X-ray emission and dynamics from large diameter superbubbles: The case of N 70 superbubble

Abstract

The morphology, dynamics and thermal X-ray emission of the superbubble N70 is studied by means of 3D hydrodynamical simulations, carried out with the {\sc{yguazú-a}} code. We have considered different scenarios: the superbubble being the product of a single supernova remnant, of the stellar winds from an OB association, or the result of the joint action of stellar winds and a supernova event. Our results show that, in spite that all scenarios produce bubbles with the observed physical size, only those where the bubble is driven by stellar winds and a SN event are successful to explain the general morphology, dynamics and the X-ray luminosity of N70. Our models predict temperatures in excess of $10^8\mathrm{K}$ at the interior of the superbubble, however the density is too low and the emission in thermal X-ray above $2\mathrm{keV}$ is too faint to be detected.

9 pages, 11 figures, ApJ accepted

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Cited by in corpus (11)

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• Spitzer Observations of Dust Emission from HII Regions in the Large Magellanic Cloud
• Diffuse X-ray emission from the superbubbles N 70 and N 185 in the Large Magellanic Cloud
• The soft and hard X-rays thermal emission from star cluster winds with a supernova explosion
• Physical Nature of the [S II]-Bright Shell Nebulae N70 and N185
• Dissecting the hot bubbles in LMC-N57 with XMM-Newton
• Evolution of superbubbles in a self-gravitating disk
• The interaction of multiple stellar winds in stellar clusters: potential flow
• H$\alpha$ Kinematics of Superbubbles and Supernova Remnants of the Dwarf galaxy NGC 4214