Protostellar accretion in low mass metal poor stars and the cosmological lithium problem

Context.The cosmological lithium problem, that is, the discrepancy between the lithium abundance predicted by the Big Bang nucleosynthesis and the one observed for the stars of the "Spite plateau", is one of the long standing problems of modern astrophysics. Recent hints for a possible sol...

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Veröffentlicht in:Astronomy and astrophysics (Berlin) 2020-06, Vol.638, p.A81, Article 81
Hauptverfasser: Tognelli, Emanuele, Prada Moroni, Pier Giorgio, Degl'Innocenti, Scilla, Salaris, Maurizio, Cassisi, Santi
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container_title Astronomy and astrophysics (Berlin)
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creator Tognelli, Emanuele
Prada Moroni, Pier Giorgio
Degl'Innocenti, Scilla
Salaris, Maurizio
Cassisi, Santi
description Context.The cosmological lithium problem, that is, the discrepancy between the lithium abundance predicted by the Big Bang nucleosynthesis and the one observed for the stars of the "Spite plateau", is one of the long standing problems of modern astrophysics. Recent hints for a possible solution involve lithium burning induced by protostellar mass accretion on Spite plateau stars. However, to date, most of the protostellar and pre-main sequence stellar models that take mass accretion into account have been computed at solar metallicity, and a detailed analysis on the impact of protostellar accretion on the lithium evolution in the metal-poor regime, which is relevant for stars in the Spite plateau, is completely missing. Aims.The purpose of this paper is to fill this gap, analysing, in detail, for the first time the effect of protostellar accretion on low metallicity low-mass stars with a focus on pre-main sequence lithium evolution. Methods.We computed the evolution from the protostar to the main-sequence phase of accreting models with final masses equal to 0.7 and 0.8M(circle dot), and three metallicities Z = 0.0001, Z = 0.0010, and Z = 0.0050, corresponding to [Fe/H] similar to -2.1, -1.1 (typical of Spite plateau stars), and [Fe/H] similar to -0.42, respectively. We followed the temporal evolution of the chemical composition by considering nuclear burning, convective mixing, and diffusion. The effects of changing some of the main parameters affecting accreting models, that is the accretion energy (i.e. cold versus hot accretion), the initial seed mass M-seed and radius R-seed, and the mass accretion ratem(also considering episodic accretion), have been investigated in detail. Results.As for the main stellar properties and in particular the surface Li-7 abundance, hot accretion models converge to standard non-accreting ones within 1 Myr, regardless of the actual value of M-seed, R-seed, and m. Also, cold accretion models with a relatively large M-seed (greater than or similar to 10 M-J) or R-seed (greater than or similar to 1 R-circle dot) converge to standard non-accreting ones in less than about 10-20 Myr. However, a drastically different evolution occurs whenever a cold protostellar accretion process starts from small values of M-seed and R-seed (M-seed similar to 1M(J), R-seed less than or similar to 1 R-circle dot). These models almost entirely skip the standard Hayashi track evolution and deplete lithium before the end of the accretion phase. The e
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Recent hints for a possible solution involve lithium burning induced by protostellar mass accretion on Spite plateau stars. However, to date, most of the protostellar and pre-main sequence stellar models that take mass accretion into account have been computed at solar metallicity, and a detailed analysis on the impact of protostellar accretion on the lithium evolution in the metal-poor regime, which is relevant for stars in the Spite plateau, is completely missing. Aims.The purpose of this paper is to fill this gap, analysing, in detail, for the first time the effect of protostellar accretion on low metallicity low-mass stars with a focus on