English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
 
 
DownloadE-Mail
  Transport of protostellar cosmic rays in turbulent dense cores

Axen, M. F., Offner, S. S. S., Gaches, B. A. L., Fryer, C. L., Hungerford, A., & Silsbee, K. (2021). Transport of protostellar cosmic rays in turbulent dense cores. The Astrophysical Journal, 915(1): 43. doi:10.3847/1538-4357/abfc55.

Item is

Files

show Files
hide Files
:
Transport of Protostellar Cosmic Rays in Turbulent Dense Cores.pdf (Any fulltext), 4MB
 
File Permalink:
-
Name:
Transport of Protostellar Cosmic Rays in Turbulent Dense Cores.pdf
Description:
-
OA-Status:
Visibility:
Private
MIME-Type / Checksum:
application/pdf
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
License:
-

Locators

show

Creators

show
hide
 Creators:
Axen, Margot Fitz, Author
Offner, Stella S. S., Author
Gaches, Brandt A. L., Author
Fryer, Chris L., Author
Hungerford, Aimee, Author
Silsbee, Kedron1, Author           
Affiliations:
1Center for Astrochemical Studies at MPE, MPI for Extraterrestrial Physics, Max Planck Society, ou_1950287              

Content

show
hide
Free keywords: -
 Abstract: Recent studies have suggested that low-energy cosmic rays (CRs) may be accelerated inside molecular clouds by the shocks associated with star formation. We use a Monte Carlo transport code to model the propagation of CRs accelerated by protostellar accretion shocks through protostellar cores. We calculate the CR attenuation and energy losses and compute the resulting flux and ionization rate as a function of both radial distance from the protostar and angular position. We show that protostellar cores have nonuniform CR fluxes that produce a broad range of CR ionization rates, with the maximum value being up to two orders of magnitude higher than the radial average at a given distance. In particular, the CR flux is focused in the direction of the outflow cavity, creating a "flashlight" effect and allowing CRs to leak out of the core. The radially averaged ionization rates are less than the measured value for the Milky Way of ζ ≈ 10−16 s−1; however, within r ≈ 0.03 pc from the protostar, the maximum ionization rates exceed this value. We show that variation in the protostellar parameters, particularly in the accretion rate, may produce ionization rates that are a couple of orders of magnitude higher or lower than our fiducial values. Finally, we use a statistical method to model unresolved subgrid magnetic turbulence in the core. We show that turbulence modifies the CR spectrum and increases the uniformity of the CR distribution but does not significantly affect the resulting ionization

Details

show
hide
Language(s):
 Dates: 2021-07-02
 Publication Status: Published online
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: -
 Identifiers: DOI: 10.3847/1538-4357/abfc55
 Degree: -

Event

show

Legal Case

show

Project information

show

Source 1

show
hide
Title: The Astrophysical Journal
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: Bristol; Vienna : IOP Publishing; IAEA
Pages: - Volume / Issue: 915 (1) Sequence Number: 43 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3