Sequential explosions of supernovae in an ob association and formation of a superbubble

Tomisaka, Kohji; Habe, Asao; Ikeuchi, Satoru

doi:10.1007/bf00648941

Cited by 67 publications

(40 citation statements)

References 28 publications

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“…As soon as this happens, however, the dynamics of the wind-blown bubble is quickly overtaken by the SNe, as is clear from comparing the mechanical luminosities of the winds and SNe (cf. Tomisaka et al 1981). The former cannot be larger than yr being the average time interval between two consecutive SNe.…”

Section: Discussionmentioning

confidence: 96%

Numerical studies on the link between radioisotopic signatures on Earth and the formation of the Local Bubble

Schulreich

Breitschwerdt

Feige

et al. 2017

A&A

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Context. The discovery of radionuclides like 60 Fe with half-lives of million years in deep-sea crusts and sediments offers the unique possibility to date and locate nearby supernovae. Aims. We want to quantitatively establish that the 60 Fe enhancement is the result of several supernovae which are also responsible for the formation of the Local Bubble, our Galactic habitat. Methods. We performed three-dimensional hydrodynamic adaptive mesh refinement simulations (with resolutions down to subparsec scale) of the Local Bubble and the neighbouring Loop I superbubble in different homogeneous, self-gravitating environments. For setting up the Local and Loop I superbubble, we took into account the time sequence and locations of the generating core-collapse supernova explosions, which were derived from the mass spectrum of the perished members of certain stellar moving groups. The release of 60 Fe and its subsequent turbulent mixing process inside the superbubble cavities was followed via passive scalars, where the yields of the decaying radioisotope were adjusted according to recent stellar evolution calculations. Results. The models are able to reproduce both the timing and the intensity of the 60 Fe excess observed with rather high precision, provided that the external density does not exceed 0.3 cm −3 on average. Thus the two best-fit models presented here were obtained with background media mimicking the classical warm ionised and warm neutral medium. We also found that 60 Fe (which is condensed onto dust grains) can be delivered to Earth via two physical mechanisms: either through individual fast-paced supernova blast waves, which cross the Earth's orbit sometimes even twice as a result of reflection from the Local Bubble's outer shell, or, alternatively, through the supershell of the Local Bubble itself, injecting the 60 Fe content of all previous supernovae at once, but over a longer time range.

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Section: Discussionmentioning

confidence: 96%

Numerical studies on the link between radioisotopic signatures on Earth and the formation of the Local Bubble

Schulreich

Breitschwerdt

Feige

et al. 2017

A&A

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“…The dominant paradigm holds that supershells are formed through the cumulative action of multiple stellar winds and supernovae, which blow hot, overpressurized bubbles, and sweep up the surrounding medium into cool, dense shells (Bruhweiler et al 1980;Tomisaka et al 1981;McCray & Kafatos 1987). The accumulation of the ISM in such superstructures is one means of generating the high densities and column densities required for the production of molecular gas, and supershells have long been suggested as drivers of molecular cloud formation (e.g., McCray & Kafatos 1987;Mashchenko & Silich 1994;Fukui et al 1999;Hartmann et al 2001).…”

Section: Introductionmentioning

confidence: 99%

SUPERSHELLS AS MOLECULAR CLOUD FACTORIES: PARSEC RESOLUTION OBSERVATIONS OF H I AND¹²CO(J= 1-0) IN GSH 287+04–17 AND GSH 277+00+36

Dawson

McClure-Griffiths

Kawamura

et al. 2011

ApJ

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We present parsec-scale resolution observations of the atomic and molecular interstellar medium in two Galactic supershells, GSH 287+04−17 and GSH 277+00+36. H i synthesis images from the Australia Telescope Compact Array are combined with 12 CO(J = 1-0) data from the NANTEN telescope to reveal substantial quantities of molecular gas closely associated with both shells. These data allow us to confirm an enhanced level of molecularization over the volumes of both objects, providing the first direct observational evidence of increased molecular cloud production due to the influence of supershells. We find that the atomic shell walls are dominated by cold gas with estimated temperatures and densities of T ∼ 100 K and n 0 ∼ 10 cm −3 , respectively. Locally, the shells show rich substructure in both tracers, with molecular gas seen elongated along the inner edges of the atomic walls, embedded within H i filaments and clouds, or taking the form of small CO clouds at the tips of tapering atomic "fingers." We discuss these structures in the context of different formation scenarios, suggesting that molecular gas embedded within shell walls is well explained by in situ formation from the swept-up medium, whereas CO seen at the ends of fingers of H i may trace remnants of molecular clouds that pre-date the shells. A preliminary assessment of star formation activity within the shells confirms ongoing star formation in the molecular gas of both GSH 287+04−17 and GSH 277+00+36.

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“…They are observationally traced at optical, radio and X-ray wavelengths. The origin of this hot gas has been the topic of numerous investigations including the interaction of the stellar winds with Send offprint requests to: W. Reich, e-mail: wreich@mpifr-bonn.mpg.de interstellar matter (Castor et al 1975;Weaver et al 1977;Abbott et al 1981) and single or sequential SN explosions (Elmegreen & Lada 1977;Tomisaka et al 1980;Higdon 1981).…”

Section: Introductionmentioning

confidence: 99%

The Cygnus superbubble revisited

Uyanıker

Fürst

Reich

et al. 2001

A&A

123

140

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Abstract. The Orion local spiral arm is seen tangential towards the Cygnus region. Intense radio emission with quite a complex morphology is observed, which appears to be surrounded by strong soft X-ray emission. This remarkable X-ray structure is known as the Cygnus superbubble. We compare a recent 1.4 GHz radio continuum and polarization map from the Effelsberg 100-m telescope with X-ray data from the ROSAT all-sky survey of this area. Including available survey data of the infrared, H i and CO emission, we investigate a number of high latitude features, which are physically related to one of the Cygnus OB associations. These OB associations, however, are located along the local arm at different distances. Our results support the view that the Cygnus superbubble is not a physical unity, but results from a projection of unrelated X-ray emitting features at different distances blown out from the local arm seen along the line of sight.

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Sequential explosions of supernovae in an ob association and formation of a superbubble

Cited by 67 publications

References 28 publications

Numerical studies on the link between radioisotopic signatures on Earth and the formation of the Local Bubble

Numerical studies on the link between radioisotopic signatures on Earth and the formation of the Local Bubble

SUPERSHELLS AS MOLECULAR CLOUD FACTORIES: PARSEC RESOLUTION OBSERVATIONS OF H I AND¹²CO(J= 1-0) IN GSH 287+04–17 AND GSH 277+00+36

The Cygnus superbubble revisited

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Sequential explosions of supernovae in an ob association and formation of a superbubble

Cited by 67 publications

References 28 publications

Numerical studies on the link between radioisotopic signatures on Earth and the formation of the Local Bubble

Numerical studies on the link between radioisotopic signatures on Earth and the formation of the Local Bubble

SUPERSHELLS AS MOLECULAR CLOUD FACTORIES: PARSEC RESOLUTION OBSERVATIONS OF H I AND12CO(J= 1-0) IN GSH 287+04–17 AND GSH 277+00+36

The Cygnus superbubble revisited

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SUPERSHELLS AS MOLECULAR CLOUD FACTORIES: PARSEC RESOLUTION OBSERVATIONS OF H I AND¹²CO(J= 1-0) IN GSH 287+04–17 AND GSH 277+00+36