astroarxiv.bsky.social
AstroArxiv
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Vector dark matter production during inflation in the gradient-expansion formalism. A.V. Lysenko et. al. https://arxiv.org/abs/2509.24963
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
On the (Im)possibility of Electrically Charged Planck Relics. Stefano Profumo https://arxiv.org/abs/2509.12520
{No-capture boundaries with extremality suppression, split by charge sign. {No-capture boundary with extremality suppression $ =0.1$. { : { :
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Extending the Dynamical Systems Toolkit: Coupled Fields in Multiscalar Dark Energy. Daniele Licciardello et. al. https://arxiv.org/abs/2509.02539
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
ACT inflation and its influence on reheating era in Einstein-Gauss-Bonnet gravity. Sergei D. Odintsov et. al. https://arxiv.org/abs/2508.11377
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Could We Observe an Exploding Black Hole in the Near Future?. Michael J. Baker et. al. https://arxiv.org/abs/2503.10755
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
On the Universality of Energy Extraction from Black Hole Spacetimes. Koushik Chatterjee et. al. https://arxiv.org/abs/2310.20043
Figure 1 Figure 2 Time evolution of the accretion rate $ {M Figure 4
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Non-Gaussian statistics of de Sitter spectators: A perturbative derivation of stochastic dynamics. Gonzalo A. Palma et. al. https://arxiv.org/abs/2309.16474
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
The TAP equation: evaluating combinatorial innovation in Biocosmology. Marina Cortês et. al. https://arxiv.org/abs/2204.14115
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Dynamical equilibria of fast neutrino flavor conversion. Jiabao Liu et. al. https://arxiv.org/abs/2509.26418
Figure 1 Probability density of the flavor-wave phase difference $ ^x_n$ for each mode $n$ in the $L = 1000$ simulation. Upper panel: nonequilibrium regime ($t [0, 40]$) showing phase misalignment. Lower panel: equilibrium regime ($t [40, 80]$) showing phase alignment. Color indicates mode index $n$. Th... Figure 3 Figure 4
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
The impact of the point spread function fitting radius on photometric uncertainty based on the Fisher information matrix. Sebastian Espinosa et. al. https://arxiv.org/abs/2509.20613
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
High-Dimensional Bayesian Model Comparison in Cosmology with GPU-accelerated Nested Sampling and Neural Emulators. Toby Lovick et. al. https://arxiv.org/abs/2509.13307
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Testing $n_s=1$ in light of the latest ACT and SPT data. Ze-Yu Peng et. al. https://arxiv.org/abs/2509.11902
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Dust Attenuation of Lyman-Werner Feedback: Reassessing Early Super Massive Black Holes Seed Formation. Bisweswar Sen https://arxiv.org/abs/2509.11111
Heavy seed formation rate as a function of redshift for the previous model (no dust shielding; red dashed line) and this work (with dust shielding; blue solid line). Dust shielding lowers the effective LW intensity, expanding the viable redshift range for heavy seed formation from a narrow $z $–... Growth history of supermassive black holes (SMBHs) from seed to $z=6$. The previous model (red dashed line) fails to reach the observed $ ^9~M_ $ masses within cosmic time, whereas our model (blue solid line) achieves rapid growth due to the enhanced number of heavy seeds formed under dust-shield... Comparison of the effective Lyman–Werner (LW) radiation field between the previous model (no dust shielding) and this work (with dust shielding). Our model predicts a substantial attenuation of LW flux even for modest dust enrichment ($D ^{-5 Relative population fractions of light, medium-weight, and heavy SMBH seeds predicted by the two models. The previous model (left bars) overpredicts heavy seeds and underrepresents intermediate channels. Our model (right bars), incorporating dust shielding, produces a more balanced distribution, ...
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Gravitational Recoil and Suppression of Super Massive Black Hole Seeds in the Early Universe. Bisweswar Sen https://arxiv.org/abs/2509.10564
Mass and radial distribution of wandering BHs. Most wanderers reside in low-mass halos and at intermediate radii ($ .1$--$1\,R_{ Distribution of GW recoil velocities for merged BHs, illustrating the diversity of kicks from varying mass ratios and spin configurations. Computation time per halo versus number of mergers. The Python framework scales efficiently, enabling large-scale SMBH population studies. Retention probability $P_{
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
GWTC-4.0: Constraints on the Cosmic Expansion Rate and Modified Gravitational-wave Propagation. The LIGO Scientific Collaboration et. al. https://arxiv.org/abs/2509.04348
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Diffusive shock acceleration: non-classical model of cosmic ray transport. A. A. Lagutin https://arxiv.org/abs/2509.03091
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Temperature induced optical scatter changes in titania-germania coatings. D. P. Kapasi et. al. https://arxiv.org/abs/2508.20043
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Tidal tails in open clusters. Morphology, binary fraction, dynamics, and rotation. Ira Sharma et. al. https://arxiv.org/abs/2508.19457
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
SMILES Data Release II: Probing Galaxy Evolution during Cosmic Noon and Beyond with NIRSpec Medium-Resolution Spectra. Yongda Zhu et. al. https://arxiv.org/abs/2508.12599
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Precision Measurement of Large Shear Signals. Jiarui Sun et. al. https://arxiv.org/abs/2508.10319
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Spatial mixing of stellar populations in globular clusters via binary-single star scattering. Václav Pavlík et. al. https://arxiv.org/abs/2508.03322
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
First Temperature Profile of a Stellar Flare using Differential Chromatic Refraction. Riley Clarke et. al. https://arxiv.org/abs/2507.19584
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Testing the Origin of Hot Jupiters with Atmospheric Surveys. Lina D'Aoust et. al. https://arxiv.org/abs/2507.13446
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Phase transition and nuclear symmetry energy from neutron star observations: Constraints in light of PSR J0614--3329. Shao-Peng Tang et. al. https://arxiv.org/abs/2507.10025
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 10h
Supernova-induced binary-interaction-powered supernovae: a model for SN2022jli. Ryosuke Hirai et. al. https://arxiv.org/abs/2507.09974
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