pre-main sequence lithium evolution. Methods.We computed the evolution from the protostar to the main-sequence phase of accreting models with final masses equal to 0.7 and 0.8M(circle dot), and three metallicities Z = 0.0001, Z = 0.0010, and Z = 0.0050, corresponding to [Fe/H] similar to -2.1, -1.1 (typical of Spite plateau stars), and [Fe/H] similar to -0.42, respectively. We followed the temporal evolution of the chemical composition by considering nuclear burning, convective mixing, and diffusion. The effects of changing some of the main parameters affecting accreting models, that is the accretion energy (i.e. cold versus hot accretion), the initial seed mass M-seed and radius R-seed, and the mass accretion ratem(also considering episodic accretion), have been investigated in detail. Results.As for the main stellar properties and in particular the surface Li-7 abundance, hot accretion models converge to standard non-accreting ones within 1 Myr, regardless of the actual value of M-seed, R-seed, and m. Also, cold accretion models with a relatively large M-seed (greater than or similar to 10 M-J) or R-seed (greater than or similar to 1 R-circle dot) converge to standard non-accreting ones in less than about 10-20 Myr. However, a drastically different evolution occurs whenever a cold protostellar accretion process starts from small values of M-seed and R-seed (M-seed similar to 1M(J), R-seed less than or similar to 1 R-circle dot). These models almost entirely skip the standard Hayashi track evolution and deplete lithium before the end of the accretion phase. The exact amount of depletion depends on the actual combination of the accretion parameters (m, M-seed, and R-seed), achieving in some cases the complete exhaustion of lithium in the whole star. Finally, the lithium evolution in models accounting for burst accretion episodes or for an initial hot accretion followed by a cold accretion phase closely resemble that of standard non-accreting ones. Conclusions.To significantly deplete lithium in low-mass metal poor stars by means of protostellar accretion, a cold accretion scenario starting from small initial M-seed and R-seed is required. Even in this extreme configuration leading to a non-standard evolution that misses almost entirely the standard Hayashi track, an unsatisfactory fine tuning of the parameters governing the accretion phase is required to deplete lithium in stars of different mass and metallicity - starting from the Big Bang nucleosynthesis abundance - in such a way as to produce the observed Spite plateau.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/201936723</identifier><language>eng</language><publisher>LES ULIS CEDEX A: Edp Sciences S A</publisher><subject>Abundance ; Astronomical models ; Astronomy &amp; Astrophysics ; Astrophysics ; Big bang cosmology ; Chemical composition ; Cold ; Cold starts ; Computation ; Convergence ; Depletion ; Deposition ; Diffusion effects ; Impact analysis ; Lithium ; Lithium isotopes ; Low mass stars ; Metallicity ; Nuclear fusion ; Nuclei (nuclear physics) ; Parameters ; Physical Sciences ; Pre-main sequence stars ; Protostars ; Science &amp; Technology ; Stellar evolution ; Stellar models</subject><ispartof>Astronomy and astrophysics (Berlin), 2020-06, Vol.638, p.A81, Article 81</ispartof><rights>Copyright EDP Sciences Jun 2020</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>true</woscitedreferencessubscribed><woscitedreferencescount>5</woscitedreferencescount><woscitedreferencesoriginalsourcerecordid>wos000546971800004</woscitedreferencesoriginalsourcerecordid><citedby>FETCH-LOGICAL-c322t-3df15d3d34d85f683fc87e22cc6834f8b4d8723d07d6ea4f6e91aa5f59b161e33</citedby><cites>FETCH-LOGICAL-c322t-3df15d3d34d85f683fc87e22cc6834f8b4d8723d07d6ea4f6e91aa5f59b161e33</cites><orcidid>0000-0001-5736-628X ; 0000-0001-5870-3735</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>315,781,785,3728,27929,27930,28253</link.rule.ids></links><search><creatorcontrib>Tognelli, Emanuele</creatorcontrib><creatorcontrib>Prada Moroni, Pier