The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars

Gaia's exquisite parallax measurements allowed for the discovery and characterization of the Q branch in the Hertzsprung–Russell diagram, where massive C/O white dwarfs (WDs) pause their dimming due to energy released during crystallization. Interestingly, the fraction of old stars on the Q bra...
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Autor*in:	Ken J. Shen [verfasserIn] Simon Blouin [verfasserIn] Katelyn Breivik [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Binary stars Cosmochronology Nucleosynthesis White dwarf stars

Übergeordnetes Werk:	In: The Astrophysical Journal Letters - IOP Publishing, 2022, 955(2023), 2, p L33
Übergeordnetes Werk:	volume:955 ; year:2023 ; number:2, p L33

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/2041-8213/acf57b

Katalog-ID:	DOAJ096663677

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source	In The Astrophysical Journal Letters 955(2023), 2, p L33 volume:955 year:2023 number:2, p L33
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format_phy_str_mv	Article
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topic_facet	Binary stars Cosmochronology Nucleosynthesis White dwarf stars Astrophysics
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container_title	The Astrophysical Journal Letters
authorswithroles_txt_mv	Ken J. Shen @@aut@@ Simon Blouin @@aut@@ Katelyn Breivik @@aut@@
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callnumber-first	Q - Science
author	Ken J. Shen
spellingShingle	Ken J. Shen misc QB460-466 misc Binary stars misc Cosmochronology misc Nucleosynthesis misc White dwarf stars misc Astrophysics The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars
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topic_title	QB460-466 The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars Binary stars Cosmochronology Nucleosynthesis White dwarf stars
topic	misc QB460-466 misc Binary stars misc Cosmochronology misc Nucleosynthesis misc White dwarf stars misc Astrophysics
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title	The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars
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title_sort	q branch cooling anomaly can be explained by mergers of white dwarfs and subgiant stars
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title_auth	The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars
abstract	Gaia's exquisite parallax measurements allowed for the discovery and characterization of the Q branch in the Hertzsprung–Russell diagram, where massive C/O white dwarfs (WDs) pause their dimming due to energy released during crystallization. Interestingly, the fraction of old stars on the Q branch is significantly higher than in the population of WDs that will become Q branch stars or that were Q branch stars in the past. From this, Cheng et al. inferred that ∼6% of WDs passing through the Q branch experience a much longer cooling delay than that of standard crystallizing WDs. Previous attempts to explain this cooling anomaly have invoked mechanisms involving supersolar initial metallicities. In this paper, we describe a novel scenario in which a standard composition WD merges with a subgiant star. The evolution of the resulting merger remnant leads to the creation of a large amount of ^26 Mg, which, along with the existing ^22 Ne, undergoes a distillation process that can release enough energy to explain the Q branch cooling problem without the need for atypical initial abundances. The anomalously high number of old stars on the Q branch may thus be evidence that mass transfer from subgiants to WDs leads to unstable mergers.
abstractGer	Gaia's exquisite parallax measurements allowed for the discovery and characterization of the Q branch in the Hertzsprung–Russell diagram, where massive C/O white dwarfs (WDs) pause their dimming due to energy released during crystallization. Interestingly, the fraction of old stars on the Q branch is significantly higher than in the population of WDs that will become Q branch stars or that were Q branch stars in the past. From this, Cheng et al. inferred that ∼6% of WDs passing through the Q branch experience a much longer cooling delay than that of standard crystallizing WDs. Previous attempts to explain this cooling anomaly have invoked mechanisms involving supersolar initial metallicities. In this paper, we describe a novel scenario in which a standard composition WD merges with a subgiant star. The evolution of the resulting merger remnant leads to the creation of a large amount of ^26 Mg, which, along with the existing ^22 Ne, undergoes a distillation process that can release enough energy to explain the Q branch cooling problem without the need for atypical initial abundances. The anomalously high number of old stars on the Q branch may thus be evidence that mass transfer from subgiants to WDs leads to unstable mergers.
abstract_unstemmed	Gaia's exquisite parallax measurements allowed for the discovery and characterization of the Q branch in the Hertzsprung–Russell diagram, where massive C/O white dwarfs (WDs) pause their dimming due to energy released during crystallization. Interestingly, the fraction of old stars on the Q branch is significantly higher than in the population of WDs that will become Q branch stars or that were Q branch stars in the past. From this, Cheng et al. inferred that ∼6% of WDs passing through the Q branch experience a much longer cooling delay than that of standard crystallizing WDs. Previous attempts to explain this cooling anomaly have invoked mechanisms involving supersolar initial metallicities. In this paper, we describe a novel scenario in which a standard composition WD merges with a subgiant star. The evolution of the resulting merger remnant leads to the creation of a large amount of ^26 Mg, which, along with the existing ^22 Ne, undergoes a distillation process that can release enough energy to explain the Q branch cooling problem without the need for atypical initial abundances. The anomalously high number of old stars on the Q branch may thus be evidence that mass transfer from subgiants to WDs leads to unstable mergers.
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title_short	The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars
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