R.K. Zamanov , B. Spassov , R. Konstantinova-Antova , M. Moyseev , J. Marti , M.F. Bode , V. Vujcic , V. Sreckovic
{"title":"Mira的光学闪烁和伴星白矮星的质量吸积速率","authors":"R.K. Zamanov , B. Spassov , R. Konstantinova-Antova , M. Moyseev , J. Marti , M.F. Bode , V. Vujcic , V. Sreckovic","doi":"10.1016/j.newast.2025.102452","DOIUrl":null,"url":null,"abstract":"<div><div>We report photometric observations in Johnson <span><math><mi>B</mi></math></span> and <span><math><mi>V</mi></math></span> bands of the short term variability (flickering) of Mira – the prototypical pulsating asymptotic giant branch (AGB) star. The observations are performed over 4 consecutive nights (24–28 November 2024), during the last minimum of the Mira pulsation. The peak-to-peak amplitude observed is 0.25-0.34 mag in <span><math><mi>B</mi></math></span> band and 0.14-0.19 mag in <span><math><mi>V</mi></math></span> band. For the flickering source we find colour <span><math><mrow><msub><mrow><mrow><mo>(</mo><mi>B</mi><mo>−</mo><mi>V</mi><mo>)</mo></mrow></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>44</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>11</mn></mrow></math></span>, temperature <span><math><mrow><mn>7000</mn><mo>±</mo><mn>700</mn></mrow></math></span> K, and average radius <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mi>f</mi><mi>l</mi></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>30</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>07</mn></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. Assuming the mass of the white dwarf <span><math><mrow><mo>≈</mo><mn>0</mn><mo>.</mo><mn>6</mn></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, we estimate a mass accretion rate <span><math><mrow><mo>≈</mo><mn>6</mn><mo>.</mo><mn>0</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>10</mn></mrow></msup></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span> yr<sup>−1</sup> during our observations.</div><div>The data will be available on Zenodo.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102452"},"PeriodicalIF":1.9000,"publicationDate":"2025-07-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Optical flickering in Mira and mass accretion rate onto the companion white dwarf\",\"authors\":\"R.K. Zamanov , B. Spassov , R. Konstantinova-Antova , M. Moyseev , J. Marti , M.F. Bode , V. Vujcic , V. Sreckovic\",\"doi\":\"10.1016/j.newast.2025.102452\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<div><div>We report photometric observations in Johnson <span><math><mi>B</mi></math></span> and <span><math><mi>V</mi></math></span> bands of the short term variability (flickering) of Mira – the prototypical pulsating asymptotic giant branch (AGB) star. The observations are performed over 4 consecutive nights (24–28 November 2024), during the last minimum of the Mira pulsation. The peak-to-peak amplitude observed is 0.25-0.34 mag in <span><math><mi>B</mi></math></span> band and 0.14-0.19 mag in <span><math><mi>V</mi></math></span> band. For the flickering source we find colour <span><math><mrow><msub><mrow><mrow><mo>(</mo><mi>B</mi><mo>−</mo><mi>V</mi><mo>)</mo></mrow></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>44</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>11</mn></mrow></math></span>, temperature <span><math><mrow><mn>7000</mn><mo>±</mo><mn>700</mn></mrow></math></span> K, and average radius <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mi>f</mi><mi>l</mi></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>30</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>07</mn></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. Assuming the mass of the white dwarf <span><math><mrow><mo>≈</mo><mn>0</mn><mo>.</mo><mn>6</mn></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, we estimate a mass accretion rate <span><math><mrow><mo>≈</mo><mn>6</mn><mo>.</mo><mn>0</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>10</mn></mrow></msup></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span> yr<sup>−1</sup> during our observations.</div><div>The data will be available on Zenodo.</div></div>\",\"PeriodicalId\":54727,\"journal\":{\"name\":\"New Astronomy\",\"volume\":\"121 \",\"pages\":\"Article 102452\"},\"PeriodicalIF\":1.9000,\"publicationDate\":\"2025-07-16\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"New Astronomy\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://www.sciencedirect.com/science/article/pii/S1384107625001010\",\"RegionNum\":4,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q2\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"New Astronomy","FirstCategoryId":"101","ListUrlMain":"https://www.sciencedirect.com/science/article/pii/S1384107625001010","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
Optical flickering in Mira and mass accretion rate onto the companion white dwarf
We report photometric observations in Johnson and bands of the short term variability (flickering) of Mira – the prototypical pulsating asymptotic giant branch (AGB) star. The observations are performed over 4 consecutive nights (24–28 November 2024), during the last minimum of the Mira pulsation. The peak-to-peak amplitude observed is 0.25-0.34 mag in band and 0.14-0.19 mag in band. For the flickering source we find colour , temperature K, and average radius R. Assuming the mass of the white dwarf M, we estimate a mass accretion rate M yr−1 during our observations.
期刊介绍：
New Astronomy publishes articles in all fields of astronomy and astrophysics, with a particular focus on computational astronomy: mathematical and astronomy techniques and methodology, simulations, modelling and numerical results and computational techniques in instrumentation.
New Astronomy includes full length research articles and review articles. The journal covers solar, stellar, galactic and extragalactic astronomy and astrophysics. It reports on original research in all wavelength bands, ranging from radio to gamma-ray.
求助内容：
应助结果提醒方式：
京公网安备 11010802042870号
