Numerical Simulations of Supernova Dust Destruction. Ii. Metal-Enriched Ejecta Knots

Silvia, Devin W.; Smith, Britton D.; Shull, J. M.

doi:10.1088/0004-637x/748/1/12

Cited by 72 publications

(91 citation statements)

References 39 publications

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“…produce a narrower wake and a lower sideways splashing velocity. Cooling of the shock-heated layer produced by the slower, reverse shock moving back into the bullet will also tend to result in extensive fragmentation as portions of the cloud rapidly cool and condense -a phenomenon observed in the cloudcrushing simulations of (Silvia et al 2010(Silvia et al , 2012. Such fragments could have considerably longer survival times than the structures present in the simulation presented here.…”

Section: Numerical Modelingmentioning

confidence: 78%

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The Orion fingers: Near-IR adaptive optics imaging of an explosive protostellar outflow

Bally¹,

Ginsburg²,

Silvia

et al. 2015

A&A

132

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Aims. Adaptive optics (AO) images are used to test the hypothesis that the explosive BN/KL outflow from the Orion OMC1 cloud core was powered by the dynamical decay of a non-hierarchical system of massive stars. Results. Several sub-arcsecond H 2 features and many [Fe ] "fingertips" on the projected outskirts of the flow show proper motions of ∼300 km s −1 . High-velocity, sub-arcsecond H 2 knots ("bullets") are seen as far as 140 from their suspected ejection site. If these knots propagated through the dense Orion A cloud, their survival sets a lower bound on their densities of order 10 7 cm −3 , consistent with an origin within a few au of a massive star and accelerated by a final multi-body dynamic encounter that ejected the BN object and radio source I from OMC1 about 500 yr ago. Conclusions. Over 120 high-velocity bow-shocks propagating in nearly all directions from the OMC1 cloud core provide evidence for an explosive origin for the BN/KL outflow triggered by the dynamic decay of a non-hierarchical system of massive stars. Such events may be linked to the origin of runaway, massive stars.

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Section: Numerical Modelingmentioning

confidence: 78%

“…The simulation set up is analogous to that of Silvia et al (2010Silvia et al ( , 2012 in which an over-dense, spherical cloud is embedded in a uniform ambient medium. For the simulation presented here, we have assumed an adiabatic equation of state that ignores any effects radiative cooling may have in this scenario.…”

Section: Numerical Modelingmentioning

confidence: 99%

The Orion fingers: Near-IR adaptive optics imaging of an explosive protostellar outflow

Bally¹,

Ginsburg²,

Silvia

et al. 2015

A&A

132

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“…However, many recent studies derive low efficiencies of dust condensation in SN ejecta from mid-and far-IR observations (e.g., Ercolano et al 2007;Rho et al 2008Rho et al , 2009Temim et al 2012), theoretical modelling of dust formation and survival in SN ejecta (Bianchi & Schneider 2007;Kozasa et al 2009;Cherchneff & Dwek 2009, and analysis of presolar grains with different origins found in meteorites . Recently, far-IR and submillimeter observations with the Herschel Space Observatory permitted the detection of larger masses of newly formed dust in SN ejecta (Matsuura et al 2011;Gomez et al 2012; see also Lakicevic et al 2011, for ground-based sub-mm observations), but it is still unclear what fraction of these grains will survive destruction in the reverse shocks of SN remnants (e.g., Silvia et al 2010Silvia et al , 2012. Given the controversies with dust input from SNe, AGB stars may be a dominant stellar source of dust production.…”

