Crystallization of white dwarfs in globular clusters
White dwarf stars are the most common end point of stellar evolution. Due to their large numbers and multiple applications, white dwarfs are among the most interesting objects to study in the universe. Based on the observations provided by the Gaia Space Mission, studies of these objects showed that...
- Autores:
-
Castro Idarraga, Juan Pablo
- Tipo de recurso:
- Trabajo de grado de pregrado
- Fecha de publicación:
- 2024
- Institución:
- Universidad de los Andes
- Repositorio:
- Séneca: repositorio Uniandes
- Idioma:
- eng
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- oai:repositorio.uniandes.edu.co:1992/74727
- Acceso en línea:
- https://hdl.handle.net/1992/74727
- Palabra clave:
- White dwarfs
Astrophysics
Crystallization
Globular clusters
Física
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| dc.title.eng.fl_str_mv |
Crystallization of white dwarfs in globular clusters |
| dc.title.alternative.spa.fl_str_mv |
Cristalización de enanas blancas en cumulos globulares |
| title |
Crystallization of white dwarfs in globular clusters |
| spellingShingle |
Crystallization of white dwarfs in globular clusters White dwarfs Astrophysics Crystallization Globular clusters Física |
| title_short |
Crystallization of white dwarfs in globular clusters |
| title_full |
Crystallization of white dwarfs in globular clusters |
| title_fullStr |
Crystallization of white dwarfs in globular clusters |
| title_full_unstemmed |
Crystallization of white dwarfs in globular clusters |
| title_sort |
Crystallization of white dwarfs in globular clusters |
| dc.creator.fl_str_mv |
Castro Idarraga, Juan Pablo |
| dc.contributor.advisor.none.fl_str_mv |
Oostra Van Noppen, Benjamín Torres Gil, Santiago Camisassa, María Eugenia |
| dc.contributor.author.none.fl_str_mv |
Castro Idarraga, Juan Pablo |
| dc.contributor.jury.none.fl_str_mv |
Sabogal Martínez, Beatriz Eugenia |
| dc.contributor.researchgroup.none.fl_str_mv |
Facultad de Ciencias::Astrofísica |
| dc.subject.keyword.eng.fl_str_mv |
White dwarfs Astrophysics Crystallization Globular clusters |
| topic |
White dwarfs Astrophysics Crystallization Globular clusters Física |
| dc.subject.themes.none.fl_str_mv |
Física |
| description |
White dwarf stars are the most common end point of stellar evolution. Due to their large numbers and multiple applications, white dwarfs are among the most interesting objects to study in the universe. Based on the observations provided by the Gaia Space Mission, studies of these objects showed that a small fraction of the ultra-massive white dwarfs undergo a substantial delay in their cooling times. To explain the delay, additional energy sources inside the white dwarf have been considered. Neon 22 sedimentation and crystallization are the most important sources. Considering these two extra energy sources and high metallicity, it was possible to explain the delay. In this framework, we aimed to analyze the effect of crystallization and Neon 22 sedimentation on white dwarfs, especially in ultra-massive white dwarfs. To do this, we generated a wide sample of synthetic globular clusters with different physical properties using Monte Carlo techniques and an up-to-date set of white dwarf cooling tracks. These synthetic stellar populations were analyzed using Hertzsprung-Russell diagrams, ς distributions, and a new quantity introduced in this text, the ultra-massive quotient. The extensive analysis showed that younger and metal-richer clusters present higher ultra-massive quotients and ς histograms centered on lower values. Moreover, Hertzsprung-Russell diagrams prove that a high metallicity and a