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? The black hole mass M and rotational energy E rot of formed after surge in centered nucleation, expressed relative to the mass M He of the progenitor He-star. The results are shown in cylindrical geometry (continuous) and spherical geometric (dashed). Note the broad distribution of high-mass black holes with large rotational energies of 5 ? 10% (spherical to cylindrical) of M He c 2 .
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We study the centered and decentered nucleation of black holes in the core collapse of massive stars in binaries. By Bekenstein's gravitational radiation recoil mechanism, a newly nucleated black hole typically leaves the central core prematurely. With low probability, the black hole remains centered and matures into a high-mass black hole that spi...
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Citations
... Finally, the dissipative photosphere model (Rees & Mészáros 2005;Pe'er et al. 2006;Giannios 2008;Beloborodov 2009;Lazzati & Begelman 2009;Ioka 2010;Toma et al. 2011;Ryde et al. 2011) attributes E p to the temperature of the photosphere. Naively, a quasi-thermal nature of emission generally calls for an intensity-tracking behavior, since hot temperature tends to be brighter. ...
We present a time-resolved spectral analysis of 51 long and 11 short bright gamma-ray bursts (GRBs) observed with the Fermi/Gamma-Ray Burst Monitor, paying special attention to E
p evolution within each burst. Among eight single-pulse long GRBs, five show an evolution from hard to soft, while three show intensity tracking. The multi-pulse long GRBs have more complicated patterns. Statistically, the hard-to-soft evolution pulses tend to be more asymmetric than the intensity-tracking ones, with a steeper rising wing than the falling wing. Short GRBs have E
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p evolution, as well as the possibility of a precessing jet in GRBs. The data pose a great challenge to each of these models, and hold the key to unveiling the physics behind GRB prompt emission.
The double neutron star (DNS) merger event GW170817 signifies the first multimessenger (MM) event with electromagnetic-gravitational (EM-GW) observations. LIGO-Virgo-KAGRA observational runs O4-5 promise to detect similar events and as yet unknown GW signals, which require confirmation in two or more detectors with comparable performance. To this end, we quantify duty cycles of comparable science quality of data in coincident H1L1-observations, further to seek consistent event rates of astrophysical transients in upcoming EM-GW surveys. Quite generally, discovery power scales with exposure time, sensitivity, and critically depends on the percentage of time when detectors operate at high quality. We quantify coincident duty cycles over a time-frequency domain W × B , defined by segments of duration W = 8 s, motivated by a long-duration descending GW-chirp during GRB170817A, and the minimum detector noise over about B = 100–250 Hz. This detector yield factor satisfies 1%–25% in S5-6 and O1-O3ab, significantly different from duty cycles of H1 and L1 individually with commensurable impact on consistency in event rates in EM-GW surveys. Significant gain in discovery power for signals whose frequency varies slowly in time may be derived from improving detector yield factors by deploying time-symmetric data analysis methods. For O4-5, these can yield improvements by factors up to ( 10 5 ) relative to existing data and methods. Furthermore, the diversity of MM afterglows to DNS mergers may be greatest for systems similar to GW170817 but possibly less so for systems of substantially different mass such as GW190425. We summarize our findings with an outlook on EM-GW surveys during O4-5 and perspectives for next-generation GRB missions like THESEUS .
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Multi-messenger emissions from SN1987A and GW170817/GRB170817A suggest a Universe rife with multi-messenger transients associated with black holes and neutron stars. For LIGO-Virgo, soon to be joined by KAGRA, these observations promise unprecedented opportunities to probe the central engines of core-collapse supernovae (CC-SNe) and gamma-ray bursts. Compared to neutron stars, central engines powered by black hole-disk or torus systems may be of particular interest to multi-messenger observations by the relatively large energy reservoir EJ of angular momentum, up to 29% of the total mass in the Kerr metric. These central engines are expected from relatively massive stellar progenitors and compact binary coalescence involving a neutron star. We review prospects of multi-messenger emission by catalytic conversion of EJ by a non-axisymmetric disk or torus. Observational support for this radiation process is found in a recent identification of \(\mathcal{E}\simeq (3.5\pm1)\% M_\odot c^{2}\) in Extended Emission to GW170817 at a significance of \( 4.2 \sigma\) concurrent with GRB170817A. A prospect on similar emissions from nearby CC-SNe justifies the need for all-sky blind searches of long duration bursts by heterogeneous computing.
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Black holes in core-collapse of massive stars are expected to surge in mass
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waves from non-axisymmetric accretion flows from fallback matter of the
progenitor envelope. It shows (a) a maximum efficiency in conversion of
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Upcoming gravitational wave observations may probe this scaling by extracting
broadband spectra using time-sliced matched filtering with chirp templates,
recently developed for identifying turbulence in noisy time series.
Extreme sources in the Transient Universe show evidence of relativistic outflows from intermittent inner engines, such as
cosmological gamma-ray bursts (GRBs). They probably derive from rotating back holes interacting with surrounding matter. We
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stars, it provides a robust explosion mechanism as a function of total energy output. At breakout, these ejecta may produce
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Observational evidence for black hole spin down has been found in the normalized light curves of long gamma-ray bursts in the BATSE catalog. Over the duration T90 of the burst, matter swept up by the central black hole is susceptible to nonaxisymmetries, producing gravitational radiation with a negative chirp. A time-sliced matched filtering method is introduced to capture phase coherence on intermediate time scales, τ, here tested by the injection of templates into experimental strain noise, hn(t). For TAMA 300, hn(f)≃10-21 Hz-1/2 at f=1 kHz gives a sensitivity distance for a reasonably accurate extraction of the trajectory in the time-frequency domain of about D≃0.07–0.10 Mpc for the spin down of black holes of mass M=10–12M⊙ with τ=1 s. Extrapolation to advanced detectors implies D≃35–50 Mpc for hn(f)≃2×10-24 Hz-1/2 around 1 kHz, which will open a new window to rigorous calorimetry on Kerr black holes.
Highly relativistic jets are a key element of current gamma‐ray burst (GRB) models, where the jet kinetic energy is converted to radiation energy at optically thin shocks. Mildly relativistic jets with smaller Lorentz factors are typically optically thick to gamma rays, and do not produce the spectacular GRB phenomenon. Jets which stall inside the progenitor similarly do not produce a GRB. However, various studies suggest that these jets are more common than GRB‐producing jets. Here we report on our study of high‐energy neutrino emission from these hidden jets. We describe the detection prospects with near‐future neutrino detectors, and discuss how the presence of jets can be studied with neutrinos. The neutrino horizon for hidden jets is of order 10 Mpc, a volume which contains at least a few supernova per year.
