2D disc simulations with vertical volatile transport produce stable CO snow surface equilibria and eliminate limit-cycle behavior seen in 1D models.
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Calypso is a parameter-conditioned stochastic surrogate model for circumbinary accretion flows using PCA and multivariate Gaussian modeling, released as open-source software with a closed-form likelihood for parameter inference from time series.
Planetary formation tracks on the HR diagram show three branches: ascending during solid accretion with L proportional to T to the 8th for in-situ planetesimals, near-horizontal during gas accretion, and descending during post-accretion cooling.
A lens model from Gaia DR3 and HST data combined with a Bayesian test on Chandra observations constrains the X-ray emission origin in lensed quasar J0659 to a 0.020 × 0.010 arcsec ellipse offset 0.014 arcsec from the optical source at 1σ.
3D simulations recover the critical obliquity for disc breaking predicted by semi-analytic models and reveal additional stabilization by spiral arms that can prevent breaking.
Simulations show the accretion rate PSD in a q=0.2 SMBH binary is a broken power-law with white noise to -4 slope transition at ~5 times orbital frequency due to damped random walk gas delivery and minidisk filtering.
Simulations show that von Zeipel-Lidov-Kozai migration from inclined companions produces misaligned short-period hot Jupiters while coplanar high-eccentricity migration preserves alignment at longer periods.
A time-dependent model shows that star-disk collisions in TDE systems hosting EMRIs can eject 10^{-3} to 1 solar masses at 0.02-0.1c years after the initial flare, producing radio emission via interaction with circumnuclear material.
Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.
Anomalous pre-intersection dissipation in TDE simulations is numerical in origin, arising from pericenter kinematics combined with algorithm sensitivities to converging versus diverging flows.
Prograde highly eccentric perturbers in a ringed isothermal disc circularize and accumulate at the ring, forming a migration trap, while retrograde perturbers migrate inward without re-intersecting.
A population of AGN coronae with magnetization parameters spanning up to σ ~ 10 can reproduce the entire observed diffuse neutrino flux from TeV to PeV energies.
High-resolution GRMHD simulations show that tearing of tilted accretion disks around rapidly spinning supermassive black holes drives order-of-magnitude variability in continuum and broad-line luminosities on months-to-years timescales, explaining changing-look AGN.
Requiring thin-disk solutions to be thermally stable and single-valued imposes η_x ≡ dlnα/dlnX > 4/7, and a viscosity law α∝X^p with p>4/7 removes the radiation-pressure unstable branch.
JWST spectra of EC 53 indicate CO fundamental and H2O bending absorption weaken by ~2 during burst due to continuum dilution, with relative veiling yielding hot-continuum ratios of 2.9 and 1.71 and viscous-disk accretion-rate ratios of ~3.6 and ~2.0.
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.
Nonlinear shock formation dominates angular momentum deposition from planet-induced density waves, cooling matches it for sub-thermal planets, and viscosity only matters at unrealistically high values.
General-relativistic ray-tracing shows that non-flat accretion disk geometries systematically bias iron Kα-derived black hole spin, coronal height, and inclination estimates when fit with flat-disk models.
Observational constraints from X-ray binaries indicate that the Ogilvie model adequately describes warped disc evolution, with possible marginal non-isotropy in the internal viscosity.
citing papers explorer
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CO snow lines are stabilised by the vertical transport of volatiles
2D disc simulations with vertical volatile transport produce stable CO snow surface equilibria and eliminate limit-cycle behavior seen in 1D models.
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\texttt{calypso}: a Parameter-Conditioned Stochastic Surrogate Model for Circumbinary Accretion Time-Series
Calypso is a parameter-conditioned stochastic surrogate model for circumbinary accretion flows using PCA and multivariate Gaussian modeling, released as open-source software with a closed-form likelihood for parameter inference from time series.
-
Planetary formation tracks on the Hertzsprung-Russell diagram: Visualising the processes of giant planet growth
Planetary formation tracks on the HR diagram show three branches: ascending during solid accretion with L proportional to T to the 8th for in-situ planetesimals, near-horizontal during gas accretion, and descending during post-accretion cooling.
