Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.
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9 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.
pGMCA separation of Chandra data yields the first uncontaminated X-ray maps of Sgr A East, with spectral fits showing lower ionization age and higher electron density than prior reports.
XSNAP provides a unified pipeline for X-ray supernova analysis and derives a progenitor mass-loss rate of (6.2±0.2)×10^{-5} solar masses per year for SN 2024ggi assuming a 20 km/s wind.
Radiative filaments in the Cygnus Loop exhibit thermal radio spectra resembling HII regions instead of typical SNR non-thermal emission.
Spectra of the western eROSITA bubbles reveal two uniform components at 0.60 keV and 0.21 keV with sub-solar abundances, plus a geometrical model constraining horizontal size to ~6 kpc but leaving vertical extent uncertain.
Time-dependent cosmic ray electron spectra in a simulated galactic disk match steady-state solutions up to 500 GeV but become steeper and more disk-confined at higher energies due to recent injections.
Reconstruction of GRO J1655-40, SAX J1819.3-2525 and 4U 1543-47 requires CE efficiencies α_0.5U ≳6.7, α_U ≳4.2, α_H ≳1.7 with no solutions below unity, implying need for additional energy or formalism changes plus natal kicks ≳50 km/s for 4U 1543-47.
Extended gamma-ray emission around Berkeley 59 is produced by cosmic rays accelerated in cluster winds colliding with ambient gas.
citing papers explorer
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Gauging the Impact of Cosmic Ray Feedback on the Stellar Initial Mass Function
Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.
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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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Isolating Sgr A East: The First Uncontaminated X-ray Maps of a Galactic Center Supernova Remnant
pGMCA separation of Chandra data yields the first uncontaminated X-ray maps of Sgr A East, with spectral fits showing lower ionization age and higher electron density than prior reports.
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XSNAP: An X-ray Supernova Analysis Pipeline with Application to the Type II Supernova 2024ggi
XSNAP provides a unified pipeline for X-ray supernova analysis and derives a progenitor mass-loss rate of (6.2±0.2)×10^{-5} solar masses per year for SN 2024ggi assuming a 20 km/s wind.
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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 SRG/eROSITA diffuse soft X-ray background II. spectra and morphology of the eROSITA bubbles in the western Galactic hemisphere
Spectra of the western eROSITA bubbles reveal two uniform components at 0.60 keV and 0.21 keV with sub-solar abundances, plus a geometrical model constraining horizontal size to ~6 kpc but leaving vertical extent uncertain.
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Steady-State or Not? The Evolution of Cosmic Ray Electron Spectra in Galaxies
Time-dependent cosmic ray electron spectra in a simulated galactic disk match steady-state solutions up to 500 GeV but become steeper and more disk-confined at higher energies due to recent injections.
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A Path to Constraints on Common Envelope Ejection in Massive Binaries: Full Evolutionary Reconstruction of Three Black Hole X-ray Binaries
Reconstruction of GRO J1655-40, SAX J1819.3-2525 and 4U 1543-47 requires CE efficiencies α_0.5U ≳6.7, α_U ≳4.2, α_H ≳1.7 with no solutions below unity, implying need for additional energy or formalism changes plus natal kicks ≳50 km/s for 4U 1543-47.
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Diffuse gamma-ray emissions around the stellar cluster Berkeley 59
Extended gamma-ray emission around Berkeley 59 is produced by cosmic rays accelerated in cluster winds colliding with ambient gas.