carbon-oxygen core chemical composition abruptly increase the delay time undergone by the white dwarfs due to Neon 22 sedimentation. In addition, we found that only a stellar population with ultra-massive carbon-oxygen core white dwarfs counts with a significant number of white dwarfs in the ultra-massive region. These findings allow us to compare our simulations with real observed clusters (NGC 6397, NGC 6791, and 47 Tucanae). The comparison shows that the ultra-massive white dwarfs are located around the same values of ς for synthetic and observed clusters. Additionally, we could predict, thanks to the ultra-massive quotient, which clusters have the highest percentage of ultra-massive white dwarfs visible in their color-magnitude diagrams. |
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2024 |
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2024-07-26T19:54:29Z |
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2024-07-26T19:54:29Z |
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2024-07-25 |
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Trabajo de grado - Pregrado |
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| dc.language.iso.none.fl_str_mv |
eng |
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eng |
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Althaus, L. G., García-Berro, E., Isern, J., & Corsico, A. H. (2005). Mass-radius relations for massive white dwarf stars. Astron. Astrophys., 441(2), 689–694. https://doi.org/10.1051/0004-6361:20052996 Althaus, L. G., García-Berro, E., Renedo, I., Isern, J., Corsico, A. H., & Rohrmann, R. D. (2010). Evolution of White Dwarf Stars with High-metallicity Progenitors: The Role of 22Ne Diffusion. Astrophys. J., 719(1), 612–621. https://doi.org/10.1088/0004- 637X/719/1/612 Althaus, L. G., Panei, J. A., Bertolami, M. M. M., Garcia-Berro, E., Corsico, A. H., Romero, A. D., Kepler, S. O., & Rohrmann, R. D. (2009). NEW EVOLUTIONARY SEQUENCES FOR HOT H-DEFICIENT WHITE DWARFS ON THE BASIS OF A FULL ACCOUNT OF PROGENITOR EVOLUTION. Astrophys. J., 704(2), 1605. https://doi.org/10.1088/0004-637X/704/2/1605 Althaus, L. G., Panei, J. A., Romero, A. D., Rohrmann, R. D., Corsico, A. H., Garcia-Berro, E., & Bertolami, M. M. M. (2009). Evolution and colors of helium-core white dwarf stars with high-metallicity progenitors. Astron. Astrophys., 502(1), 207–216. https: //doi.org/10.1051/0004-6361/200911640 Althaus, L. G., Serenelli, A. M., Corsico, A. H., & Montgomery, M. H. (2003). New evolutionary models for massive ZZ Ceti stars. I. First results for their pulsational properties. Astron. Astrophys., 404(2), 593–609. https://doi.org/10.1051/0004- 6361: 20030472 Althaus, L. G., Camisassa, M. E., Bertolami, M. M. M., Corsico, A. H., & Garcıa-Berro, E. (2015). White dwarf evolutionary sequences for low-metallicity progenitors: The impact of third dredge-up. Astron. Astrophys., 576, A9. https://doi.org/10.1051/0004- 6361/201424922 Althaus, L. G., Corsico, A. H., Isern, J., & Garcia-Berro, E. (2010). Evolutionary and pulsational properties of white dwarf stars. arXiv. https://doi.org/10.1007/s00159-010- 0033-1 Althaus, L. G., De Geronimo, F., Corsico, A., Torres, S., & Garcia-Berro, E. (2017). The evo lution of white dwarfs resulting from helium-enhanced, low-metallicity progenitor stars. Astron. Astrophys., 597, A67. https://doi.org/10.1051/0004-6361/201629909 Althaus, L. G., Pons, P. G., Corsico, A. H., Bertolami, M. M., De Gernimo, F., Camisassa, M. E., Torres, S., Gutierrez, J., & Rebassa-Mansergas, A. (2021). The formation of ultra-massive carbon-oxygen core white dwarfs and their evolutionary and pulsational properties. Astron. Astrophys., 646, A30. https : / / doi . org / 10 . 