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Abstract The spin of a newly formed black hole (BH) at the center of a massive star evolves from its natal value due to two competing processes: accretion of gas angular momentum that increases the spin and extraction of BH angular momentum by outflows that decreases the spin. Ultimately, the final, equilibrium spin is set by a balance between both processes. In order for the BH to launch relativistic jets and power aγ-ray burst (GRB), the BH magnetic field needs to be dynamically important. Thus, we consider the case of a magnetically arrested disk (MAD) driving the spin evolution of the BH. By applying the semianalytic MAD BH spin evolution model of Lowell et al. to collapsars, we show that if the BH accretes ∼20% of its initial mass, its dimensionless spin inevitably reaches small values,a≲ 0.2. For such spins, and for mass accretion rates inferred from collapsar simulations, we show that our semianalytic model reproduces the energetics of typical GRB jets,Ljet∼ 1050erg s−1. We show that our semianalytic model reproduces the nearly constant power of typical GRB jets. If the MAD onset is delayed, this allows powerful jets at the high end of the GRB luminosity distribution,Ljet∼ 1052erg s−1, but the final spin remains low,a≲ 0.3. These results are consistent with the low spins inferred from gravitational wave detections of binary BH mergers. In a companion paper by Gottlieb et al., we use GRB observations to constrain the natal BH spin to bea≃ 0.2.
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Revised Estimates of Ocean Surface Drag in Strong Winds
Abstract Air‐sea drag governs the momentum transfer between the atmosphere and the ocean and remains largely unknown in hurricane winds. We revisit the momentum budget and eddy covariance methods to estimate the surface drag coefficient in the laboratory. Our drag estimates agree with field measurements in low‐to‐moderate winds and previous laboratory measurements in hurricane‐force winds. The drag coefficient saturates at 2.6×10−3andU10≈25 m s−1, in agreement with previous laboratory results by Takagaki et al. (2012,). During our analysis, we discovered an error in the original source code used by Donelan et al. (2004,). We present the corrected data and describe the correction procedure. Although the correction to the data does not change the key finding of drag saturation in strong winds, its magnitude and wind speed threshold are significantly changed. Our findings emphasize the need for an updated and unified drag parameterization based on field and laboratory data.
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- Award ID(s):
- 1745384
- PAR ID:
- 10447472
- Publisher / Repository:
- DOI PREFIX: 10.1029
- Date Published:
- Journal Name:
- Geophysical Research Letters
- Volume:
- 47
- Issue:
- 10
- ISSN:
- 0094-8276
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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