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Pair-Instability Supernovae, Gravity Waves, and Gamma-Ray Transients
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Growing theoretical evidence suggests that the first generation of stars may have been quite massive (~100-300 solar masses). If they retain their high mass until death, such stars will, after about 3Myr, make pair-instability supernovae. We consider the complete evolution of two zero-metallicity stars of 250 and 300 solar masses. Explosive oxygen and silicon burning cause the 130 solar mass helium core to explode, but explosive burning is unable to drive an explosion in the 300 solar mass star and it collapses to a black hole. For this star, the calculated angular momentum in the presupernova model is sufficient to delay black hole formation and the star initially forms a 50 solar mass, 1000km core within which neutrinos are trapped. Although the star does not become dynamically unstable, the calculated growth time of secular rotational instabilities is shorter than the black hole formation time, and such instabilities may develop. We estimate the energy and amplitude of the gravitational waves emitted during this collapse. After the black hole forms, accretion continues through a disk. Although the disk is far too large and cool to transport energy efficiently to the rotational axis by neutrino annihilation, it has ample potential energy to produce a 1e54erg jet driven by magnetic fields. The interaction of this jet with surrounding circumstellar gas may produce an energetic gamma-ray transient, but given the redshift and time scale, this is probably not a model for typical gamma-ray bursts.
Forward citations
Cited by 7 Pith papers
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Prospects for characterizing Population III remnants with next-generation gravitational-wave observatories
For an ET+CE network, loud Population III BBH mergers at z>15 can be confidently placed above z~12, masses measured to about 12 percent, but spin constraints remain weak.
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Searching for Population III stars with line intensity mapping cross-correlations
Adding Pop III stars to the oLIMpus analytical framework shows that only next-generation instruments can detect the H-alpha/HeII cross-correlation and constrain the first stars' IMF.
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Temperature-resolved sensitivities of $^{56}{\rm Ni}$ production to helium-burning reactions in pair-instability supernovae
Temperature-resolved Monte Carlo analysis of PISNe finds peak sensitivity of 56Ni production to triple-alpha and 12C(alpha,gamma)16O rates at T~2.5e8 K with opposite signs, tied to pre-carbon C/O ratio.
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Searching for intermediate mass ratio binary black hole mergers in the third observing run of LIGO-Virgo-KAGRA
No confident intermediate mass ratio inspirals are found in LIGO-Virgo-KAGRA O3 data, yielding 90% upper limits of roughly 30-1000 Gpc^-3 yr^-1 on their local merger rate and showing higher modes boost search volume b...
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Improving the detection significance of gravitational wave transient searches with CNN models
A CNN-based classifier applied to time-frequency images re-weights triggers from two PyCBC intermediate-mass black hole searches, improving their sensitive volume-time by about 30 percent at a false alarm rate of once...
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Eccentric Stellar-mass Binary Black Holes: Population, Detectability, and Waveform Analysis in the LISA and LIGO Era
Simulations of dynamically formed eccentric stellar-mass BBHs predict dozens of LISA-detectable sources in the Milky Way, hundreds of low-SNR extragalactic mHz sources, a merger rate of ~9 Gpc^{-3} yr^{-1}, and potent...
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Searching for binary black hole mergers with deep learning in Advanced LIGO's third observing run
A hybrid matched-filter/deep-learning pipeline recovers 31 known O3 events and reports a new tentative high-mass candidate, with sensitivity comparable to existing searches only for chirp masses above 25 solar masses.
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