Particle acceleration and magnetic field amplification in massive young stellar object jets

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00547589" target="_blank" >RIV/67985815:_____/21:00547589 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/68378271:_____/21:00548971

Výsledek na webu

<a href="https://doi.org/10.1093/mnras/stab635" target="_blank" >https://doi.org/10.1093/mnras/stab635</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stab635" target="_blank" >10.1093/mnras/stab635</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Particle acceleration and magnetic field amplification in massive young stellar object jets

Popis výsledku v původním jazyce

We study diffusive shock acceleration and magnetic field amplification in protostellar jets with speeds between 300 and 1500 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 in the range 0.04-0.65 TeV and emit gamma rays in their interaction with matter fields. We predict detectable levels of gamma rays in IRAS 16547-5247 and IRAS 16848-4603. The gamma ray flux can be significantly enhanced by the gas mixing due to Rayleigh-Taylor instability. 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

Particle acceleration and magnetic field amplification in massive young stellar object jets

Popis výsledku anglicky

We study diffusive shock acceleration and magnetic field amplification in protostellar jets with speeds between 300 and 1500 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 in the range 0.04-0.65 TeV and emit gamma rays in their interaction with matter fields. We predict detectable levels of gamma rays in IRAS 16547-5247 and IRAS 16848-4603. The gamma ray flux can be significantly enhanced by the gas mixing due to Rayleigh-Taylor instability. 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

J_imp - Článek v periodiku v databázi Web of Science

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

2021

Kód důvěrnosti údajů

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

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

504

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

15

Strana od-do

2405-2419

Kód UT WoS článku

000659453800059

EID výsledku v databázi Scopus

2-s2.0-85107987229