Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/34516
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Padovani, Marco | en_US |
dc.contributor.author | Marcowith, Alexandre | en_US |
dc.contributor.author | GALLI, Daniele | en_US |
dc.contributor.author | HUNT, Leslie Kipp | en_US |
dc.contributor.author | FONTANI, FRANCESCO | en_US |
dc.date.accessioned | 2024-01-09T14:52:37Z | - |
dc.date.available | 2024-01-09T14:52:37Z | - |
dc.date.issued | 2021 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/34516 | - |
dc.description.abstract | Context. Recently, there has been an increased interest in the study of the generation of low-energy cosmic rays (< 1 TeV) in shocks situated on the surface of a protostar or along protostellar jets. These locally accelerated cosmic rays offer an attractive explanation for the high levels of non-thermal emission and ionisation rates observed close to these sources. Aims: The high ionisation rate observed in some protostellar sources is generally attributed to shock-generated UV photons. The aim of this article is to show that when synchrotron emission and a high ionisation rate are measured in the same spatial region, a locally shock-accelerated cosmic-ray flux is sufficient to explain both phenomena. Methods: We assume that relativistic protons and electrons are accelerated according to the first-order Fermi acceleration mechanism, and we calculate their emerging fluxes at the shock surface. These fluxes are used to compute the ionisation rate and the non-thermal emission at centimetre wavelengths. We then apply our model to the star-forming region OMC-2 FIR 3/FIR 4. Using a Bayesian analysis, we constrain the parameters of the model and estimate the spectral indices of the non-thermal radio emission, the intensity of the magnetic field, and its degree of turbulence. Results: We demonstrate that the local cosmic-ray acceleration model makes it possible to simultaneously explain the synchrotron emission along the HOPS 370 jet within the FIR 3 region and the ionisation rate observed near the FIR 4 protocluster. In particular, our model constrains the magnetic field strength (∼250−450 μG), its turbulent component (∼20−40 μG), and the jet velocity in the shock reference frame for the three non-thermal sources of the HOPS 370 jet (between 350 km s-1 and 1000 km s-1). Conclusions: Beyond the modelling of the OMC-2 FIR 3/FIR 4 system, we show how the combination of continuum observations at centimetre wavelengths and molecular transitions is a powerful new tool for the analysis of star-forming regions: These two types of observations can be simultaneously interpreted by invoking only the presence of locally accelerated cosmic rays, without having to resort to shock-generated UV photons. | en_US |
dc.language.iso | eng | en_US |
dc.title | The double signature of local cosmic-ray acceleration in star-forming regions | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/202039918 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2021/05/aa39918-20/aa39918-20.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 649 | en_US |
dc.relation.firstpage | A149 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | FRA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2021A&A...649A.149P | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.fulltext | With Fulltext | - |
item.openairetype | Article | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.languageiso639-1 | en | - |
item.grantfulltext | open | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0003-2303-0096 | - |
crisitem.author.orcid | 0000-0001-7706-6049 | - |
crisitem.author.orcid | 0000-0001-9162-2371 | - |
crisitem.author.orcid | 0000-0003-0348-3418 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
Padovani (2021a).pdf | Pdf editoriale | 3.33 MB | Adobe PDF | View/Open |
doublesig.pdf | postprint | 3.35 MB | Adobe PDF | View/Open |
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