1051 / 0004 - 6361/202038930 Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. (2009). The Chemical Composition of the Sun. Annual Review of Astronomy and Astrophysics, 47(1), 481–522. https: //doi.org/10.1146/annurev.astro.46.060407.145222 Bastian, N., & Lardo, C. (2017). Multiple Stellar Populations in Globular Clusters. arXiv. https://doi.org/10.1146/annurev-astro-081817-051839 Camacho D´ıaz, J. (2014, June). 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Accreted versus In Situ Milky Way Globular Clusters. arXiv. https://doi.org/10.1111/j.1365-2966.2010.16373.x Gaia collaboration, c. (2018). Gaia Data Release 2 - Observational Hertzsprung-Russell diagrams. Astron. Astrophys., 616, A10. https://doi.org/10.1051/0004-6361/201832843 Gaia collaborators, c. (2023). Gaia Data Release 3 - Summary of the content and survey properties. Astron. Astrophys., 674, A1. https://doi.org/10.1051/0004-6361/202243940 Gaia DR2 Passbands - Gaia - Cosmos [[Online; accessed 12. May 2024]]. (2024, May). https://www.cosmos.esa.int/web/gaia/iow 20180316 Garcia-Berro, E., Torres, S., Renedo, I., Camacho, J., Althaus, L. G., Corsico, A. H., Salaris, M., & Isern, J. (2011). The white-dwarf cooling sequence of NGC 6791: a unique tool for stellar evolution. aap, 533, Article A31, A31. https://doi.org/10.1051/0004- 6361/201116499 Garcia–Berro, E., & Oswalt, T. D. (2016). The white dwarf luminosity function. New As tronomy Reviews, 72-74, 1–22. https://doi.org/https://doi.org/10.1016/j.newar.2016. 08.001 Garcia-Berro, E., Torres, S., Isern, J., & Burkert, A. (2004). Monte Carlo simulations of the halo white dwarf population. Astron. Astrophys., 418(1), 53–65. https://doi.org/10. 1051/0004-6361:2003454 Garcia-Berro, E., Torres, S., Althaus, L. G., & Miller Bertolami, M. M. (2014). The white dwarf cooling sequence of 47 Tucanae. Astron. Astrophys., 571, A56. https://doi.org/ 10.1051/0004-6361/201424652 Garcia-Berro, E., Torres, S., Althaus, L. G., Renedo, I., Loren-Aguilar, P., Corsico, A. H., Rohrmann, R. D., Salaris, M., & Isern, J. (2010). A white dwarf cooling age of 8 Gyr for NGC 6791 from physical separation processes. Nature, 465, 194–196. https: //doi.org/10.1038/nature09045 Gratton, R., Bragaglia, A., Carretta, E., D’Orazi, V., Lucatello, S., & Sollima, A. (2019). What is a globular cluster? An observational perspective. arXiv. https://doi.org/10. 1007/s00159-019-0119-3 Harris, W. 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M., Torres, S., Rebassa-Mansergas, A., Cruz, P., Murillo-Ojeda, R., Solano, E., Rodrigo, C., & Camisassa, M. E. (2023). Spectral classification of the 100 pc white dwarf population from Gaia-DR3 and the virtual observatory. Mon. Not. R. Astron. Soc., 518(4), 5106–5122. https://doi.org/10.1093/mnras/stac3382 Jimenez-Esteban, F. M., Torres, S., Rebassa-Mansergas, A., Skorobogatov, G., Solano, E., ´ Cantero, C., & Rodrigo, C. (2018). A white dwarf catalogue from Gaia-DR2 and the Virtual Observatory. Mon. Not. R. Astron. Soc., 480(4), 4505–4518. https://doi.org/ 10.1093/mnras/sty2120 Kato, M., Saio, H., & Hachisu, I. (2017). A Millennium-long Evolution of the 1 yr Recur rence Period Nova—Search for Any Indication of the Forthcoming He Flash. Astro phys. J., 844(2), 143. https://doi.org/10.3847/1538-4357/aa7c5e Mermilliod, J.-C., & Paunzen, E. (2003). Analysing the database for stars in open clusters I. General methods and description of the data. Astron. 