Period Variation Rates of Four Radial Single-Mode High-Amplitude Delta Scuti Stars
In this work, we present a study on the long time-scale period variations of four single-mode high-amplitude delta Scuti stars (HADS) via the classical <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><m...
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| author | Tian-Fang Ma Jia-Shu Niu Hui-Fang Xue |
| author_facet | Tian-Fang Ma Jia-Shu Niu Hui-Fang Xue |
| author_sort | Tian-Fang Ma |
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| description | In this work, we present a study on the long time-scale period variations of four single-mode high-amplitude delta Scuti stars (HADS) via the classical <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>O</mi><mo>−</mo><mi>C</mi></mrow></semantics></math></inline-formula> analysis. The target HADS are (i) XX Cygni, (ii) YZ Bootis, (iii) GP Andromedae, and (iv) ZZ Microscopii. The newly determined times of maximum light came from the Transiting Exoplanet Survey Satellite (TESS), American Association of Variable Star Observers (AAVSO), and Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne (BAV) projects. Together with the times of maximum light obtained in the historical literature, the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>O</mi><mo>−</mo><mi>C</mi></mrow></semantics></math></inline-formula> analysis was performed on these HADS, in which we obtained the linear period variation rates <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mover accent="true"><mi>P</mi><mo>˙</mo></mover><mo>/</mo><mi>P</mi></mrow></semantics></math></inline-formula> as <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mrow><mo>(</mo><mn>9.2</mn><mo>±</mo><mn>0.2</mn><mo>)</mo></mrow><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>9</mn></mrow></msup><mspace width="4pt"></mspace><msup><mi>yr</mi><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></semantics></math></inline-formula>, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mrow><mo>(</mo><mn>3.2</mn><mo>±</mo><mn>0.2</mn><mo>)</mo></mrow><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>9</mn></mrow></msup><mspace width="4pt"></mspace><msup><mi>yr</mi><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></semantics></math></inline-formula>, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mrow><mo>(</mo><mn>4.22</mn><mo>±</mo><mn>0.03</mn><mo>)</mo></mrow><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>8</mn></mrow></msup><mspace width="4pt"></mspace><msup><mi>yr</mi><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></semantics></math></inline-formula>, and <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mrow><mo>(</mo><mo>−</mo><mn>2.06</mn><mo>±</mo><mn>0.02</mn><mo>)</mo></mrow><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>8</mn></mrow></msup><mspace width="4pt"></mspace><msup><mi>yr</mi><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></semantics></math></inline-formula>, respectively. Based on these results and some earlier research, we also discuss the evolutionary stages and the mechanisms of the period variation of these four HADS. |
| format | Article |
| id | doaj-art-2f13cb794a08465baa3133172c7f668c |
| institution | DOAJ |
| issn | 2218-1997 |
| language | English |
| publishDate | 2025-03-01 |
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| spelling | doaj-art-2f13cb794a08465baa3133172c7f668c2025-08-20T02:43:09ZengMDPI AGUniverse2218-19972025-03-011138610.3390/universe11030086Period Variation Rates of Four Radial Single-Mode High-Amplitude Delta Scuti StarsTian-Fang Ma0Jia-Shu Niu1Hui-Fang Xue2Institute of Theoretical Physics, Shanxi University, Taiyuan 030006, ChinaInstitute of Theoretical Physics, Shanxi University, Taiyuan 030006, ChinaDepartment of Physics, Taiyuan Normal University, Jinzhong 030619, ChinaIn this work, we present a study on the long time-scale period variations of four single-mode high-amplitude delta Scuti stars (HADS) via the classical <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>O</mi><mo>−</mo><mi>C</mi></mrow></semantics></math></inline-formula> analysis. The target HADS are (i) XX Cygni, (ii) YZ Bootis, (iii) GP Andromedae, and (iv) ZZ Microscopii. The newly determined times of maximum light came from the Transiting Exoplanet Survey Satellite (TESS), American Association of Variable Star Observers (AAVSO), and Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne (BAV) projects. Together with the times of maximum light obtained in the historical literature, the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>O</mi><mo>−</mo><mi>C</mi></mrow></semantics></math></inline-formula> analysis was performed on these HADS, in which we obtained the linear period variation rates <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mover accent="true"><mi>P</mi><mo>˙</mo></mover><mo>/</mo><mi>P</mi></mrow></semantics></math></inline-formula> as <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mrow><mo>(</mo><mn>9.2</mn><mo>±</mo><mn>0.2</mn><mo>)</mo></mrow><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>9</mn></mrow></msup><mspace width="4pt"></mspace><msup><mi>yr</mi><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></semantics></math></inline-formula>, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mrow><mo>(</mo><mn>3.2</mn><mo>±</mo><mn>0.2</mn><mo>)</mo></mrow><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>9</mn></mrow></msup><mspace width="4pt"></mspace><msup><mi>yr</mi><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></semantics></math></inline-formula>, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mrow><mo>(</mo><mn>4.22</mn><mo>±</mo><mn>0.03</mn><mo>)</mo></mrow><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>8</mn></mrow></msup><mspace width="4pt"></mspace><msup><mi>yr</mi><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></semantics></math></inline-formula>, and <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mrow><mo>(</mo><mo>−</mo><mn>2.06</mn><mo>±</mo><mn>0.02</mn><mo>)</mo></mrow><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>8</mn></mrow></msup><mspace width="4pt"></mspace><msup><mi>yr</mi><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></semantics></math></inline-formula>, respectively. Based on these results and some earlier research, we also discuss the evolutionary stages and the mechanisms of the period variation of these four HADS.https://www.mdpi.com/2218-1997/11/3/86pulsating starsdelta Scuti starsstellar evolution |
| spellingShingle | Tian-Fang Ma Jia-Shu Niu Hui-Fang Xue Period Variation Rates of Four Radial Single-Mode High-Amplitude Delta Scuti Stars Universe pulsating stars delta Scuti stars stellar evolution |
| title | Period Variation Rates of Four Radial Single-Mode High-Amplitude Delta Scuti Stars |
| title_full | Period Variation Rates of Four Radial Single-Mode High-Amplitude Delta Scuti Stars |
| title_fullStr | Period Variation Rates of Four Radial Single-Mode High-Amplitude Delta Scuti Stars |
| title_full_unstemmed | Period Variation Rates of Four Radial Single-Mode High-Amplitude Delta Scuti Stars |
| title_short | Period Variation Rates of Four Radial Single-Mode High-Amplitude Delta Scuti Stars |
| title_sort | period variation rates of four radial single mode high amplitude delta scuti stars |
| topic | pulsating stars delta Scuti stars stellar evolution |
| url | https://www.mdpi.com/2218-1997/11/3/86 |
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