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AstroArxiv
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Astrophysical Consequences of an Electroweak $η_{\rm w}$ Pseudo-Scalar. Hooman Davoudiasl https://arxiv.org/abs/2510.02310
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
When backgrounds become signals: neutrino interactions in xenon-based dark matter detectors. M. Atzori Corona et. al. https://arxiv.org/abs/2509.22178
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Hawking tunneling radiation with thermodynamic pressure. Cheng Hu et. al. https://arxiv.org/abs/2509.03552
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Boomerang mechanism explaining the excess radio background. Bhupal Dev et. al. https://arxiv.org/abs/2509.03441
Figure 1 Allowed region shaded with different shades corresponding to different photon energy bands and with the best-fit point {orange Figure 3 Best fit curve for $T_{
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Imprints of screened dark energy on nonlocal quantum correlations. Fabiano Feleppa et. al. https://arxiv.org/abs/2508.18448
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Neural Posterior Estimation of Neutron Star Equations of State. Valéria Carvalho et. al. https://arxiv.org/abs/2507.23506
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Cosmology with a Non-minimally Coupled Dark Matter Fluid I. Background Evolution. Samuele Silveravalle et. al. https://arxiv.org/abs/2507.16614
Evolution of the density parameters as a function of redshift $1+z ^{-1 The comoving Hubble horizon as a function of redshift. The solid, dashed and dotted-dashed lines are the behavior in the presence of NMC with negative, null, or positive curvature respectively, while the dotted line is the one in $ $CDM. The vertical dotted grey lines represent matter-radiation e... The dynamical state parameter $w$ as a function of redshift. The solid, dashed and dotted-dashed lines are the behavior in the presence of NMC with negative, null, or positive curvature respectively, while the dotted line is the one in $ $CDM. The vertical dotted grey lines represent matter-radia...
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Learning Representations of Event Time Series with Sparse Autoencoders for Anomaly Detection, Similarity Search, and Unsupervised Classification. Steven Dillmann et. al. https://arxiv.org/abs/2507.11620
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Primordial Gravitational Wave Background as a Probe of the Primordial Black Holes. Utkarsh Kumar https://arxiv.org/abs/2507.10033
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Insights in $f(Q)$ cosmology: the relevance of the connection. Ismael Ayuso et. al. https://arxiv.org/abs/2506.03506
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Primordial Stochastic Gravitational Waves from Massive Higher-Spin Bosons. Haipeng An et. al. https://arxiv.org/abs/2504.05389
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Impact of dineutrons on nuclear compositions of a core-collapse supernova. Tatsuya Matsuki et. al. https://arxiv.org/abs/2412.19521
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Impact of dineutrons on nuclear compositions of a core-collapse supernova. Tatsuya Matsuki et. al. https://arxiv.org/abs/2412.19521
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
SimpleBounce : a simple package for the false vacuum decay. Ryosuke Sato https://arxiv.org/abs/1908.10868
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Simple Gradient Flow Equation for the Bounce Solution. Ryosuke Sato https://arxiv.org/abs/1907.02417
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Effects of Primordial Black Holes on IGM History. Emily Koivu et. al. https://arxiv.org/abs/2510.00246
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
The Draco Dwarf Spheroidal Galaxy in the First Year of DESI Data. J. Ding et. al. https://arxiv.org/abs/2509.21822
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
The Draco Dwarf Spheroidal Galaxy in the First Year of DESI Data. J. Ding et. al. https://arxiv.org/abs/2509.21822
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona. Surajit Mondal et. al. https://arxiv.org/abs/2509.16453
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Improving cosmological reach of a gravitational wave observatory using Deep Loop Shaping. Jonas Buchli et. al. https://arxiv.org/abs/2509.14016
{Detailed illustration of Deep Loop Shaping. Figure 2 Figure 3 Figure 4
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Investigating aerosols as a way to reconcile K2-18 b JWST MIRI and NIRISS/NIRSpec observations. Adam Yassin Jaziri et. al. https://arxiv.org/abs/2509.13932
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Bayesian recalibration of flux scale factors in diffuse radio maps using low-resolution absolute radiometers. Ainulnabilah Nasirudin et. al. https://arxiv.org/abs/2509.11894
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Metallicity of the double Red Clump in the Milky Way Bulge. Zofia Budzik et. al. https://arxiv.org/abs/2509.03402
Posterior distribution of fitted mixture model parameters without RGBB. {corner_None Same as Figure {corner_None Same as Figure {feh_None Posterior distribution of fitted mean metallicities and their dispersions for a mixture model without RGBB. The top right panel shows the posterior distribution of metallicity difference between two RC. {feh_None
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Investigations of MWISP Clumps: 13CO Clump Source Catalog and Physical Properties. Yu Jiang et. al. https://arxiv.org/abs/2509.01955
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
The orbital period and inclination of the neutron star X-ray transient MAXI J1807+132. E. A. Saavedra et. al. https://arxiv.org/abs/2508.20178
Figure 1 Figure 2 Light curve modelling. Upper panel: J1807 data (black dots) and the synthetic light curves based on the 68 per cent confidence intervals from the MCMC analysis (red lines). The teal line indicates the best-fit model. Lower panel: Residuals from the best-fit model (black dots) and for each individ... Figure 4