Section: Introductionmentioning

confidence: 99%

Dust input from AGB stars in the Large Magellanic Cloud

Zhukovska

Henning

2013

A&A

112

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Aims. The dust-forming population of AGB stars and their input to the interstellar dust budget of the Large Magellanic Cloud (LMC) are studied with evolutionary dust models with the main goals (1) to investigate how the amount and composition of dust from AGB stars vary over the galactic history; (2) to characterise the mass and metallicity distribution of the present population of AGB stars; (3) to quantify the contribution of AGB stars of different mass and metallicity to the present stardust population in the interstellar medium (ISM). Methods. We used models of the stardust lifecycle in the ISM developed and tested for the solar neighbourhood. The first global spatially resolved reconstruction of the star formation history of the LMC from the Magellanic Clouds Photometric Survey was employed to calculate the stellar populations in the LMC. Results. The dust input from AGB stars is dominated by carbon grains from stars with masses 4 M almost during the entire history of the LMC. The production of silicate, silicon carbide, and iron dust is delayed until the ISM is enriched to about half the present metallicity in the LMC. For the first time, theoretically calculated dust production rates of AGB stars are compared with those derived from infrared observations of AGB stars for the entire galaxy. We find good agreement within scatter of various observational estimates. We show that the majority of silicate and iron grains in the present stardust population originate from a small population of intermediate-mass stars consisting of only 4% of the total number of stars, whereas in the solar neighbourhood they originate from low-mass stars. With models of the lifecycle of stardust grains in the ISM we confirm the strong discrepancy between dust input from stars and the existing interstellar dust mass in the LMC reported previously.

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“…More recently, Sarangi & Cherchneff (2013, hereafter SC13) show that the molecular clusters precursors to dust (hereafter, dust clusters) gradually grow from low to high masses on a time-span of a few years after the explosion and provide a genuine explanation to the discrepancy on dust mass derived from IR data of SNe and submm data of SN remnants. The reprocessing of dust by the RS in SN remnants has been modelled by assuming pre-shock dust distributions derived from CNT and in the context of a homogeneous SN ejecta (Nozawa et al 2010;Silvia et al 2012). None of these studies addresses the chemistry of the RS, the survival of molecules, and the possibility to reform dust after the passage of the RS.…”

Section: Introductionmentioning

confidence: 99%

Molecules and dust in Cassiopeia A

Biscaro

Cherchneff

2014

A&A

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Aims. We study the chemistry of the type IIb supernova ejecta, which led to the Cas A supernova remnant, to assess the chemical type and quantity of dust that forms and evolves in the remnant phase. We later model a dense oxygen-rich ejecta knot, which is crossed by the reverse shock in Cas A, to study the evolution of the clump gas phase and the possibility to reform dust clusters in the post-reverse shock gas. Methods. The chemistry is described by a chemical network that includes all possible processes that are efficient at high gas temperatures and densities. The formation of key bimolecular species (e.g., CO and SiO) and dust clusters of silicates, alumina, silica, metal carbides and sulphides, pure metals, and amorphous carbon is considered. A set of stiff, coupled ordinary differential equations is solved for the conditions pertaining to both the SN ejecta and the post-reverse shock gas. Results. We find that the ejecta of type IIb SNe are unable to form large amounts of molecules and molecular clusters that are precursors to dust grains, when compared to their type II-P counterparts, because of their diffuse ejecta. The ejecta gas density needs to be increased by several orders of magnitude to allow for the formation of dust clusters. We show that the chemical composition of the dust clusters that form changes drastically and gains in chemical complexity with increasing gas density. Hence, the ejecta of the Cas A supernova progenitor must have been in the form of dense clumps to account for the dust chemical composition and masses that have been inferred from infrared observations of Cas A. As for the impact of the reverse shock on dense ejecta clumps, we show that the ejecta molecules that are destroyed by the shock reform in the post-reverse shock gas with lower abundances than those of the initial ejecta clump, except for SiO. These molecules include CO, SiS, and O 2 . On the other hand, dust clusters are destroyed by the reverse shock and do not reform in the post-reverse shock gas, even for the highest gas density. These results indicate that the synthesis of dust grains out of the gas phase in the dense knots of Cas A and in other supernova remnants is unlikely.

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Numerical Simulations of Supernova Dust Destruction. Ii. Metal-Enriched Ejecta Knots

Cited by 72 publications

References 39 publications

The Orion fingers: Near-IR adaptive optics imaging of an explosive protostellar outflow

The Orion fingers: Near-IR adaptive optics imaging of an explosive protostellar outflow

Dust input from AGB stars in the Large Magellanic Cloud

Molecules and dust in Cassiopeia A

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