Forever young white dwarfs: When stellar ageing stops
Visualitza/Obre
10.1051/0004-6361/202140720
Inclou dades d'ús des de 2022
Cita com:
hdl:2117/359180
Tipus de documentArticle
Data publicació2021-05-01
EditorEDP Sciences
Condicions d'accésAccés obert
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continguts d'aquesta obra estan subjectes a la llicència de Creative Commons
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Reconeixement-NoComercial-SenseObraDerivada 3.0 Espanya
Abstract
White dwarf stars are the most common end point of stellar evolution. The ultramassive white dwarfs are of special interest as they are related to type Ia supernovae explosions, merger events, and fast radio bursts. Ultramassive white dwarfs are expected to harbour oxygen-neon (ONe) cores as a result of single standard stellar evolution. However, a fraction of them could have carbon-oxygen (CO) cores. Recent studies, based on the new observations provided by the Gaia space mission, indicate that a small fraction of the ultramassive white dwarfs experience a strong delay in their cooling, which cannot be solely attributed to the occurrence of crystallisation, thus requiring an unknown energy source able to prolong their life for long periods of time
CitacióCamisassa, M. [et al.]. Forever young white dwarfs: When stellar ageing stops. "Astronomy & astrophysics", 1 Maig 2021, vol. 649, núm. L7, p. 1-5.
ISSN1432-0746
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