Formation of GW190521 from stellar evolution: the impact of the hydrogen-rich envelope, dredge-up, and 12C(α, γ)16O rate on the pair-instability black hole mass gap
ABSTRACT Pair-instability (PI) is expected to open a gap in the mass spectrum of black holes (BHs) between ≈40–65 and ≈120 M⊙. The existence of the mass gap is currently being challenged by the detection of GW190521, with a primary component mass of $85^{+21}_{-14}$ M⊙. Here, we investigate the main...
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creator | Costa, Guglielmo Bressan, Alessandro Mapelli, Michela Marigo, Paola Iorio, Giuliano Spera, Mario |
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Pair-instability (PI) is expected to open a gap in the mass spectrum of black holes (BHs) between ≈40–65 and ≈120 M⊙. The existence of the mass gap is currently being challenged by the detection of GW190521, with a primary component mass of $85^{+21}_{-14}$ M⊙. Here, we investigate the main uncertainties on the PI mass gap: the 12C(α, γ)16O reaction rate and the H-rich envelope collapse. With the standard 12C(α, γ)16O rate, the lower edge of the mass gap can be 70 M⊙ if we allow for the collapse of the residual H-rich envelope at metallicity Z ≤ 0.0003. Adopting the uncertainties given by the starlib database, for models computed with the 12C(α, γ)16O rate $-1\, \sigma$, we find that the PI mass gap ranges between ≈80 and ≈150 M⊙. Stars with MZAMS > 110 M⊙ may experience a deep dredge-up episode during the core helium-burning phase, that extracts matter from the core enriching the envelope. As a consequence of the He-core mass reduction, a star with MZAMS = 160 M⊙ may avoid the PI and produce a BH of 150 M⊙. In the $-2\, {}\sigma {}$ case, the PI mass gap ranges from 92 to 110 M⊙. Finally, in models computed with 12C(α, γ)16O $-3\, {}\sigma {}$, the mass gap is completely removed by the dredge-up effect. The onset of this dredge-up is particularly sensitive to the assumed model for convection and mixing. The combined effect of H-rich envelope collapse and low 12C(α, γ)16O rate can lead to the formation of BHs with masses consistent with the primary component of GW190521. |
doi_str_mv | 10.1093/mnras/staa3916 |
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Pair-instability (PI) is expected to open a gap in the mass spectrum of black holes (BHs) between ≈40–65 and ≈120 M⊙. The existence of the mass gap is currently being challenged by the detection of GW190521, with a primary component mass of $85^{+21}_{-14}$ M⊙. Here, we investigate the main uncertainties on the PI mass gap: the 12C(α, γ)16O reaction rate and the H-rich envelope collapse. With the standard 12C(α, γ)16O rate, the lower edge of the mass gap can be 70 M⊙ if we allow for the collapse of the residual H-rich envelope at metallicity Z ≤ 0.0003. Adopting the uncertainties given by the starlib database, for models computed with the 12C(α, γ)16O rate $-1\, \sigma$, we find that the PI mass gap ranges between ≈80 and ≈150 M⊙. Stars with MZAMS > 110 M⊙ may experience a deep dredge-up episode during the core helium-burning phase, that extracts matter from the core enriching the envelope. As a consequence of the He-core mass reduction, a star with MZAMS = 160 M⊙ may avoid the PI and produce a BH of 150 M⊙. In the $-2\, {}\sigma {}$ case, the PI mass gap ranges from 92 to 110 M⊙. Finally, in models computed with 12C(α, γ)16O $-3\, {}\sigma {}$, the mass gap is completely removed by the dredge-up effect. The onset of this dredge-up is particularly sensitive to the assumed model for convection and mixing. The combined effect of H-rich envelope collapse and low 12C(α, γ)16O rate can lead to the formation of BHs with masses consistent with the primary component of GW190521.