Bibcode
Silich, Sergiy; Tenorio-Tagle, Guillermo; Torres-Campos, Ana; Muñoz-Tuñón, Casiana; Monreal-Ibero, Ana; Melo, Veronica
Referencia bibliográfica
The Astrophysical Journal, Volume 700, Issue 2, pp. 931-936 (2009).
Fecha de publicación:
8
2009
Revista
Número de citas
20
Número de citas referidas
16
Descripción
Here, we discuss the mechanical feedback that massive stellar clusters
provide to the interstellar medium of their host galaxy. We apply an
analytic theory developed in a previous study for M82-A1 to a sample of
10 clusters located in the central zone of the starburst galaxy M82, all
surrounded by compact and dense H II regions. We claim that the only way
that such H II regions can survive around the selected clusters, is if
they are embedded into a high-pressure ISM and if the majority of their
mechanical energy is lost within the star cluster volume via strong
radiative cooling. The latter implies that these clusters have a low
heating efficiency, η, and evolve in the bimodal hydrodynamic
regime. In this regime, the shock-heated plasma in the central zones of
a cluster becomes thermally unstable, loses its pressure and is
accumulated there, whereas the matter injected by supernovae and stellar
winds outside this volume forms a high-velocity outflow—the star
cluster wind. We calculated the heating efficiency for each of the
selected clusters and found that in all cases it does not exceed 10%.
Such low heating efficiency values imply a low mechanical energy output
and the impact that the selected clusters provide to the ISM of M82 is
thus much smaller than what one would expect using stellar cluster
synthetic models.
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Casiana
Muñoz Tuñón