New Method to Detect and Characterize Active Be Star Candidates in Open Clusters
With the aim of better understanding the physical conditions under which Be stars form and evolve, it is imperative to further investigate whether poorly studied young open clusters host Be stars. In this work, we explain how data from Gaia DR2 and DR3 can be combined to recover and characterize act...
| Main Authors: | , , , |
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| Format: | Article |
| Language: | English |
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MDPI AG
2023-02-01
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| Series: | Galaxies |
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| Online Access: | https://www.mdpi.com/2075-4434/11/1/37 |
| _version_ | 1797620906396221440 |
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| author | Anahí Granada Maziar R. Ghoreyshi Carol E. Jones Tõnis Eenmäe |
| author_facet | Anahí Granada Maziar R. Ghoreyshi Carol E. Jones Tõnis Eenmäe |
| author_sort | Anahí Granada |
| collection | DOAJ |
| description | With the aim of better understanding the physical conditions under which Be stars form and evolve, it is imperative to further investigate whether poorly studied young open clusters host Be stars. In this work, we explain how data from Gaia DR2 and DR3 can be combined to recover and characterize active Be stars in open clusters. We test our methodology in four open clusters broadly studied in the literature, known for hosting numerous Be stars. In addition, we show that the disk formation and dissipation approach that is typically used to model long term Be star variability, can explain the observed trends for Be stars in a (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">G</mi><mrow><mi>D</mi><mi>R</mi><mn>3</mn></mrow></msub></semantics></math></inline-formula>-<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">G</mi><mrow><mi>D</mi><mi>R</mi><mn>2</mn></mrow></msub></semantics></math></inline-formula>) versus <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">G</mi><mrow><mi>D</mi><mi>R</mi><mn>3</mn></mrow></msub></semantics></math></inline-formula> plot. We propose that extending this methodology to other open clusters, and, in particular, those that are poorly studied, will help to increase the number of Be candidates. Eventually, Be stars may eclipse binary systems in open clusters. |
| first_indexed | 2024-03-11T08:48:13Z |
| format | Article |
| id | doaj.art-bddff45ec0f640cd8a97b93ab549b937 |
| institution | Directory Open Access Journal |
| issn | 2075-4434 |
| language | English |
| last_indexed | 2024-03-11T08:48:13Z |
| publishDate | 2023-02-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Galaxies |
| spelling | doaj.art-bddff45ec0f640cd8a97b93ab549b9372023-11-16T20:38:34ZengMDPI AGGalaxies2075-44342023-02-011113710.3390/galaxies11010037New Method to Detect and Characterize Active Be Star Candidates in Open ClustersAnahí Granada0Maziar R. Ghoreyshi1Carol E. Jones2Tõnis Eenmäe3Centro Interdisciplinario de Telecomunicaciones, Electrónica, Computación y Ciencia Aplicada (CITECCA), Sede Andina, Universidad Nacional de Río Negro, Anasagasti 1463, San Carlos de Bariloche R8400AHN, Río Negro, ArgentinaPhysics and Astronomy Department, The University of Western Ontario, London, ON N6A 3K7, CanadaPhysics and Astronomy Department, The University of Western Ontario, London, ON N6A 3K7, CanadaFaculty of Science and Technology, University of Tartu, Observatooriumi 1, 61602 Tõravere, EstoniaWith the aim of better understanding the physical conditions under which Be stars form and evolve, it is imperative to further investigate whether poorly studied young open clusters host Be stars. In this work, we explain how data from Gaia DR2 and DR3 can be combined to recover and characterize active Be stars in open clusters. We test our methodology in four open clusters broadly studied in the literature, known for hosting numerous Be stars. In addition, we show that the disk formation and dissipation approach that is typically used to model long term Be star variability, can explain the observed trends for Be stars in a (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">G</mi><mrow><mi>D</mi><mi>R</mi><mn>3</mn></mrow></msub></semantics></math></inline-formula>-<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">G</mi><mrow><mi>D</mi><mi>R</mi><mn>2</mn></mrow></msub></semantics></math></inline-formula>) versus <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">G</mi><mrow><mi>D</mi><mi>R</mi><mn>3</mn></mrow></msub></semantics></math></inline-formula> plot. We propose that extending this methodology to other open clusters, and, in particular, those that are poorly studied, will help to increase the number of Be candidates. Eventually, Be stars may eclipse binary systems in open clusters.https://www.mdpi.com/2075-4434/11/1/37Be starsearly-type emission starscircumstellar disksearly-type variable starsopen star clustersGaia |
| spellingShingle | Anahí Granada Maziar R. Ghoreyshi Carol E. Jones Tõnis Eenmäe New Method to Detect and Characterize Active Be Star Candidates in Open Clusters Galaxies Be stars early-type emission stars circumstellar disks early-type variable stars open star clusters Gaia |
| title | New Method to Detect and Characterize Active Be Star Candidates in Open Clusters |
| title_full | New Method to Detect and Characterize Active Be Star Candidates in Open Clusters |
| title_fullStr | New Method to Detect and Characterize Active Be Star Candidates in Open Clusters |
| title_full_unstemmed | New Method to Detect and Characterize Active Be Star Candidates in Open Clusters |
| title_short | New Method to Detect and Characterize Active Be Star Candidates in Open Clusters |
| title_sort | new method to detect and characterize active be star candidates in open clusters |
| topic | Be stars early-type emission stars circumstellar disks early-type variable stars open star clusters Gaia |
| url | https://www.mdpi.com/2075-4434/11/1/37 |
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