Cloud Formation by Supernova Implosion

Leonard E. C. Romano

doi:10.3847/1538-4357/ad2c05

2024-04-17

Leonard E. C. Romano *

Manuel Behrendt

Andreas Burkert

DOI：10.3847/1538-4357/ad2c05

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The deposition of energy and momentum by supernova explosions has been subject to numerous studies in the past few decades. However, while there has been some work that focused on the transition from the adiabatic to the radiative stage of a supernova remnant (SNR), the late radiative stage and merging with the interstellar medium (ISM) have received little attention. Here, we use three-dimensional, hydrodynamic simulations, focusing on the evolution of SNRs during the radiative phase, considering a wide range of physical explosion parameters ( n H , ISM is an element of 0.1 , 100 cm - 3 and E SN is an element of 1 , 14 x 10 51 erg ). We find that the radiative phase can be subdivided in four stages: A pressure-driven snowplow phase, during which the hot overpressurized bubble gas is evacuated and pushed into the cold shell; a momentum-conserving snowplow phase that is accompanied by a broadening of the shell; an implosion phase where cold material from the back of the shell is flooding the central vacuum; and a final cloud phase, during which the imploding gas is settling as a central, compact overdensity. The launching timescale for the implosion ranges from a few 100 kyr to a few Myr, while the cloud formation timescale ranges from a few to about 10 Myr. The highly chemically enriched clouds can become massive (M cl similar to 103-104 M circle dot) and self-gravitating within a few Myr after their formation, providing an attractive, novel pathway for supernova-induced star and planet formation in the ISM.

Keyword:

STAR-FORMATION

INTERSTELLAR-MEDIUM

CLUSTERED SUPERNOVAE

DUST GRAINS

FEEDBACK

EVOLUTION

REMNANTS

MODEL

GALAXIES

ORIGIN