Solar Evolution Models with a Central Black Hole

Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter pr...
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Autor*in:	Earl P. Bellinger [verfasserIn] Matt E. Caplan [verfasserIn] Taeho Ryu [verfasserIn] Deepika Bollimpalli [verfasserIn] Warrick H. Ball [verfasserIn] Florian Kühnel [verfasserIn] R. Farmer [verfasserIn] S. E. de Mink [verfasserIn] Jørgen Christensen-Dalsgaard [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Stellar evolution Primordial black holes Dark matter

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 959(2023), 2, p 113
Übergeordnetes Werk:	volume:959 ; year:2023 ; number:2, p 113

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/ad04de

Katalog-ID:	DOAJ099303884

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allfields	10.3847/1538-4357/ad04de doi (DE-627)DOAJ099303884 (DE-599)DOAJa421c3f39dcc4332b7c897950ddde847 DE-627 ger DE-627 rakwb eng QB460-466 Earl P. Bellinger verfasserin aut Solar Evolution Models with a Central Black Hole 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter problem, and could grow to become stellar-mass BHs if captured by stars. Here we compute the evolution of stars having such a BH at their center. We find that such objects can be surprisingly long-lived, with the lightest BHs having no influence over stellar evolution, while more massive ones consume the star over time to produce a range of observable consequences. Models of the Sun born about a BH whose mass has since grown to approximately 10 ^−6 M _⊙ are compatible with current observations. In this scenario, the Sun would first dim to half its current luminosity over a span of 100 Myr as the accretion starts to generate enough energy to quench nuclear reactions. The Sun would then expand into a fully convective star, where it would shine luminously for potentially several gigayears with an enriched surface helium abundance, first as a sub-subgiant star, and later as a red straggler, before becoming a subsolar-mass BH. We also present results for a range of stellar masses and metallicities. The unique internal structures of stars harboring BHs may make it possible for asteroseismology to discover them, should they exist. We conclude with a list of open problems and predictions. Stellar evolution Primordial black holes Dark matter Astrophysics Matt E. Caplan verfasserin aut Taeho Ryu verfasserin aut Deepika Bollimpalli verfasserin aut Warrick H. Ball verfasserin aut Florian Kühnel verfasserin aut R. Farmer verfasserin aut S. E. de Mink verfasserin aut Jørgen Christensen-Dalsgaard verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 959(2023), 2, p 113 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:959 year:2023 number:2, p 113 https://doi.org/10.3847/1538-4357/ad04de kostenfrei https://doaj.org/article/a421c3f39dcc4332b7c897950ddde847 kostenfrei https://doi.org/10.3847/1538-4357/ad04de kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 959 2023 2, p 113
spelling	10.3847/1538-4357/ad04de doi (DE-627)DOAJ099303884 (DE-599)DOAJa421c3f39dcc4332b7c897950ddde847 DE-627 ger DE-627 rakwb eng QB460-466 Earl P. Bellinger verfasserin aut Solar Evolution Models with a Central Black Hole 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter problem, and could grow to become stellar-mass BHs if captured by stars. Here we compute the evolution of stars having such a BH at their center. We find that such objects can be surprisingly long-lived, with the lightest BHs having no influence over stellar evolution, while more massive ones consume the star over time to produce a range of observable consequences. Models of the Sun born about a BH whose mass has since grown to approximately 10 ^−6 M _⊙ are compatible with current observations. In this scenario, the Sun would first dim to half its current luminosity over a span of 100 Myr as the accretion starts to generate enough energy to quench nuclear reactions. The Sun would then expand into a fully convective star, where it would shine luminously for potentially several gigayears with an enriched surface helium abundance, first as a sub-subgiant star, and later as a red straggler, before becoming a subsolar-mass BH. We also present results for a range of stellar masses and metallicities. The unique internal structures of stars harboring BHs may make it possible for asteroseismology to discover them, should they exist. We conclude with a list of open problems and predictions. Stellar evolution Primordial black holes Dark matter Astrophysics Matt E. Caplan verfasserin aut Taeho Ryu verfasserin aut Deepika Bollimpalli verfasserin aut Warrick H. Ball verfasserin aut Florian Kühnel verfasserin aut R. Farmer verfasserin aut S. E. de Mink verfasserin aut Jørgen Christensen-Dalsgaard verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 959(2023), 2, p 113 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:959 year:2023 number:2, p 113 https://doi.org/10.3847/1538-4357/ad04de kostenfrei https://doaj.org/article/a421c3f39dcc4332b7c897950ddde847 kostenfrei https://doi.org/10.3847/1538-4357/ad04de kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 959 2023 2, p 113