Giorgio</creatorcontrib><creatorcontrib>Degl'Innocenti, Scilla</creatorcontrib><creatorcontrib>Salaris, Maurizio</creatorcontrib><creatorcontrib>Cassisi, Santi</creatorcontrib><title>Protostellar accretion in low mass metal poor stars and the cosmological lithium problem</title><title>Astronomy and astrophysics (Berlin)</title><addtitle>ASTRON ASTROPHYS</addtitle><description>Context.The cosmological lithium problem, that is, the discrepancy between the lithium abundance predicted by the Big Bang nucleosynthesis and the one observed for the stars of the "Spite plateau", is one of the long standing problems of modern astrophysics. Recent hints for a possible solution involve lithium burning induced by protostellar mass accretion on Spite plateau stars. However, to date, most of the protostellar and pre-main sequence stellar models that take mass accretion into account have been computed at solar metallicity, and a detailed analysis on the impact of protostellar accretion on the lithium evolution in the metal-poor regime, which is relevant for stars in the Spite plateau, is completely missing. Aims.The purpose of this paper is to fill this gap, analysing, in detail, for the first time the effect of protostellar accretion on low metallicity low-mass stars with a focus on pre-main sequence lithium evolution. Methods.We computed the evolution from the protostar to the main-sequence phase of accreting models with final masses equal to 0.7 and 0.8M(circle dot), and three metallicities Z = 0.0001, Z = 0.0010, and Z = 0.0050, corresponding to [Fe/H] similar to -2.1, -1.1 (typical of Spite plateau stars), and [Fe/H] similar to -0.42, respectively. We followed the temporal evolution of the chemical composition by considering nuclear burning, convective mixing, and diffusion. The effects of changing some of the main parameters affecting accreting models, that is the accretion energy (i.e. cold versus hot accretion), the initial seed mass M-seed and radius R-seed, and the mass accretion ratem(also considering episodic accretion), have been investigated in detail. Results.As for the main stellar properties and in particular the surface Li-7 abundance, hot accretion models converge to standard non-accreting ones within 1 Myr, regardless of the actual value of M-seed, R-seed, and m. Also, cold accretion models with a relatively large M-seed (greater than or similar to 10 M-J) or R-seed (greater than or similar to 1 R-circle dot) converge to standard non-accreting ones in less than about 10-20 Myr. However, a drastically different evolution occurs whenever a cold protostellar accretion process starts from small values of M-seed and R-seed (M-seed similar to 1M(J), R-seed less than or similar to 1 R-circle dot). These models almost entirely skip the standard Hayashi track evolution and deplete lithium before the end of the accretion phase. The exact amount of depletion depends on the actual combination of the accretion parameters (m, M-seed, and R-seed), achieving in some cases the complete exhaustion of lithium in the whole star. Finally, the lithium evolution in models accounting for burst accretion episodes or for an initial hot accretion followed by a cold accretion phase closely resemble that of standard non-accreting ones. Conclusions.To significantly deplete lithium in low-mass metal poor stars by means of protostellar accretion, a cold accretion scenario starting from small initial M-seed and R-seed is required. Even in this extreme configuration leading to a non-standard evolution that misses almost entirely the standard Hayashi track, an unsatisfactory fine tuning of the parameters governing the accretion phase is required to deplete lithium in stars of different mass and metallicity - starting from the Big Bang nucleosynthesis abundance - in such a way as to produce the observed Spite plateau.