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/staa3916</identifier><language>eng</language><publisher>Oxford University Press</publisher><ispartof>Monthly notices of the Royal Astronomical Society, 2021-03, Vol.501 (3), p.4514-4533</ispartof><rights>2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society 2021</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c309t-5415a39636f1d3841d690f87c0ab8612bc63a9aeadeae8e80caa1153b2fda6e63</citedby><cites>FETCH-LOGICAL-c309t-5415a39636f1d3841d690f87c0ab8612bc63a9aeadeae8e80caa1153b2fda6e63</cites><orcidid>0000-0003-0293-503X ; 0000-0001-8799-2548 ; 0000-0003-0930-6930 ; 0000-0002-6213-6988</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,1598,27901,27902</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/staa3916$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Costa, Guglielmo</creatorcontrib><creatorcontrib>Bressan, Alessandro</creatorcontrib><creatorcontrib>Mapelli, Michela</creatorcontrib><creatorcontrib>Marigo, Paola</creatorcontrib><creatorcontrib>Iorio, Giuliano</creatorcontrib><creatorcontrib>Spera, Mario</creatorcontrib><title>Formation of GW190521 from stellar evolution: the impact of the hydrogen-rich envelope, dredge-up, and 12C(α, γ)16O rate on the pair-instability black hole mass gap</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
Pair-instability (PI) is expected to open a gap in the mass spectrum of black holes (BHs) between ≈40–65 and ≈120 M⊙. The existence of the mass gap is currently being challenged by the detection of GW190521, with a primary component mass of $85^{+21}_{-14}$ M⊙. Here, we investigate the main uncertainties on the PI mass gap: the 12C(α, γ)16O reaction rate and the H-rich envelope collapse. With the standard 12C(α, γ)16O rate, the lower edge of the mass gap can be 70 M⊙ if we allow for the collapse of the residual H-rich envelope at metallicity Z ≤ 0.0003. Adopting the uncertainties given by the starlib database, for models computed with the 12C(α, γ)16O rate $-1\, \sigma$, we find that the PI mass gap ranges between ≈80 and ≈150 M⊙. Stars with MZAMS > 110 M⊙ may experience a deep dredge-up episode during the core helium-burning phase, that extracts matter from the core enriching the envelope. As a consequence of the He-core mass reduction, a star with MZAMS = 160 M⊙ may avoid the PI and produce a BH of 150 M⊙. In the $-2\, {}\sigma {}$ case, the PI mass gap ranges from 92 to 110 M⊙. Finally, in models computed with 12C(α, γ)16O $-3\, {}\sigma {}$, the mass gap is completely removed by the dredge-up effect. The onset of this dredge-up is particularly sensitive to the assumed model for convection and mixing. The combined effect of H-rich envelope collapse and low 12C(α, γ)16O rate can lead to the formation of BHs with masses consistent with the primary component of GW190521.</description><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNqFkEFLw0AQhRdRsFavnudooWl3ss028SbFVqHQi-IxTJJJG02yYTcV-oe8i_-jv8nG6tnTMPC9N_OeENcoRygjNa5qS27sWiIVoT4RPVQ68PxI61PRk1IFXjhFPBcXzr1KKSfK1z3xMTe2orYwNZgcFi8YycBHyK2pwLVclmSB30257ZBbaDcMRdVQ2nZ4t212mTVrrj1bpBvg-p1L0_AQMsvZmr1tMwSqM0B_drP_HML-a4B6BZZahsPNzqGhwnpFfXg8Kcqi3UFSUvoGG1MyVOQcrKm5FGc5lY6vfmdfPM_vn2YP3nK1eJzdLb1Uyaj1ggkGh_Ra6RwzFU4w05HMw2kqKQk1-kmqFUXElDFxyKFMiRADlfh5Rpq16ovR0Te1xjnLedzYoiK7i1HGXcvxT8vxX8sHweAoMNvmP_Yb41-C9g</recordid><startdate>20210301</startdate><enddate>20210301</enddate><creator>Costa, Guglielmo</creator><creator>Bressan, Alessandro</creator><creator>Mapelli, Michela</creator><creator>Marigo, Paola</creator><creator>Iorio, Giuliano</creator><creator>Spera, Mario</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><orcidid>https://orcid.org/0000-0003-0293-503X</orcidid><orcidid>https://orcid.org/0000-0001-8799-2548</orcidid><orcidid>https://orcid.org/0000-0003-0930-6930</orcidid><orcidid>https://orcid.org/0000-0002-6213-6988</orcidid></search><sort><creationdate>20210301</creationdate><title>Formation