allfields_unstemmed	10.3847/1538-4357/ad04de doi (DE-627)DOAJ099303884 (DE-599)DOAJa421c3f39dcc4332b7c897950ddde847 DE-627 ger DE-627 rakwb eng QB460-466 Earl P. Bellinger verfasserin aut Solar Evolution Models with a Central Black Hole 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter problem, and could grow to become stellar-mass BHs if captured by stars. Here we compute the evolution of stars having such a BH at their center. We find that such objects can be surprisingly long-lived, with the lightest BHs having no influence over stellar evolution, while more massive ones consume the star over time to produce a range of observable consequences. Models of the Sun born about a BH whose mass has since grown to approximately 10 ^−6 M _⊙ are compatible with current observations. In this scenario, the Sun would first dim to half its current luminosity over a span of 100 Myr as the accretion starts to generate enough energy to quench nuclear reactions. The Sun would then expand into a fully convective star, where it would shine luminously for potentially several gigayears with an enriched surface helium abundance, first as a sub-subgiant star, and later as a red straggler, before becoming a subsolar-mass BH. We also present results for a range of stellar masses and metallicities. The unique internal structures of stars harboring BHs may make it possible for asteroseismology to discover them, should they exist. We conclude with a list of open problems and predictions. Stellar evolution Primordial black holes Dark matter Astrophysics Matt E. Caplan verfasserin aut Taeho Ryu verfasserin aut Deepika Bollimpalli verfasserin aut Warrick H. Ball verfasserin aut Florian Kühnel verfasserin aut R. Farmer verfasserin aut S. E. de Mink verfasserin aut Jørgen Christensen-Dalsgaard verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 959(2023), 2, p 113 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:959 year:2023 number:2, p 113 https://doi.org/10.3847/1538-4357/ad04de kostenfrei https://doaj.org/article/a421c3f39dcc4332b7c897950ddde847 kostenfrei https://doi.org/10.3847/1538-4357/ad04de kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 959 2023 2, p 113
allfieldsGer	10.3847/1538-4357/ad04de doi (DE-627)DOAJ099303884 (DE-599)DOAJa421c3f39dcc4332b7c897950ddde847 DE-627 ger DE-627 rakwb eng QB460-466 Earl P. Bellinger verfasserin aut Solar Evolution Models with a Central Black Hole 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter problem, and could grow to become stellar-mass BHs if captured by stars. Here we compute the evolution of stars having such a BH at their center. We find that such objects can be surprisingly long-lived, with the lightest BHs having no influence over stellar evolution, while more massive ones consume the star over time to produce a range of observable consequences. Models of the Sun born about a BH whose mass has since grown to approximately 10 ^−6 M _⊙ are compatible with current observations. In this scenario, the Sun would first dim to half its current luminosity over a span of 100 Myr as the accretion starts to generate enough energy to quench nuclear reactions. The Sun would then expand into a fully convective star, where it would shine luminously for potentially several gigayears with an enriched surface helium abundance, first as a sub-subgiant star, and later as a red straggler, before becoming a subsolar-mass BH. We also present results for a range of stellar masses and metallicities. The unique internal structures of stars harboring BHs may make it possible for asteroseismology to discover them, should they exist. We conclude with a list of open problems and predictions. Stellar evolution Primordial black holes Dark matter Astrophysics Matt E. Caplan verfasserin aut Taeho Ryu verfasserin aut Deepika Bollimpalli verfasserin aut Warrick H. Ball verfasserin aut Florian Kühnel verfasserin aut R. Farmer verfasserin aut S. E. de Mink verfasserin aut Jørgen Christensen-Dalsgaard verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 959(2023), 2, p 113 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:959 year:2023 number:2, p 113 https://doi.org/10.3847/1538-4357/ad04de kostenfrei https://doaj.org/article/a421c3f39dcc4332b7c897950ddde847 kostenfrei https://doi.org/10.3847/1538-4357/ad04de kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 959 2023 2, p 113
allfieldsSound	10.3847/1538-4357/ad04de doi (DE-627)DOAJ099303884 (DE-599)DOAJa421c3f39dcc4332b7c897950ddde847 DE-627 ger DE-627 rakwb eng QB460-466 Earl P. Bellinger verfasserin aut Solar Evolution Models with a Central Black Hole 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter problem, and could grow to become stellar-mass BHs if captured by stars. Here we compute the evolution of stars having such a BH at their center. We find that such objects can be surprisingly long-lived, with the lightest BHs having no influence over stellar evolution, while more massive ones consume the star over time to produce a range of observable consequences. Models of the Sun born about a BH whose mass has since grown to approximately 10 ^−6 M _⊙ are compatible with current observations. In this scenario, the Sun would first dim to half its current luminosity over a span of 100 Myr as the accretion starts to generate enough energy to quench nuclear reactions. The Sun would then expand into a fully convective star, where it would shine luminously for potentially several gigayears with an enriched surface helium abundance, first as a sub-subgiant star, and later as a red straggler, before becoming a subsolar-mass BH. We also present results for a range of stellar masses and metallicities. The unique internal structures of stars harboring BHs may make it possible for asteroseismology to discover them, should they exist. We conclude with a list of open problems and predictions. Stellar evolution Primordial black holes Dark matter Astrophysics Matt E. Caplan verfasserin aut Taeho Ryu verfasserin aut Deepika Bollimpalli verfasserin aut Warrick H. Ball verfasserin aut Florian Kühnel verfasserin aut R. Farmer verfasserin aut S. E. de Mink verfasserin aut Jørgen Christensen-Dalsgaard verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 959(2023), 2, p 113 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:959 year:2023 number:2, p 113 https://doi.org/10.3847/1538-4357/ad04de kostenfrei https://doaj.org/article/a421c3f39dcc4332b7c897950ddde847 kostenfrei https://doi.org/10.3847/1538-4357/ad04de kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 959 2023 2, p 113