</description><subject>Abundance</subject><subject>Astronomical models</subject><subject>Astronomy &amp; Astrophysics</subject><subject>Astrophysics</subject><subject>Big bang cosmology</subject><subject>Chemical composition</subject><subject>Cold</subject><subject>Cold starts</subject><subject>Computation</subject><subject>Convergence</subject><subject>Depletion</subject><subject>Deposition</subject><subject>Diffusion effects</subject><subject>Impact analysis</subject><subject>Lithium</subject><subject>Lithium isotopes</subject><subject>Low mass stars</subject><subject>Metallicity</subject><subject>Nuclear fusion</subject><subject>Nuclei (nuclear physics)</subject><subject>Parameters</subject><subject>Physical Sciences</subject><subject>Pre-main sequence stars</subject><subject>Protostars</subject><subject>Science &amp; Technology</subject><subject>Stellar evolution</subject><subject>Stellar models</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><sourceid>AOWDO</sourceid><recordid>eNqNkMtOxCAUhonRxHH0CdyQuDR1uJW2S9N4SybRhSbuCKXgMKFlBJqJby_NmFm74cDh-znhA-AaozuMSrxCCLGCU45XBOGG8orQE7DAjJICVYyfgsWROAcXMW7zkeCaLsDnW_DJx6SdkwFKpYJO1o_QjtD5PRxkjHDQSTq48z7AmGSIUI49TBsNlY-Dd_7LqnzvbNrYaYC74Dunh0twZqSL-uqvLsHH48N7-1ysX59e2vt1oSghqaC9wWVPe8r6ujS8pkbVlSZEqbxnpu5yP_-mR1XPtWSG6wZLWZqy6TDHmtIluDm8m-d-TzomsfVTGPNIQVhdYZJXnCl6oFTwMQZtxC7YQYYfgZGYFYpZkJgFiaPCnLo9pPa68yYqq0elj8mcKBlvKlyjOZzp-v90a5OcRbd-GhP9BS-qhSI</recordid><startdate>20200601</startdate><enddate>20200601</enddate><creator>Tognelli, Emanuele</creator><creator>Prada Moroni, Pier Giorgio</creator><creator>Degl'Innocenti, Scilla</creator><creator>Salaris, Maurizio</creator><creator>Cassisi, Santi</creator><general>Edp Sciences S A</general><general>EDP Sciences</general><scope>AOWDO</scope><scope>BLEPL</scope><scope>DTL</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0001-5736-628X</orcidid><orcidid>https://orcid.org/0000-0001-5870-3735</orcidid></search><sort><creationdate>20200601</creationdate><title>Protostellar accretion in low mass metal poor stars and the cosmological lithium problem</title><author>Tognelli, Emanuele ; Prada Moroni, Pier Giorgio ; Degl'Innocenti, Scilla ; Salaris, Maurizio ; Cassisi, Santi</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c322t-3df15d3d34d85f683fc87e22cc6834f8b4d8723d07d6ea4f6e91aa5f59b161e33</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Abundance</topic><topic>Astronomical models</topic><topic>Astronomy &amp; Astrophysics</topic><topic>Astrophysics</topic><topic>Big bang cosmology</topic><topic>Chemical composition</topic><topic>Cold</topic><topic>Cold starts</topic><topic>Computation</topic><topic>Convergence</topic><topic>Depletion</topic><topic>Deposition</topic><topic>Diffusion effects</topic><topic>Impact analysis</topic><topic>Lithium</topic><topic>Lithium isotopes</topic><topic>Low mass stars</topic><topic>Metallicity</topic><topic>Nuclear fusion</topic><topic>Nuclei (nuclear physics)</topic><topic>Parameters</topic><topic>Physical Sciences</topic><topic>Pre-main sequence stars</topic><topic>Protostars</topic><topic>Science &amp; Technology</topic><topic>Stellar evolution</topic><topic>Stellar models</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Tognelli, Emanuele</creatorcontrib><creatorcontrib>Prada Moroni, Pier Giorgio</creatorcontrib><creatorcontrib>Degl'Innocenti, Scilla</creatorcontrib><creatorcontrib>Salaris, Maurizio</creatorcontrib><creatorcontrib>Cassisi, Santi</creatorcontrib><collection>Web of Science - Science Citation Index Expanded - 2020</collection><collection>Web of Science Core Collection</collection><collection>Science Citation Index Expanded</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Tognelli, Emanuele</au><au>Prada Moroni, Pier Giorgio</au><au>Degl'Innocenti, Scilla</au><au>Salaris, Maurizio</au><au>Cassisi, Santi</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Protostellar accretion in low mass metal poor stars and the cosmological lithium problem</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><stitle>ASTRON ASTROPHYS</stitle><date>2020-06-01</date><risdate>2020</risdate><volume>638</volume><spage>A81</spage><pages>A81-</pages><artnum>81</artnum><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>Context.The cosmological lithium problem, that is, the discrepancy between the lithium abundance predicted by the Big Bang nucleosynthesis and the one observed for the stars of the "Spite plateau", is one of the long standing problems of