White dwarf mass-radius data exclude large parameter space for ultralight scalars quadratically coupled to fermions by predicting forbidden radius gaps and mass shifts toward the Chandrasekhar limit or altered maximum masses.
Mass models of the Milky Way
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abstract
We present a simple method for fitting parametrized mass models of the Milky Way to observational constraints. We take a Bayesian approach which allows us to take into account input from photometric and kinematic data, and expectations from theoretical modelling. This provides us with a best-fitting model, which is a suitable starting point for dynamical modelling. We also determine a probability density function on the properties of the model, which demonstrates that the mass distribution of the Galaxy remains very uncertain. For our choices of parametrization and constraints, we find disc scale lengths of 3.00 \pm 0.22 kpc and 3.29 \pm 0.56 kpc for the thin and thick discs respectively; a Solar radius of 8.29 \pm 0.16 kpc and a circular speed at the Sun of 239 \pm 5 km/s; a total stellar mass of 6.43 \pm 0.63 * 10^10 M_sun; a virial mass of 1.26 \pm 0.24 * 10^12 M_sun and a local dark matter density of 0.40 \pm 0.04 GeV/cm^3. We find some correlations between the best-fitting parameters of our models (for example, between the disk scale lengths and the Solar radius), which we discuss. The chosen disc scale-heights are shown to have little effect on the key properties of the model.
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The Fermi and eROSITA bubbles likely result from identical ~10^56 erg collimated outbursts separated by ~10 Myr, with asymmetry indicating an eastern ambient density gradient.
Axion stars in miniclusters can reach bosenova conditions within the age of the Universe for QCD axions when initial overdensity exceeds roughly 100, once self-interaction effects are included.
citing papers explorer
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$\phi$-Dwarfs: White Dwarfs probe Quadratically Coupled Scalars
White dwarf mass-radius data exclude large parameter space for ultralight scalars quadratically coupled to fermions by predicting forbidden radius gaps and mass shifts toward the Chandrasekhar limit or altered maximum masses.
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Nested Fermi and eROSITA bubbles require very similar $\sim10^{56}$ erg collimated Galactic-center outbursts; their asymmetry indicates an eastern density gradient
The Fermi and eROSITA bubbles likely result from identical ~10^56 erg collimated outbursts separated by ~10 Myr, with asymmetry indicating an eastern ambient density gradient.
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Axion Star Bosenova in Axion Miniclusters
Axion stars in miniclusters can reach bosenova conditions within the age of the Universe for QCD axions when initial overdensity exceeds roughly 100, once self-interaction effects are included.