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source	In The Astrophysical Journal 959(2023), 2, p 113 volume:959 year:2023 number:2, p 113
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author	Earl P. Bellinger
spellingShingle	Earl P. Bellinger misc QB460-466 misc Stellar evolution misc Primordial black holes misc Dark matter misc Astrophysics Solar Evolution Models with a Central Black Hole
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title	Solar Evolution Models with a Central Black Hole
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abstract	Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter problem, and could grow to become stellar-mass BHs if captured by stars. Here we compute the evolution of stars having such a BH at their center. We find that such objects can be surprisingly long-lived, with the lightest BHs having no influence over stellar evolution, while more massive ones consume the star over time to produce a range of observable consequences. Models of the Sun born about a BH whose mass has since grown to approximately 10 ^−6 M _⊙ are compatible with current observations. In this scenario, the Sun would first dim to half its current luminosity over a span of 100 Myr as the accretion starts to generate enough energy to quench nuclear reactions. The Sun would then expand into a fully convective star, where it would shine luminously for potentially several gigayears with an enriched surface helium abundance, first as a sub-subgiant star, and later as a red straggler, before becoming a subsolar-mass BH. We also present results for a range of stellar masses and metallicities. The unique internal structures of stars harboring BHs may make it possible for asteroseismology to discover them, should they exist. We conclude with a list of open problems and predictions.
abstractGer	Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter problem, and could grow to become stellar-mass BHs if captured by stars. Here we compute the evolution of stars having such a BH at their center. We find that such objects can be surprisingly long-lived, with the lightest BHs having no influence over stellar evolution, while more massive ones consume the star over time to produce a range of observable consequences. Models of the Sun born about a BH whose mass has since grown to approximately 10 ^−6 M _⊙ are compatible with current observations. In this scenario, the Sun would first dim to half its current luminosity over a span of 100 Myr as the accretion starts to generate enough energy to quench nuclear reactions. The Sun would then expand into a fully convective star, where it would shine luminously for potentially several gigayears with an enriched surface helium abundance, first as a sub-subgiant star, and later as a red straggler, before becoming a subsolar-mass BH. We also present results for a range of stellar masses and metallicities. The unique internal structures of stars harboring BHs may make it possible for asteroseismology to discover them, should they exist. We conclude with a list of open problems and predictions.
abstract_unstemmed	Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter problem, and could grow to become stellar-mass BHs if captured by stars. Here we compute the evolution of stars having such a BH at their center. We find that such objects can be surprisingly long-lived, with the lightest BHs having no influence over stellar evolution, while more massive ones consume the star over time to produce a range of observable consequences. Models of the Sun born about a BH whose mass has since grown to approximately 10 ^−6 M _⊙ are compatible with current observations. In this scenario, the Sun would first dim to half its current luminosity over a span of 100 Myr as the accretion starts to generate enough energy to quench nuclear reactions. The Sun would then expand into a fully convective star, where it would shine luminously for potentially several gigayears with an enriched surface helium abundance, first as a sub-subgiant star, and later as a red straggler, before becoming a subsolar-mass BH. We also present results for a range of stellar masses and metallicities. The unique internal structures of stars harboring BHs may make it possible for asteroseismology to discover them, should they exist. We conclude with a list of open problems and predictions.
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title_short	Solar Evolution Models with a Central Black Hole
url	https://doi.org/10.3847/1538-4357/ad04de https://doaj.org/article/a421c3f39dcc4332b7c897950ddde847 https://doaj.org/toc/1538-4357
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