Critical Metallicity of Cool Supergiant Formation. I. Effects on Stellar-mass Loss and Feedback

This paper systematically studies the relation between metallicity and mass loss of massive stars. We perform one-dimensional stellar evolution simulations and build a grid of ∼2000 models with initial masses ranging between 11 and 60 M _⊙ and absolute metallicities Z between 0.00001 and 0.02. Stead...
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Autor*in:	Po-Sheng Ou [verfasserIn] Ke-Jung Chen [verfasserIn] You-Hua Chu [verfasserIn] Sung-Han Tsai [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Stellar mass loss Massive stars Late-type supergiant stars Metallicity

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 944(2023), 1, p 34
Übergeordnetes Werk:	volume:944 ; year:2023 ; number:1, p 34

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/aca96e

Katalog-ID:	DOAJ089166728

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source	In The Astrophysical Journal 944(2023), 1, p 34 volume:944 year:2023 number:1, p 34
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callnumber-first	Q - Science
author	Po-Sheng Ou
spellingShingle	Po-Sheng Ou misc QB460-466 misc Stellar mass loss misc Massive stars misc Late-type supergiant stars misc Metallicity misc Astrophysics Critical Metallicity of Cool Supergiant Formation. I. Effects on Stellar-mass Loss and Feedback
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topic_title	QB460-466 Critical Metallicity of Cool Supergiant Formation. I. Effects on Stellar-mass Loss and Feedback Stellar mass loss Massive stars Late-type supergiant stars Metallicity
topic	misc QB460-466 misc Stellar mass loss misc Massive stars misc Late-type supergiant stars misc Metallicity misc Astrophysics
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title	Critical Metallicity of Cool Supergiant Formation. I. Effects on Stellar-mass Loss and Feedback
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title_sort	critical metallicity of cool supergiant formation. i. effects on stellar-mass loss and feedback
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title_auth	Critical Metallicity of Cool Supergiant Formation. I. Effects on Stellar-mass Loss and Feedback
abstract	This paper systematically studies the relation between metallicity and mass loss of massive stars. We perform one-dimensional stellar evolution simulations and build a grid of ∼2000 models with initial masses ranging between 11 and 60 M _⊙ and absolute metallicities Z between 0.00001 and 0.02. Steady-state winds, comprising hot main-sequence winds and cool supergiant winds, are the main drivers of the mass loss of massive stars in our models. We calculate the total mass loss over the stellar lifetime for each model. Our results reveal the existence of a critical metallicity Z _c at Z ∼ 10 ^−3 , where the mass loss exhibits a dramatic jump. If Z < Z _c , massive stars tend to evolve into cool supergiants, and a robust cool wind is operational. In contrast, if Z < Z _c , massive stars usually remain as blue supergiants, wherein the cool wind is not activated and the mass loss is generally weak. Moreover, we calculate the wind feedback in a 10 ^5 M _⊙ star cluster with the Salpeter initial mass function. The kinetic energy released by winds does not exhibit any significant transition at Z _c because the wind velocity of a cool supergiant wind is low and contributes little to the kinetic energy. The effects of critical metallicity provide implications for the fates of metal-poor stars in the early universe.
abstractGer	This paper systematically studies the relation between metallicity and mass loss of massive stars. We perform one-dimensional stellar evolution simulations and build a grid of ∼2000 models with initial masses ranging between 11 and 60 M _⊙ and absolute metallicities Z between 0.00001 and 0.02. Steady-state winds, comprising hot main-sequence winds and cool supergiant winds, are the main drivers of the mass loss of massive stars in our models. We calculate the total mass loss over the stellar lifetime for each model. Our results reveal the existence of a critical metallicity Z _c at Z ∼ 10 ^−3 , where the mass loss exhibits a dramatic jump. If Z < Z _c , massive stars tend to evolve into cool supergiants, and a robust cool wind is operational. In contrast, if Z < Z _c , massive stars usually remain as blue supergiants, wherein the cool wind is not activated and the mass loss is generally weak. Moreover, we calculate the wind feedback in a 10 ^5 M _⊙ star cluster with the Salpeter initial mass function. The kinetic energy released by winds does not exhibit any significant transition at Z _c because the wind velocity of a cool supergiant wind is low and contributes little to the kinetic energy. The effects of critical metallicity provide implications for the fates of metal-poor stars in the early universe.
abstract_unstemmed	This paper systematically studies the relation between metallicity and mass loss of massive stars. We perform one-dimensional stellar evolution simulations and build a grid of ∼2000 models with initial masses ranging between 11 and 60 M _⊙ and absolute metallicities Z between 0.00001 and 0.02. Steady-state winds, comprising hot main-sequence winds and cool supergiant winds, are the main drivers of the mass loss of massive stars in our models. We calculate the total mass loss over the stellar lifetime for each model. Our results reveal the existence of a critical metallicity Z _c at Z ∼ 10 ^−3 , where the mass loss exhibits a dramatic jump. If Z < Z _c , massive stars tend to evolve into cool supergiants, and a robust cool wind is operational. In contrast, if Z < Z _c , massive stars usually remain as blue supergiants, wherein the cool wind is not activated and the mass loss is generally weak. Moreover, we calculate the wind feedback in a 10 ^5 M _⊙ star cluster with the Salpeter initial mass function. The kinetic energy released by winds does not exhibit any significant transition at Z _c because the wind velocity of a cool supergiant wind is low and contributes little to the kinetic energy. The effects of critical metallicity provide implications for the fates of metal-poor stars in the early universe.
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title_short	Critical Metallicity of Cool Supergiant Formation. I. Effects on Stellar-mass Loss and Feedback
url	https://doi.org/10.3847/1538-4357/aca96e https://doaj.org/article/80f6613151d54cc98c1cba2e8c539f81 https://doaj.org/toc/1538-4357
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Critical Metallicity of Cool Supergiant Formation. I. Effects on Stellar-mass Loss and Feedback

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