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D., Toonen, S., Zapartas, E., Justham, S., & Gansicke, B. T. (2020). Looks can ¨ be deceiving - Underestimating the age of single white dwarfs due to binary mergers. Astron. Astrophys., 636, A31. https://doi.org/10.1051/0004-6361/201936889 Torres, S., Canals, P., Jimenez-Esteban, F. M., Rebassa-Mansergas, A., & Solano, E. (2022). ´ A population synthesis fitting of the Gaia resolved white dwarf binary populationwithin 100 pc. Monthly Notices of the Royal Astronomical Society, 511(4), 5462– 5474. https://doi.org/10.1093/mnras/stac374 Torres, S. (2002, July). Simulacion de Monte Carlo de la poblaci ´ on de enanas blancas de la ´ galaxia [Doctoral dissertation, Universitat Politecnica de Catalunya]. https://doi.org/ ` 10.5821/dissertation-2117-93889 Torres, S., Garcia-Berro, E., Burkert, A., & Isern, J. (2002). High-proper-motion white dwarfs and halo dark matter. Mon. Not. R. Astron. Soc., 336(3), 971–978. https : //doi.org/10.1046/j.1365-8711.2002.05830.x Torres, S., Garc´ıa-Berro, E., Althaus, L. G., & Camisassa, M. E. (2015). The white dwarf population of NGC 6397. Astron. Astrophys., 581, A90. https://doi.org/10.1051/ 0004-6361/201526157 Tremblay, N. P., Gentile Fusillo, Tremblay, P.-E., Gensicke, B. T., Manser, C. J., Cunning ham, T., Cukanovaite, E., Hollands, M., Marsh, T., Raddi, R., Jordan, S., Toonen, S., Geier, S., Barstow, M., & Cummings, J. D. (2019). A Gaia Data Release 2 catalog of white dwarfs and a comparison with SDSS. Mon. Not. R. Astron. Soc., 482(4), 4570–4591. https://doi.org/10.1093/mnras/sty3016 van Horn, H. M. (1968). Crystallization of White Dwarfs. Astrophys. J., 151, 227. https: //doi.org/10.1086/149432 Yoon, S.-C., Podsiadlowski, P., & Rosswog, S. (2007). Remnant evolution after a car bon–oxygen white dwarf merger. Mon. Not. R. Astron. Soc., 380(3), 933–948. https: //doi.org/10.1111/j.1365-2966.2007.12161.x |
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Oostra Van Noppen, BenjamínTorres Gil, SantiagoCamisassa, María EugeniaCastro Idarraga, Juan PabloSabogal Martínez, Beatriz EugeniaFacultad de Ciencias::Astrofísica2024-07-26T19:54:29Z2024-07-26T19:54:29Z2024-07-25https://hdl.handle.net/1992/74727instname:Universidad de los Andesreponame:Repositorio Institucional Sénecarepourl:https://repositorio.uniandes.edu.co/White dwarf stars are the most common end point of stellar evolution. Due to their large numbers and multiple applications, white dwarfs are among the most interesting objects to study in the universe. Based on the observations provided by the Gaia Space Mission, studies of these objects showed that a small fraction of the ultra-massive white dwarfs undergo a substantial delay in their cooling times. To explain the delay, additional energy sources inside the white dwarf have been considered. Neon 22 sedimentation and crystallization are the most important sources. Considering these two extra energy sources and high metallicity, it was possible to explain the delay. In this framework, we aimed to analyze the effect of crystallization and Neon 22 sedimentation on white dwarfs, especially in ultra-massive white dwarfs. To do this, we generated a wide sample of synthetic globular clusters with different physical properties using Monte Carlo techniques and an up-to-date set of white dwarf cooling tracks. These synthetic stellar populations were analyzed using Hertzsprung-Russell diagrams, ς distributions, and a new quantity introduced in this text, the ultra-massive quotient. The extensive analysis showed that younger and metal-richer clusters present higher ultra-massive quotients and ς histograms centered on lower values. Moreover, Hertzsprung-Russell diagrams prove that a high metallicity and a carbon-oxygen core chemical composition abruptly increase the delay time undergone by the white dwarfs due to Neon 22 sedimentation. In addition, we found that only a