The mass of stellar black holes (BHs) is currently thought to be in the 3-20 M_☉ range, but is highly uncertain: recent observations indicate the existence of at least one BH with mass 〉20 M_☉. The metallicity of the progenitor star strongly influences the mass of the remnant, as only metal-poor stars can have a final mass higher than ̃{}40 M_☉, and are expected to directly collapse into BHs with mass 〉25 M_☉. By means of N-body simulations, we investigate the formation and evolution of massive stellar BHs (MSBHs, with mass 〉25 M_☉) in young dense star clusters. We study the effects of MSBHs on the population of X-ray sources.
X-ray binaries powered by massive stellar black holes
Mapelli, Michela
2013
Abstract
The mass of stellar black holes (BHs) is currently thought to be in the 3-20 M_☉ range, but is highly uncertain: recent observations indicate the existence of at least one BH with mass 〉20 M_☉. The metallicity of the progenitor star strongly influences the mass of the remnant, as only metal-poor stars can have a final mass higher than ̃{}40 M_☉, and are expected to directly collapse into BHs with mass 〉25 M_☉. By means of N-body simulations, we investigate the formation and evolution of massive stellar BHs (MSBHs, with mass 〉25 M_☉) in young dense star clusters. We study the effects of MSBHs on the population of X-ray sources.File in questo prodotto:
Non ci sono file associati a questo prodotto.
Pubblicazioni consigliate
I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
