Impact of galaxy clusters on the propagation of ultrahigh-energy cosmic rays

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378271%3A90232%2F23%3A00603851" target="_blank" >RIV/68378271:90232/23:00603851 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.3847/1538-4357/acfeef" target="_blank" >https://doi.org/10.3847/1538-4357/acfeef</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/acfeef" target="_blank" >10.3847/1538-4357/acfeef</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Impact of galaxy clusters on the propagation of ultrahigh-energy cosmic rays

Popis výsledku v původním jazyce

Galaxy clusters are the largest objects in the Universe kept together by gravity. Most of their baryonic content is made of a magnetized diffuse plasma. We investigate the impact of such a magnetized environment on the propagation of ultrahigh-energy cosmic rays (UHECRs). The intracluster medium (ICM) is described according to the self-similar assumption, in which gas density and pressure profiles are fully determined by the cluster mass and redshift. The magnetic field is scaled to the thermal components of the ICM under different assumptions. We model the propagation of UHECRs in the ICM using a modified version of the Monte Carlo code SimProp, where hadronic processes and diffusion in the turbulent magnetic field are implemented.

Název v anglickém jazyce

Impact of galaxy clusters on the propagation of ultrahigh-energy cosmic rays

Popis výsledku anglicky

Galaxy clusters are the largest objects in the Universe kept together by gravity. Most of their baryonic content is made of a magnetized diffuse plasma. We investigate the impact of such a magnetized environment on the propagation of ultrahigh-energy cosmic rays (UHECRs). The intracluster medium (ICM) is described according to the self-similar assumption, in which gas density and pressure profiles are fully determined by the cluster mass and redshift. The magnetic field is scaled to the thermal components of the ICM under different assumptions. We model the propagation of UHECRs in the ICM using a modified version of the Monte Carlo code SimProp, where hadronic processes and diffusion in the turbulent magnetic field are implemented.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10303 - Particles and field physics

Projekt

—

Návaznosti

—

Rok uplatnění

2023

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Svazek periodika

957

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

8

Strana od-do

80

Kód UT WoS článku

001092135700001

EID výsledku v databázi Scopus

2-s2.0-85176936516