Slowly cooling white dwarfs in M13 from stable hydrogen burning

White dwarfs (WDs) are the final evolutionary product of the vast majority of stars in the Universe. They are electron-degenerate structures characterized by no stable thermonuclear activity, and their evolution is generally described as a pure cooling process. Their cooling rate is adopted as cosmi...

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Autores principales: Chen, Jianxing, Ferraro, Francesco R., Cadelano, M., Salaris, Maurizio, Lanzoni, Barbara, Pallanca, C., Althaus, Leandro Gabriel, Dalessandro, Emanuele
Formato: Articulo Preprint
Lenguaje:Inglés
Publicado: 2021
Materias:
Ciencias Astronómicas
Estrellas
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/138293
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-138293
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
Estrellas
spellingShingle Ciencias Astronómicas
Estrellas
Chen, Jianxing
Ferraro, Francesco R.
Cadelano, M.
Salaris, Maurizio
Lanzoni, Barbara
Pallanca, C.
Althaus, Leandro Gabriel
Dalessandro, Emanuele
Slowly cooling white dwarfs in M13 from stable hydrogen burning
topic_facet Ciencias Astronómicas
Estrellas
description White dwarfs (WDs) are the final evolutionary product of the vast majority of stars in the Universe. They are electron-degenerate structures characterized by no stable thermonuclear activity, and their evolution is generally described as a pure cooling process. Their cooling rate is adopted as cosmic chronometer to constrain the age of several Galactic populations, including the disk, globular and open clusters. By analysing high-resolution photometric data of two very similar Galactic globular clusters (M3 and M13), we find a clear-cut and unexpected overabundance of bright WDs in M13. Theoretical models suggest that, consistent with the horizontal branch morphology, this overabundance is due to a slowing down of the cooling process in ~70% of the WDs in M13, caused by stable thermonuclear burning in their residual hydrogen-rich envelope. The presented observational evidence of quiescent thermonuclear activity occurring in cooling WDs brings new attention on the use of the WD cooling rate as cosmic chronometer for low-metallicity environments. Rather than cooling down according to a well-established rate, some ~70% of the white dwarfs in globular cluster M13 are delaying their stellar demise by burning left-over hydrogen conserved by skipping the third dredge-up event.
format Articulo
Preprint
author Chen, Jianxing
Ferraro, Francesco R.
Cadelano, M.
Salaris, Maurizio
Lanzoni, Barbara
Pallanca, C.
Althaus, Leandro Gabriel
Dalessandro, Emanuele
author_facet Chen, Jianxing
Ferraro, Francesco R.
Cadelano, M.
Salaris, Maurizio
Lanzoni, Barbara
Pallanca, C.
Althaus, Leandro Gabriel
Dalessandro, Emanuele
author_sort Chen, Jianxing
title Slowly cooling white dwarfs in M13 from stable hydrogen burning
title_short Slowly cooling white dwarfs in M13 from stable hydrogen burning
title_full Slowly cooling white dwarfs in M13 from stable hydrogen burning
title_fullStr Slowly cooling white dwarfs in M13 from stable hydrogen burning
title_full_unstemmed Slowly cooling white dwarfs in M13 from stable hydrogen burning
title_sort slowly cooling white dwarfs in m13 from stable hydrogen burning
publishDate 2021
url http://sedici.unlp.edu.ar/handle/10915/138293
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