series data from Kepler and TESS, we performed in-depth analysis of the periodic modulation in pulsation frequency phases, successfully determining the orbital periods and companion mass distribution ranges for these binary systems. Additionally, we thoroughly investigated the temporal evolution characteristics of pulsation periods and amplitudes. Based on calculations using Modules for Experiments in Stellar Astrophysics stellar evolution models, we determined that KIC 12602250 has a mass of $M=1.6{6}_{-0.07}^{+0.05}\,{M}_{\odot }$ with metallicity $Z=0.03{9}_{-0.010}^{+0.018}$ and is currently in the main-sequence evolutionary stage. For KIC 5768203, we derived precise parameters through rigorous constraints: mass M = 2.09 ± 0.01 M _⊙ , metallicity Z = 0.024 ± 0.003, and radius R = 3.19 ± 0.01 R _⊙ . Theoretical models reveal that this star has already crossed the first main-sequence turn-off point and entered the late-main-sequence evolutionary stage. Through comparative studies with typical High Amplitude δ Scuti stars, we believe that the primary reason for the low radial pulsation amplitudes in these two stars likely stems from their specific evolutionary states. |
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| institution | Matheson Library |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-248e59c516404c8889acd42d92cdda4c2025-07-17T12:41:12ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198813710.3847/1538-4357/add406Modeling of Two Low-amplitude Radially Pulsating δ Scuti Stars: KIC 12602250 and KIC 5768203Shuguo Ma0A-Li Luo1https://orcid.org/0000-0001-7865-2648Peng Wei2https://orcid.org/0000-0002-5674-4223Chenglong Lv3https://orcid.org/0000-0001-6354-1646Ming Yang4Fang Zuo5https://orcid.org/0000-0002-9081-8951Yingzhen Cui6https://orcid.org/0000-0002-6926-2872Shuo Li7https://orcid.org/0000-0002-8913-3605Gang Meng8Wen Hou9https://orcid.org/0000-0003-0716-1029Yuji He10https://orcid.org/0009-0008-0146-118XYinbi Li11https://orcid.org/0000-0001-7607-2666Zhongyang Liu12https://orcid.org/0009-0005-2920-7261Xiao-Xiao Ma13https://orcid.org/0000-0002-9279-2783Jun-Chao Liang14https://orcid.org/0009-0001-9085-8718Fei Dang15Daoye Yang16Ali Esamdin17https://orcid.org/0000-0003-1845-4900Hao Zeng18Cai-Xia Qu19https://orcid.org/0000-0002-5460-2205CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cnCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People’s Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People’s Republic of ChinaCollege of Surveying and Geo-Informatics, Tongji University , Shanghai 200092, People’s Republic of ChinaCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cnCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cnCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaDepartment of Astronomy, Beijing Normal University , Beijing, 100875, People’s Republic of ChinaCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cnCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cnDepartment of Astronomy, Beijing Normal University , Beijing, 100875, People’s Republic of ChinaCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People’s Republic of ChinaSchool of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China; Xinjiang Astronomical Observatory, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People’s Republic of ChinaSchool of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China; Xinjiang Astronomical Observatory, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People’s Republic of ChinaCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; masg@bao.ac.cn, lal@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaIn this research, we conducted systematic photometric, spectroscopic, and theoretical modeling analyses of two δ Scuti stars—KIC 12602250 and KIC 5768203—that pulsate only in radial modes. We collected their relevant photometric and spectroscopic parameters from multiple catalogs and estimated the absolute luminosities of both stars. Using high-precision time-series data from Kepler and TESS, we performed in-depth analysis of the periodic modulation in pulsation frequency phases, successfully determining the orbital periods and companion mass distribution ranges for these binary systems. Additionally, we thoroughly investigated the temporal evolution characteristics of pulsation periods and amplitudes. Based on calculations using Modules for Experiments in Stellar Astrophysics stellar evolution models, we determined that KIC 12602250 has a mass of $M=1.6{6}_{-0.07}^{+0.05}\,{M}_{\odot }$ with metallicity $Z=0.03{9}_{-0.010}^{+0.018}$ and is currently in the main-sequence evolutionary stage. For KIC 5768203, we derived precise parameters through rigorous constraints: mass M = 2.09 ± 0.01 M _⊙ , metallicity Z = 0.024 ± 0.003, and radius R = 3.19 ± 0.01 R _⊙ . Theoretical models reveal that this star has already crossed the first main-sequence turn-off point and entered the late-main-sequence evolutionary stage. Through comparative studies with typical High Amplitude δ Scuti stars, we believe that the primary reason for the low radial pulsation amplitudes in these two stars likely stems from their specific evolutionary states.https://doi.org/10.3847/1538-4357/add406Delta Scuti variable starsMulti-periodic variable starsPulsating variable stars |
| spellingShingle | Shuguo Ma A-Li Luo Peng Wei Chenglong Lv Ming Yang Fang Zuo Yingzhen Cui Shuo Li Gang Meng Wen Hou Yuji He Yinbi Li Zhongyang Liu Xiao-Xiao Ma Jun-Chao Liang Fei Dang Daoye Yang Ali Esamdin Hao Zeng Cai-Xia Qu Modeling of Two Low-amplitude Radially Pulsating δ Scuti Stars: KIC 12602250 and KIC 5768203 The Astrophysical Journal Delta Scuti variable stars Multi-periodic variable stars Pulsating variable stars |
| title | Modeling of Two Low-amplitude Radially Pulsating δ Scuti Stars: KIC 12602250 and KIC 5768203 |
| title_full | Modeling of Two Low-amplitude Radially Pulsating δ Scuti Stars: KIC 12602250 and KIC 5768203 |
| title_fullStr | Modeling of Two Low-amplitude Radially Pulsating δ Scuti Stars: KIC 12602250 and KIC 5768203 |
| title_full_unstemmed | Modeling of Two Low-amplitude Radially Pulsating δ Scuti Stars: KIC 12602250 and KIC 5768203 |
| title_short | Modeling of Two Low-amplitude Radially Pulsating δ Scuti Stars: KIC 12602250 and KIC 5768203 |
| title_sort | modeling of two low amplitude radially pulsating δ scuti stars kic 12602250 and kic 5768203 |
| topic | Delta Scuti variable stars Multi-periodic variable stars Pulsating variable stars |
| url | https://doi.org/10.3847/1538-4357/add406 |
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