Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.
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9 Pith papers cite this work. Polarity classification is still indexing.
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Joint NICER+IXPE pulse-profile modeling of SRGA J144459.2-604207 favors large neutron-star mass and radius with two independent hotspots but shows strong sensitivity to joint-analysis methodology.
Multi-epoch observations of 1A 1246-588 show blackbody temperature rising from 0.28 to 0.39 keV with emitting radius 6.9-13.8 km and Comptonization photon index varying 1.8-2.3, consistent with atoll-state changes from accretion power redistribution.
A centered swept-back multipolar magnetic field up to octupole order reproduces the bolometric thermal X-ray light curve of MSP J0030+0451.
Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.
Deep Keck/NIRC2 adaptive optics imaging rules out a helium star companion to PSR J1928+1815, supporting a massive white dwarf with possible wind-driven eclipses.
A census of ~3600 variable compact radio sources at 3 GHz from VLASS epochs 1 and 2, with 5-9% showing >30% flux changes above 20-300 mJy and most consistent with blazars or quasars.
Observational case study of PSR J2338+4818 providing updated timing, single-pulse statistics from 27,228 detections, and scintillation parameters with no detected nulling.
Tidal deformability modeling for pulsar companions enables constraints on their equations of state by matching predicted orbital precession to timing data from four systems.
citing papers explorer
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Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions
Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.
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Pulse profile modelling of the 2024 outburst of the accreting millisecond pulsar SRGA J144459.2-604207
Joint NICER+IXPE pulse-profile modeling of SRGA J144459.2-604207 favors large neutron-star mass and radius with two independent hotspots but shows strong sensitivity to joint-analysis methodology.
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A NICER and AstroSat view of the neutron star low-mass X-ray binary 1A 1246-588
Multi-epoch observations of 1A 1246-588 show blackbody temperature rising from 0.28 to 0.39 keV with emitting radius 6.9-13.8 km and Comptonization photon index varying 1.8-2.3, consistent with atoll-state changes from accretion power redistribution.
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The swept-back multipolar magnetic field of neutron stars: Application to NICER MSP J0030+0451
A centered swept-back multipolar magnetic field up to octupole order reproduces the bolometric thermal X-ray light curve of MSP J0030+0451.
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Adiabatic Mass Loss In Binary Stars. VI. Massive Helium Binary Stars
Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.
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Deep Adaptive Optics Imaging Rules Out a Helium Star Companion to PSR J1928+1815
Deep Keck/NIRC2 adaptive optics imaging rules out a helium star companion to PSR J1928+1815, supporting a massive white dwarf with possible wind-driven eclipses.
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A Census of Variable Radio Sources at $3\,$GHz
A census of ~3600 variable compact radio sources at 3 GHz from VLASS epochs 1 and 2, with 5-9% showing >30% flux changes above 20-300 mJy and most consistent with blazars or quasars.
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A Pilot Study of Mildly Recycled Pulsars: A Case Study of PSR J2338+4818
Observational case study of PSR J2338+4818 providing updated timing, single-pulse statistics from 27,228 detections, and scintillation parameters with no detected nulling.
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What Are Pulsar Companions Made of? Using Gravitational Tides to Probe Their Compositions
Tidal deformability modeling for pulsar companions enables constraints on their equations of state by matching predicted orbital precession to timing data from four systems.