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Titolo:
Shocks and sonic booms in the intracluster medium: X-ray shells and radio galaxy activity
Autore:
Reynolds, CS; Heinz, S; Begelman, MC;
Indirizzi:
Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA Univ Colorado Boulder CO USA 80309 t Lab Astrophys, Boulder, CO 80309 USA
Titolo Testata:
ASTROPHYSICAL JOURNAL
fascicolo: 2, volume: 549, anno: 2001,
parte:, 2
pagine: L179 - L182
SICI:
0004-637X(20010310)549:2<L179:SASBIT>2.0.ZU;2-X
Fonte:
ISI
Lingua:
ENG
Soggetto:
RADIATION MAGNETOHYDRODYNAMICS CODE; 2 SPACE DIMENSIONS; ASTROPHYSICAL FLOWS; EMITTING GAS; CLUSTER GAS; CYGNUS-A; ALGORITHMS; ZEUS-2D; LOBES; TESTS;
Keywords:
galaxies : clusters : general; galaxies : jets; hydrodynamics; shock waves;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
23
Recensione:
Indirizzi per estratti:
Indirizzo: Reynolds, CS Univ Colorado, Joint Inst Lab Astrophys, Campus Box 440, Boulder, CO 80309USA Univ Colorado Campus Box 440 Boulder CO USA 80309 CO 80309USA
Citazione:
C.S. Reynolds et al., "Shocks and sonic booms in the intracluster medium: X-ray shells and radio galaxy activity", ASTROPHYS J, 549(2), 2001, pp. L179-L182

Abstract

Motivated by hydrodynamic simulations, we discuss the X-ray appearance of radio galaxies embedded in the intracluster medium (ICM) of a galaxy cluster. We distinguish three regimes. In the early life of a powerful source, the entire radio cocoon is expanding supersonically and hence drives a strongshock into the ICM. Eventually, the sides of the cocoon become subsonic, and the ICM is disturbed by the sonic booms of the jet's working surface. Inboth of these regimes, X-ray observations would find an X-ray shell. In the strong shock regime, this shell will be hot and relatively thin. However,in the weak shock (sonic-boom) regime, the shell will be approximately thesame temperature as the undisturbed ICM. If a cooling flow is present, theobserved shell may even be cooler than the undisturbed ICM because of the lifting of cooler material into the shell from the inner (cooler) regions of the cluster. In the third and final regime, the cocoon has collapsed, andno well-defined X-ray shell will be seen. We discuss ways of estimating the power and age of the source once its regime of behavior has been determined.

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Documento generato il 30/03/20 alle ore 12:45:15