stellar population with ultra-massive carbon-oxygen core white dwarfs counts with a significant number of white dwarfs in the ultra-massive region. These findings allow us to compare our simulations with real observed clusters (NGC 6397, NGC 6791, and 47 Tucanae). The comparison shows that the ultra-massive white dwarfs are located around the same values of ς for synthetic and observed clusters. Additionally, we could predict, thanks to the ultra-massive quotient, which clusters have the highest percentage of ultra-massive white dwarfs visible in their color-magnitude diagrams.Las enanas blancas son la etapa final en la vida de la mayoría de las estrellas de secuencia principal. debido a su gran numero y a sus múltiples aplicaciones, las enanas blancas están entre los objetos de estudio más interesantes del universo. Basándose en las observaciones de la Misión Espacial Gaia, diversos estudios encontraron que una pequeña porción de las enanas blancas ultramasivas sufre un efecto de retardo en sus tiempos de enfriamiento. Para explicar este retardo, es necesario considerar fuentes adicionales de energía dentro de la enana blanca. La sedimentación del neón-22 y la cristalización son los efectos más importantes. Al considerar estas dos fuentes extra de energía y una alta metalicidad, fue posible dar cuenta del retardo en el tiempo de enfriamiento de las enanas blancas. En este contexto, nuestro objetivo es analizar los efectos de la cristalización y la sedimentación del neón-22 en enanas blancas, especialmente en enanas blancas ultramasivas. Para esto, usando técnicas de Monte Carlo y modelos de enfriamiento de última generación, generamos una amplia gama de poblaciones sintéticas de estrellas con diferentes propiedades. Estas poblaciones sintéticas fueron analizadas usando diagramas Hertzsprung-Russell, histogramas de la variable ς y una nueva cantidad introducida en este texto, el cociente ultramasivo. Este extenso análisis mostro que los cúmulos más jóvenes y con las abundancias de metal más alta tienen cocientes ultramasivos más altos e histogramas de ς centrados en valores más bajos. Además, con los diagramas Hertzsprung-Russell se comprueba que una alta metalicidad y una composición química de carbono-oxigeno aumenta en gran medida el retardo en los modelos de enfriamiento causado por la sedimentación del neón-22. Comparamos nuestras simulaciones con la población de enanas blancas de cúmulos reales observados por el telescopio espacial Hubble, como lo son NGC 6397, NGC 6791 y 47 Tucanae. La comparación muestra que las enanas blancas ultramasivas se ubican sobre la misma región de ς, tanto para cúmulos sintéticos como observados. Adicionalmente, logramos predecir con ayuda del cociente ultramasivo el cumulo observado con el mayor porcentaje de enanas blancas ultramasivas visibles en su diagrama color magnitud.PregradoAstrofísica computacional74 páginasapplication/pdfengUniversidad de los AndesFísicaFacultad de CienciasDepartamento de FísicaAttribution-ShareAlike 4.0 Internationalhttp://creativecommons.org/licenses/by-sa/4.0/info:eu-repo/semantics/openAccesshttp://purl.org/coar/access_right/c_abf2Crystallization of white dwarfs in globular clustersCristalización de enanas blancas en cumulos globularesTrabajo de grado - Pregradoinfo:eu-repo/semantics/bachelorThesisinfo:eu-repo/semantics/acceptedVersionhttp://purl.org/coar/resource_type/c_7a1fTexthttp://purl.org/redcol/resource_type/TPWhite dwarfsAstrophysicsCrystallizationGlobular clustersFísicaAlthaus, L. G., García-Berro, E., Isern, J., & Corsico, A. H. (2005). Mass-radius relations for massive white dwarf stars. Astron. 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