Detection of helium lines in Balmer-dominated shocks of Type Ia SNRs reveals enhanced helium in some remnants and challenges shock models, enabling new constraints on progenitor environments.
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5 Pith papers cite this work. Polarity classification is still indexing.
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Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
Pulsational mass loss from supermassive stars ejects discrete shells that form the compact dense gas cocoons observed in Little Red Dots.
Radiative filaments in the Cygnus Loop exhibit thermal radio spectra resembling HII regions instead of typical SNR non-thermal emission.
Thin-shell numerical model of supernova remnants shows high ambient densities inhibit the Sedov-Taylor phase and prevent the reverse shock from reaching the explosion center above n0 = 5e5 cm^-3 due to rapid cooling.
citing papers explorer
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Helium emission from Balmer-dominated shocks in Type Ia supernova remnants provides constraints to their progenitor systems
Detection of helium lines in Balmer-dominated shocks of Type Ia SNRs reveals enhanced helium in some remnants and challenges shock models, enabling new constraints on progenitor environments.
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Revisiting radio synchrotron diagnostics in star-forming galaxies
Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
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Pulsational mass loss from supermassive stars creates the compact shells of Little Red Dots
Pulsational mass loss from supermassive stars ejects discrete shells that form the compact dense gas cocoons observed in Little Red Dots.
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The radio emission from radiative filaments of Cygnus Loop
Radiative filaments in the Cygnus Loop exhibit thermal radio spectra resembling HII regions instead of typical SNR non-thermal emission.
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The full evolution of supernova remnants in low and high density ambient media
Thin-shell numerical model of supernova remnants shows high ambient densities inhibit the Sedov-Taylor phase and prevent the reverse shock from reaching the explosion center above n0 = 5e5 cm^-3 due to rapid cooling.