We present an analysis of XMM-Newton observations of the superbubble 30 Dor C and compare the results with the predictions from the standard wind-blown bubble model. We find that the observed X-ray spectra cannot be fitted satisfactorily with the model alone and that there is evidence for nonthermal X-ray emission, which is particularly important at 4 keV. The combination of the bubble model and a power law gives a reasonable fit to the observed spectra. The thermal pressure and central temperature of the bubble are 3.3 × 10-11 dynes cm-2 and 7.4 × 106 K, respectively, and we infer that for a bubble age of t ~ 4 × 106 yr the ambient density is n0 38 cm-3, the mechanical luminosity is Lmech ~ 1037 ergs s-1, and the coefficient of thermal co...
Deep-sea archives all over the world show an enhanced concentration of the radionuclide 60Fe, isolat...
Context. Massive stars influence their environment through stellar winds, ionising radiation, and su...
Using Chandra and HST, we show that X-ray and Hα filaments that form the 1.3 kpc diameter superbubbl...
We present an analysis of XMM-Newton observations of the superbubble 30 Dor C and compare the result...
We present an analysis of XMM-Newton observations of the superbubble 30 Dor C and compare the result...
The hot, X-ray-emitting gas in superbubbles imparts energy and enriched material to the interstellar...
We present evidence of diffuse, non-thermal X-ray emission from the superbubble 30 Doradus C (30 Dor...
This article has an erratum M. Krause, et al., “Feedback by massive stars and the emergence of super...
Aims. We present a detailed study of the superbubble 30 Dor C and the newly identified supernova re...
Aims. We present a detailed study of the superbubble 30 Dor C and the newly identified supernova rem...
Martin G. H. Krause, and Roland Diehl, “Dynamics and Energy Loss in Superbubble”, The Astrophysical ...
Recent observations have revealed a superbubble associated with the young stellar cluster OCl 352 ne...
Aims. We perform an analysis of the X-ray superbubble in the N 206 H ii region in the Large Magellan...
The morphology, dynamics and thermal X-ray emission of the superbubble N70 is studied by means of 3D...
We have used optical echelle spectra along with ROSAT and ASCA X-ray spectra to test the hypothesis ...
Deep-sea archives all over the world show an enhanced concentration of the radionuclide 60Fe, isolat...
Context. Massive stars influence their environment through stellar winds, ionising radiation, and su...
Using Chandra and HST, we show that X-ray and Hα filaments that form the 1.3 kpc diameter superbubbl...
We present an analysis of XMM-Newton observations of the superbubble 30 Dor C and compare the result...
We present an analysis of XMM-Newton observations of the superbubble 30 Dor C and compare the result...
The hot, X-ray-emitting gas in superbubbles imparts energy and enriched material to the interstellar...
We present evidence of diffuse, non-thermal X-ray emission from the superbubble 30 Doradus C (30 Dor...
This article has an erratum M. Krause, et al., “Feedback by massive stars and the emergence of super...
Aims. We present a detailed study of the superbubble 30 Dor C and the newly identified supernova re...
Aims. We present a detailed study of the superbubble 30 Dor C and the newly identified supernova rem...
Martin G. H. Krause, and Roland Diehl, “Dynamics and Energy Loss in Superbubble”, The Astrophysical ...
Recent observations have revealed a superbubble associated with the young stellar cluster OCl 352 ne...
Aims. We perform an analysis of the X-ray superbubble in the N 206 H ii region in the Large Magellan...
The morphology, dynamics and thermal X-ray emission of the superbubble N70 is studied by means of 3D...
We have used optical echelle spectra along with ROSAT and ASCA X-ray spectra to test the hypothesis ...
Deep-sea archives all over the world show an enhanced concentration of the radionuclide 60Fe, isolat...
Context. Massive stars influence their environment through stellar winds, ionising radiation, and su...
Using Chandra and HST, we show that X-ray and Hα filaments that form the 1.3 kpc diameter superbubbl...