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.
Title resolution pending
8 Pith papers cite this work. Polarity classification is still indexing.
8
Pith papers citing it
representative citing papers
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.
Late-time radio observations of SN 2012au show re-brightening best explained by emission from a newborn pulsar wind nebula rather than continued shock interaction with circumstellar material.
Middle-aged PWNe exhibit diverse reverberation-phase evolution but converge to Sedov-like states; 2D instabilities increase apparent size by up to 50% without changing global dynamics, supporting 1D model robustness.
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.
3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.
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
-
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.