A Textbook Example of a Bow Shock in the Merging Galaxy Cluster 1E 0657-56

2002 ◽  
Vol 567 (1) ◽  
pp. L27-L31 ◽  
Author(s):  
M. Markevitch ◽  
A. H. Gonzalez ◽  
L. David ◽  
A. Vikhlinin ◽  
S. Murray ◽  
...  
Keyword(s):  
Galaxy Cluster ◽  
Bow Shock

scholarly journals A SPECTACULAR BOW SHOCK IN THE 11 keV GALAXY CLUSTER AROUND 3C 438

2017 ◽  
Vol 834 (2) ◽  
pp. 159 ◽  
Author(s):  
Deanna L. Emery ◽  
Ákos Bogdán ◽  
Ralph P. Kraft ◽  
Felipe Andrade-Santos ◽  
William R. Forman ◽  
...  
Keyword(s):  
Galaxy Cluster ◽  
Bow Shock

scholarly journals Pairs of giant shock waves (N-waves) in merging galaxy clusters

2020 ◽  
Vol 501 (1) ◽  
pp. 1038-1045
Author(s):  
Congyao Zhang ◽  
Eugene Churazov ◽  
Irina Zhuravleva
Keyword(s):  
Galaxy Cluster ◽  
Spherical Geometry ◽  
Bow Shock ◽  
X Rays ◽  
Coma Cluster ◽  
Linear Evolution ◽  
Cluster Centre ◽  
Main Cluster ◽  
Merger Event ◽  
Radio Band

ABSTRACT When a subcluster merges with a larger galaxy cluster, a bow shock is driven ahead of the subcluster. At a later merger stage, this bow shock separates from the subcluster, becoming a ‘runaway’ shock that propagates down the steep density gradient through the cluster outskirts and approximately maintains its strength and the Mach number. Such shocks are plausible candidates for producing radio relics in the periphery of clusters. We argue that, during the same merger stage, a secondary shock is formed much closer to the main cluster centre. A close analogue of this structure is known in the usual hydrodynamics as N-waves, where the trailing part of the ‘N’ is the result of the non-linear evolution of a shock. In merging clusters, spherical geometry and stratification could further promote its development. Both the primary and the secondary shocks are the natural outcome of a single merger event and often both components of the pair should be present. However, in the radio band, the leading shock could be more prominent, while the trailing shock might conversely be more easily seen in X-rays. The latter argument implies that for some of the (trailing) shocks found in X-ray data, it might be difficult to identify their ‘partner’ leading shocks or the merging subclusters, which are farther away from the cluster centre. We argue that the Coma cluster and A2744 could be two examples in a post-merger state with such well-separated shock pairs.

Dependence of the Properties of a Turbulent Cascade behind the Bow Shock on the Dynamics of the Solar Wind Parameters

2020 ◽  
Vol 58 (6) ◽  
pp. 478-486
Author(s):  
L. S. Rakhmanova ◽  
M. O. Riazantseva ◽  
G. N. Zastenker ◽  
Yu. I. Yermolaev ◽  
I. G. Lodkina
Keyword(s):  
Solar Wind ◽  
Bow Shock ◽  
Solar Wind Parameters ◽  
Turbulent Cascade

An X-Ray–Selected Galaxy Cluster at [CLC][ITAL]z[/ITAL][/CLC] = 1.26

1999 ◽  
Vol 118 (1) ◽  
pp. 76-85 ◽  
Author(s):  
Piero Rosati ◽  
S. A. Stanford ◽  
Peter R. Eisenhardt ◽  
Richard Elston ◽  
Hyron Spinrad ◽  
...  
Keyword(s):  
Galaxy Cluster ◽  
X Ray
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