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Determining the spatial origin of X-ray and optical emission in the $z = 3.1$ strongly lensed radio-quiet quasar GraL J065904.1+162909 to hundreds of parsecs
A lens model from Gaia DR3 and HST data combined with a Bayesian test on Chandra observations constrains the X-ray emission origin in lensed quasar J0659 to a 0.020 × 0.010 arcsec ellipse offset 0.014 arcsec from the optical source at 1σ.
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The Bardeen-Petterson effect in accreting supermassive black-hole binaries: disc breaking and critical obliquity
3D simulations recover the critical obliquity for disc breaking predicted by semi-analytic models and reveal additional stabilization by spiral arms that can prevent breaking.
-
Stochastic Variability of Binary Accretion
Simulations show the accretion rate PSD in a q=0.2 SMBH binary is a broken power-law with white noise to -4 slope transition at ~5 times orbital frequency due to damped random walk gas delivery and minidisk filtering.
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Planet-Planet Secular Migration Predicts a Stellar Obliquity-Period Anti-Correlation
Simulations show that von Zeipel-Lidov-Kozai migration from inclined companions produces misaligned short-period hot Jupiters while coplanar high-eccentricity migration preserves alignment at longer periods.
-
Delayed Radio Flares in Tidal Disruption Events from Star-Disk Collision Outflows
A time-dependent model shows that star-disk collisions in TDE systems hosting EMRIs can eject 10^{-3} to 1 solar masses at 0.02-0.1c years after the initial flare, producing radio emission via interaction with circumnuclear material.
-
Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models
Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.
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On the origin of anomalous dissipation in simulations of tidal disruption events
Anomalous pre-intersection dissipation in TDE simulations is numerical in origin, arising from pericenter kinematics combined with algorithm sensitivities to converging versus diverging flows.
-
Orbital evolution of highly eccentric bodies embedded in a ringed accretion disc
Prograde highly eccentric perturbers in a ringed isothermal disc circularize and accumulate at the ring, forming a migration trap, while retrograde perturbers migrate inward without re-intersecting.
-
Turbulent AGN coronae as the origin of diffuse neutrinos up to PeV energies
A population of AGN coronae with magnetization parameters spanning up to σ ~ 10 can reproduce the entire observed diffuse neutrino flux from TeV to PeV energies.
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Changing-Look AGN Powered By Disk Tearing
High-resolution GRMHD simulations show that tearing of tilted accretion disks around rapidly spinning supermassive black holes drives order-of-magnitude variability in continuum and broad-line luminosities on months-to-years timescales, explaining changing-look AGN.
-
Radiation-pressure instability is an artifact of constant-$\alpha$ closure. Implications for AGN disk tensions
Requiring thin-disk solutions to be thermally stable and single-valued imposes η_x ≡ dlnα/dlnX > 4/7, and a viscosity law α∝X^p with p>4/7 removes the radiation-pressure unstable branch.
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EPISODE II: Variability in the CO and H$_2$O rovibrational absorption lines in a periodically variable protostar EC 53
JWST spectra of EC 53 indicate CO fundamental and H2O bending absorption weaken by ~2 during burst due to continuum dilution, with relative veiling yielding hot-continuum ratios of 2.9 and 1.71 and viscous-disk accretion-rate ratios of ~3.6 and ~2.0.
-
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.
-
$\alpha\beta q_\mathrm{th}$-mapping of planet-induced density wave damping in protoplanetary discs
Nonlinear shock formation dominates angular momentum deposition from planet-induced density waves, cooling matches it for sub-thermal planets, and viscosity only matters at unrealistically high values.
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The Effects of Complex Accretion Disk Geometry on Broadened Iron K$\alpha$ Lines
General-relativistic ray-tracing shows that non-flat accretion disk geometries systematically bias iron Kα-derived black hole spin, coronal height, and inclination estimates when fit with flat-disk models.
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On the isotropy of viscosity in accretion discs
Observational constraints from X-ray binaries indicate that the Ogilvie model adequately describes warped disc evolution, with possible marginal non-isotropy in the internal viscosity.