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%.
M., Terzieva, R., & Herbst, E
6 Pith papers cite this work, alongside 356 external citations. Polarity classification is still indexing.
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Neglect of time-dependent chemistry causes steady-state analyses of H3+ observations to overestimate the cosmic-ray ionization rate by a median factor of ~3, yielding a revised mean ζ_H2 ≈ 2×10^{-17} s^{-1}.
Water binding energy on silicate grains is twice that on ice, enabling local retention and inheritance for terrestrial planets without outer Solar System delivery.
Low-energy cosmic ray ionization rates in the Orion region scale with star formation rate as log10 ζ = (1.4±0.70)log10 SFR + (-10.5±2.9), supporting local generation by star formation.
Ionization rates in the envelopes of NGC-1333 IRAS4A, L1448-C, and L1157 reach 1e-16 to 1e-13 s^{-1}, far above the ISM baseline of 6e-17 s^{-1}.
The paper reviews techniques for measuring protostellar accretion, analyzes methodological differences and caveats in comparing observations with simulations, and outlines next steps for a fuller picture.
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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The cosmic ray ionization rate from H3+ observations can be overestimated due to neglect of time-dependent chemistry
Neglect of time-dependent chemistry causes steady-state analyses of H3+ observations to overestimate the cosmic-ray ionization rate by a median factor of ~3, yielding a revised mean ζ_H2 ≈ 2×10^{-17} s^{-1}.
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Astrochemical Inheritance of Terrestrial Planets Water from Local Wet Silicates
Water binding energy on silicate grains is twice that on ice, enabling local retention and inheritance for terrestrial planets without outer Solar System delivery.
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Star Formation Drives Production of Low Energy Cosmic Rays
Low-energy cosmic ray ionization rates in the Orion region scale with star formation rate as log10 ζ = (1.4±0.70)log10 SFR + (-10.5±2.9), supporting local generation by star formation.
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Evidence of Enhanced Ionization in Protostellar Envelopes
Ionization rates in the envelopes of NGC-1333 IRAS4A, L1448-C, and L1157 reach 1e-16 to 1e-13 s^{-1}, far above the ISM baseline of 6e-17 s^{-1}.
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The Accretion Process on Protostars
The paper reviews techniques for measuring protostellar accretion, analyzes methodological differences and caveats in comparing observations with simulations, and outlines next steps for a fuller picture.