Cosmic ray acceleration and gamma-ray emission from protostellar jets

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00582019" target="_blank" >RIV/67985815:_____/22:00582019 - isvavai.cz</a>

Výsledek na webu

<a href="https://pos.sissa.it/395/684/pdf" target="_blank" >https://pos.sissa.it/395/684/pdf</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.22323/1.395.0684" target="_blank" >10.22323/1.395.0684</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Cosmic ray acceleration and gamma-ray emission from protostellar jets

Popis výsledku v původním jazyce

The detection of synchrotron radio emission from jets powered by massive protostars indicates the presence of relativistic electrons and magnetic fields of strength ∼0.3-5 mG. We study diffusive shock acceleration and magnetic field amplification in protostellar jets with speed 1000 km s-1. We show that the magnetic field in the synchrotron emitter can be amplified by the non-resonant hybrid (Bell) instability excited by the cosmic-ray streaming. By combining the synchrotron data with basic theory of Bell instability we estimate the magnetic field in the synchrotron emitter and the maximum energy of protons. Protons can achieve maximum energies ∼ 0.1 TeV and emit γ rays in their interaction with matter fields. We predict detectable levels of γ rays in IRAS 16547-5247 and IRAS 16848-4603. The detection of this radiation by the Fermi satellite in the GeV domain and the forthcoming Cherenkov Telescope Array at higher energies may open a new window to study the formation of massive stars, as well as diffusive acceleration and magnetic field amplification in shocks with velocities of about 1000 km s-1

Název v anglickém jazyce

Cosmic ray acceleration and gamma-ray emission from protostellar jets

Popis výsledku anglicky

The detection of synchrotron radio emission from jets powered by massive protostars indicates the presence of relativistic electrons and magnetic fields of strength ∼0.3-5 mG. We study diffusive shock acceleration and magnetic field amplification in protostellar jets with speed 1000 km s-1. We show that the magnetic field in the synchrotron emitter can be amplified by the non-resonant hybrid (Bell) instability excited by the cosmic-ray streaming. By combining the synchrotron data with basic theory of Bell instability we estimate the magnetic field in the synchrotron emitter and the maximum energy of protons. Protons can achieve maximum energies ∼ 0.1 TeV and emit γ rays in their interaction with matter fields. We predict detectable levels of γ rays in IRAS 16547-5247 and IRAS 16848-4603. The detection of this radiation by the Fermi satellite in the GeV domain and the forthcoming Cherenkov Telescope Array at higher energies may open a new window to study the formation of massive stars, as well as diffusive acceleration and magnetic field amplification in shocks with velocities of about 1000 km s-1

Druh

D - Stať ve sborníku

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA20-19854S" target="_blank" >GA20-19854S: Studium urychlení částic v astrofyzikálních výtryscích</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2022

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název statě ve sborníku

Proceedings of Science

ISBN

—

ISSN

1824-8039

e-ISSN

—

Počet stran výsledku

8

Strana od-do

684

Název nakladatele

Sissa Medilab srl

Místo vydání

Trieste

Místo konání akce

Berlin

Datum konání akce

12. 7. 2021

Typ akce podle státní příslušnosti

WRD - Celosvětová akce

Kód UT WoS článku

001081844900004