modern astrophysics. Recent hints for a possible solution involve lithium burning induced by protostellar mass accretion on Spite plateau stars. However, to date, most of the protostellar and pre-main sequence stellar models that take mass accretion into account have been computed at solar metallicity, and a detailed analysis on the impact of protostellar accretion on the lithium evolution in the metal-poor regime, which is relevant for stars in the Spite plateau, is completely missing. Aims.The purpose of this paper is to fill this gap, analysing, in detail, for the first time the effect of protostellar accretion on low metallicity low-mass stars with a focus on pre-main sequence lithium evolution. Methods.We computed the evolution from the protostar to the main-sequence phase of accreting models with final masses equal to 0.7 and 0.8M(circle dot), and three metallicities Z = 0.0001, Z = 0.0010, and Z = 0.0050, corresponding to [Fe/H] similar to -2.1, -1.1 (typical of Spite plateau stars), and [Fe/H] similar to -0.42, respectively. We followed the temporal evolution of the chemical composition by considering nuclear burning, convective mixing, and diffusion. The effects of changing some of the main parameters affecting accreting models, that is the accretion energy (i.e. cold versus hot accretion), the initial seed mass M-seed and radius R-seed, and the mass accretion ratem(also considering episodic accretion), have been investigated in detail. Results.As for the main stellar properties and in particular the surface Li-7 abundance, hot accretion models converge to standard non-accreting ones within 1 Myr, regardless of the actual value of M-seed, R-seed, and m. Also, cold accretion models with a relatively large M-seed (greater than or similar to 10 M-J) or R-seed (greater than or similar to 1 R-circle dot) converge to standard non-accreting ones in less than about 10-20 Myr. However, a drastically different evolution occurs whenever a cold protostellar accretion process starts from small values of M-seed and R-seed (M-seed similar to 1M(J), R-seed less than or similar to 1 R-circle dot). These models almost entirely skip the standard Hayashi track evolution and deplete lithium before the end of the accretion phase. The exact amount of depletion depends on the actual combination of the accretion parameters (m, M-seed, and R-seed), achieving in some cases the complete exhaustion of lithium in the whole star. Finally, the lithium evolution in models accounting for burst accretion episodes or for an initial hot accretion followed by a cold accretion phase closely resemble that of standard non-accreting ones. Conclusions.To significantly deplete lithium in low-mass metal poor stars by means of protostellar accretion, a cold accretion scenario starting from small initial M-seed and R-seed is required. Even in this extreme configuration leading to a non-standard evolution that misses almost entirely the standard Hayashi track, an unsatisfactory fine tuning of the parameters governing the accretion phase is required to deplete lithium in stars of different mass and metallicity - starting from the Big Bang nucleosynthesis abundance - in such a way as to produce the observed Spite plateau.</abstract><cop>LES ULIS CEDEX A</cop><pub>Edp Sciences S A</pub><doi>10.1051/0004-6361/201936723</doi><tpages>18</tpages><orcidid>https://orcid.org/0000-0001-5736-628X</orcidid><orcidid>https://orcid.org/0000-0001-5870-3735</orcidid><oa>free_for_read</oa></addata></record>
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subjects Abundance
Astronomical models
Astronomy & Astrophysics
Astrophysics
Big bang cosmology
Chemical composition
Cold
Cold starts
Computation
Convergence
Depletion
Deposition
Diffusion effects
Impact analysis
Lithium
Lithium isotopes
Low mass stars
Metallicity
Nuclear fusion
Nuclei (nuclear physics)
Parameters
Physical Sciences
Pre-main sequence stars
Protostars
Science & Technology
Stellar evolution
Stellar models
title Protostellar accretion in low mass metal poor stars and the cosmological lithium problem
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