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. Issue 3 (21st December 2020)

• Record Type: Journal Article
• Authors: Costa, Guglielmo; Bressan, Alessandro; Mapelli, Michela; Marigo, Paola; Iorio, Giuliano; Spera, Mario
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 501:Issue 3(2021)
• Page Start: 4514
• Page End: 4533
• Publication Date: 2020-12-21
• Subjects: convection -- stars: black holes -- stars: evolution -- stars: interiors -- stars: massive -- stars: mass-loss; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa3916
• Languages: English
• ISSNs: 0035-8711

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 12 C(α, γ) 16 O reaction rate and the H-rich envelope collapse. With the standard 12 C(α, γ) 16 O 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 12 C(α, γ) 16 O rate $-1\, \sigma$, we find that the PI mass gap ranges between ≈80 and ≈150 M⊙ . Stars with M ZAMS > 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 M ZAMS = 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 12 C(α, γ) 16 O $-3\, {}\sigma {}$, 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 12 C(α, γ) 16 O rate can lead to the formation of BHs with masses consistent with the primary component of GW190521.