The plasma physics of cosmic rays in star-forming regions
Date Issued
2017
Author(s)
Abstract
It is largely accepted that Galactic cosmic rays, which pervade the interstellar medium, originate by means of shock waves in supernova remnants. Cosmic rays activate the rich chemistry that is observed in a molecular cloud and they also regulate its collapse timescale, determining the efficiency of star and planet formation, but they cannot penetrate up to the densest part of a molecular cloud, where the formation of stars is expected, because of energy loss processes and magnetic field deflections. Recently, observations towards young protostellar systems showed a surprisingly high value of the ionisation rate, the main indicator of the presence of cosmic rays in molecular cloud. Synchrotron emission, the typical feature of relativistic electrons, has also been detected towards the bow shock of a T Tauri star. Nevertheless, the origin of these signatures peculiar to accelerated particles is still puzzling. Here we show that particle acceleration can be driven by shock waves occurring in protostars through the first-order Fermi acceleration mechanism. We expect that shocks in protostellar jets can be efficient accelerators of protons, which can be boosted up to mildly relativistic energies. A strong acceleration can also take place at the protostellar surface, where shocks produced by infalling material during the phase of collapse are powerful enough to accelerate protons. Our model shows that thermal particles can experience an acceleration during the first phases of a system similar to the proto-Sun, and can also be used to explain recent observations. The presence of a local source of cosmic rays may have an unexpected impact over the process of the formation of stars and planets, as well as on the pre-biotic molecule formation.
Volume
59
Issue
1
Start page
014002
Issn Identifier
0741-3335
Ads BibCode
2017PPCF...59a4002P
Rights
open.access
File(s)![Thumbnail Image]()
![Thumbnail Image]()
Loading...
Name
epspaper_padovani.pdf
Description
postprint
Size
599.46 KB
Format
Adobe PDF
Checksum (MD5)
8a383f1b74d4dbe9decb668d050d21d2
Loading...
Name
Padovani (2017).pdf
Description
[Administrators only]
Size
709.47 KB
Format
Adobe PDF
Checksum (MD5)
46cffb81091a5c6b0324b70b1383256f