First public GPU-accelerated pulse-profile modeling code for X-ray millisecond pulsars that delivers 10^3–10^4 speedups to 2–5 ms per evaluation at 10^{-3} relative accuracy and removes an interpolation bias in atmosphere tables.
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T., Fonseca , E., Ransom , S
14 Pith papers cite this work. Polarity classification is still indexing.
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Detection of GW190814 from the coalescence of a 23 solar-mass black hole and a 2.6 solar-mass compact object, the most unequal-mass binary yet observed with gravitational waves.
A PCA-based generalization of template matching corrects jitter noise in pulsar TOA measurements by modeling pulse shape variations.
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.
Enhanced AML via L2-point mass loss in the RLOF channel alters ELM WD internal structure and mass-radius relation, reproducing observed shorter orbital periods.
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.
Bayesian EOS inference with χEFT uncertainty priors and LIGO/NICER data yields posteriors consistent with prior work, a stiffening above 3n0, negligible pQCD impact, and an inferred symmetry-energy slope L of 42.6-56.7 MeV.
A centered swept-back multipolar magnetic field up to octupole order reproduces the bolometric thermal X-ray light curve of MSP J0030+0451.
A Bayesian combination of eight M-R posteriors for PSR J0030+0451 yields M = 1.46^{+0.09}_{-0.08} M_⊙, R = 12.69^{+0.64}_{-0.55} km while marginalizing over unknown model systematics.
Reports timing solutions and basic properties for 49 pulsars (18 new) from the AO327 survey, with emission feature notes and model comparisons for distances.
The single Λ hyperon quasiparticle in nuclear matter at saturation density has energy -29.55 MeV at zero momentum, residue 0.98, and effective mass ratio 0.747.
An extended linear sigma model with delta meson and negative sigma_piN produces a symmetry-energy plateau and stiffer EOS that satisfies neutron-star and nuclear constraints.
Neutron star observations, especially the heaviest known pulsar masses and GW170817 tidal deformability, provide the strongest restrictions on the allowed cold dense matter equation of state.
citing papers explorer
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GPU-Accelerated X-ray Pulse Profile Modeling
First public GPU-accelerated pulse-profile modeling code for X-ray millisecond pulsars that delivers 10^3–10^4 speedups to 2–5 ms per evaluation at 10^{-3} relative accuracy and removes an interpolation bias in atmosphere tables.
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GW190814: Gravitational Waves from the Coalescence of a 23 M$_\odot$ Black Hole with a 2.6 M$_\odot$ Compact Object
Detection of GW190814 from the coalescence of a 23 solar-mass black hole and a 2.6 solar-mass compact object, the most unequal-mass binary yet observed with gravitational waves.
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A Generalized Template Matching Algorithm for Correcting Jitter Noise in Pulsar Timing
A PCA-based generalization of template matching corrects jitter noise in pulsar TOA measurements by modeling pulse shape variations.
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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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Formation of extremely low-mass white dwarf binaries undergoing enhanced angular momentum loss
Enhanced AML via L2-point mass loss in the RLOF channel alters ELM WD internal structure and mass-radius relation, reproducing observed shorter orbital periods.
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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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Astrophysics equation of state inference with Bayesian chiral effective field theory uncertainties
Bayesian EOS inference with χEFT uncertainty priors and LIGO/NICER data yields posteriors consistent with prior work, a stiffening above 3n0, negligible pQCD impact, and an inferred symmetry-energy slope L of 42.6-56.7 MeV.
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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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Combining the Mass--Radius Posteriors of J0030+0451 Allowing for Unknown Model Systematics
A Bayesian combination of eight M-R posteriors for PSR J0030+0451 yields M = 1.46^{+0.09}_{-0.08} M_⊙, R = 12.69^{+0.64}_{-0.55} km while marginalizing over unknown model systematics.
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Discovery and Timing of 49 Pulsars from the Arecibo 327-MHz Drift Survey
Reports timing solutions and basic properties for 49 pulsars (18 new) from the AO327 survey, with emission feature notes and model comparisons for distances.
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Quasiparticle properties of a single $\Lambda$ impurity in symmetric nuclear matter with a regulated $N\Lambda$ interaction
The single Λ hyperon quasiparticle in nuclear matter at saturation density has energy -29.55 MeV at zero momentum, residue 0.98, and effective mass ratio 0.747.
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Nuclear matter properties and neutron star structures from an extended linear sigma model
An extended linear sigma model with delta meson and negative sigma_piN produces a symmetry-energy plateau and stiffer EOS that satisfies neutron-star and nuclear constraints.
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Astrophysical constraints on the cold equation of state of the strongly interacting matter
Neutron star observations, especially the heaviest known pulsar masses and GW170817 tidal deformability, provide the strongest restrictions on the allowed cold dense matter equation of state.
- Eccentricity as a signature of hierarchical subsolar-mass mergers in collapsar disks