期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 466, 期 1, 页码 1052-1060出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw3126
关键词
stars: black holes; stars: early-type; stars: evolution; stars: magnetic field; stars: massive; stars: mass-loss
资金
- National Aeronautics and Space Administration through Chandra Award [GO3-14017A]
- National Aeronautics Space Administration [NAS8-03060]
- NASA through a grant from the Space Telescope Science Institute [HST-GO-13734.011-A]
- NASA [NAS8-03060, NAS 5-26555]
- Chandra Award [TM4-15001B]
- NSF SI2 [ACI-1339600]
- NASA TCAN grant [NNX14AB55G]
- Natural Sciences and Engineering Research Council (NSERC) of Canada
- NASA through Chandra Award [GO5-16005X, AR6-17002C, G06-17007B, 18200020]
- NASA [686682, NNX14AB55G] Funding Source: Federal RePORTER
- Office of Advanced Cyberinfrastructure (OAC)
- Direct For Computer & Info Scie & Enginr [1339606] Funding Source: National Science Foundation
The groundbreaking detection of gravitational waves produced by the inspiralling and coalescence of the black hole (BH) binary GW150914 confirms the existence of 'heavy' stellar-mass BHs with masses >25 M-circle dot. Initial characterization of the system by Abbott et al. supposes that the formation of BHs with such large masses from the evolution of single massive stars is only feasible if the wind mass-loss rates of the progenitors were greatly reduced relative to the mass-loss rates of massive stars in the Galaxy, concluding that heavy BHs must form in low-metallicity (Z less than or similar to 0.25-0.5Z(circle dot)) environments. However, strong surface magnetic fields also provide a powerful mechanism for modifying mass-loss and rotation of massive stars, independent of environmental metallicity. In this paper, we explore the hypothesis that some heavy BHs, with masses > 25M(circle dot) such as those inferred to compose GW150914, could be the natural end-point of evolution of magnetic massive stars in a solar-metallicity environment. Using the MESA code, we developed a new grid of single, non-rotating, solar-metallicity evolutionary models for initial zero-age main sequence masses from 40 to 80M(circle dot) that include, for the first time, the quenching of the mass-loss due to a realistic dipolar surface magnetic field. The new models predict terminal-age main-sequence (TAMS) masses that are significantly greater than those from equivalent non-magnetic models, reducing the total mass lost by a strongly magnetized 80M(circle dot) star during its main-sequence evolution by 20M(circle dot). This corresponds approximately to the mass-loss reduction expected from an environment with metallicity Z = 1/30 Z(circle dot).
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