of GW190521 from stellar evolution: the impact of the hydrogen-rich envelope, dredge-up, and 12C(α, γ)16O rate on the pair-instability black hole mass gap</title><author>Costa, Guglielmo ; Bressan, Alessandro ; Mapelli, Michela ; Marigo, Paola ; Iorio, Giuliano ; Spera, Mario</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c309t-5415a39636f1d3841d690f87c0ab8612bc63a9aeadeae8e80caa1153b2fda6e63</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Costa, Guglielmo</creatorcontrib><creatorcontrib>Bressan, Alessandro</creatorcontrib><creatorcontrib>Mapelli, Michela</creatorcontrib><creatorcontrib>Marigo, Paola</creatorcontrib><creatorcontrib>Iorio, Giuliano</creatorcontrib><creatorcontrib>Spera, Mario</creatorcontrib><collection>CrossRef</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Costa, Guglielmo</au><au>Bressan, Alessandro</au><au>Mapelli, Michela</au><au>Marigo, Paola</au><au>Iorio, Giuliano</au><au>Spera, Mario</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Formation of GW190521 from stellar evolution: the impact of the hydrogen-rich envelope, dredge-up, and 12C(α, γ)16O rate on the pair-instability black hole mass gap</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2021-03-01</date><risdate>2021</risdate><volume>501</volume><issue>3</issue><spage>4514</spage><epage>4533</epage><pages>4514-4533</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
Pair-instability (PI) is expected to open a gap in the mass spectrum of black holes (BHs) between ≈40–65 and ≈120 M⊙. The existence of the mass gap is currently being challenged by the detection of GW190521, with a primary component mass of $85^{+21}_{-14}$ M⊙. Here, we investigate the main uncertainties on the PI mass gap: the 12C(α, γ)16O reaction rate and the H-rich envelope collapse. With the standard 12C(α, γ)16O rate, the lower edge of the mass gap can be 70 M⊙ if we allow for the collapse of the residual H-rich envelope at metallicity Z ≤ 0.0003. Adopting the uncertainties given by the starlib database, for models computed with the 12C(α, γ)16O rate $-1\, \sigma$, we find that the PI mass gap ranges between ≈80 and ≈150 M⊙. Stars with MZAMS > 110 M⊙ may experience a deep dredge-up episode during the core helium-burning phase, that extracts matter from the core enriching the envelope. As a consequence of the He-core mass reduction, a star with MZAMS = 160 M⊙ may avoid the PI and produce a BH of 150 M⊙. In the $-2\, {}\sigma {}$ case, the PI mass gap ranges from 92 to 110 M⊙. Finally, in models computed with 12C(α, γ)16O $-3\, {}\sigma {}$, the mass gap is completely removed by the dredge-up effect. The onset of this dredge-up is particularly sensitive to the assumed model for convection and mixing. The combined effect of H-rich envelope collapse and low 12C(α, γ)16O rate can lead to the formation of BHs with masses consistent with the primary component of GW190521.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/staa3916</doi><tpages>20</tpages><orcidid>https://orcid.org/0000-0003-0293-503X</orcidid><orcidid>https://orcid.org/0000-0001-8799-2548</orcidid><orcidid>https://orcid.org/0000-0003-0930-6930</orcidid><orcidid>https://orcid.org/0000-0002-6213-6988</orcidid><oa>free_for_read</oa></addata></record> |
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title | Formation of GW190521 from stellar evolution: the impact of the hydrogen-rich envelope, dredge-up, and 12C(α, γ)16O rate on the pair-instability black hole mass gap |
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