Dust Destruction Rates and Lifetimes in the Magellanic Clouds

Temim, Tea; Dwek, Eli; Tchernyshyov, Kirill; Boyer, Martha L.; Meixner, Margaret; Gall, C.; Roman-Duval, Julia

doi:10.1088/0004-637x/799/2/158

Cited by 72 publications

(98 citation statements)

References 98 publications

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“…Most recent calculations show that in the local solar neighbourhood SNRs destroy more dust than is produced by SNe and asymptotic giant branch (AGB) stars combined (Bocchio et al 2014;Slavin et al 2015, and references therein). Similar conclusions were reached for the Magellanic Clouds (Temim et al 2015). This imbalance between the production and destruction rate also prevails in local and high-redshift galaxies; this suggests that dust may need to reconstitute by accretion in the dense phases of the interstellar medium (ISM; Dwek & Scalo 1980;Valiante et al 2011;Gall et al 2011a,b).…”

Section: Introductionsupporting

confidence: 54%

Dust destruction by the reverse shock in the Cassiopeia A supernova remnant

Micelotta

Dwek

Slavin

2016

A&A

Self Cite

149

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Context. Core collapse supernovae (CCSNe) are important sources of interstellar dust, which are potentially capable of producing 1 M of dust in their explosively expelled ejecta. However, unlike other dust sources, the dust has to survive the passage of the reverse shock, generated by the interaction of the supernova blast wave with its surrounding medium. Knowledge of the net amount of dust produced by CCSNe is crucial for understanding the origin and evolution of dust in the local and high-redshift Universe. Aims. We identify the dust destruction mechanisms in the ejecta and derive the net amount of dust that survives the passage of the reverse shock. Methods. We use analytical models for the evolution of a supernova blast wave and of the reverse shock with special application to the clumpy ejecta of the remnant of Cassiopeia A (Cas A). We assume that the dust resides in cool oxygen-rich clumps, which are uniformly distributed within the remnant and surrounded by a hot X-ray emitting plasma (smooth ejecta), and that the dust consists of silicates (MgSiO 3 ) and amorphous carbon grains. The passage of the reverse shock through the clumps gives rise to a relative gas-grain motion and also destroys the clumps. While residing in the ejecta clouds, dust is processed via kinetic sputtering, which is terminated either when the grains escape the clumps or when the clumps are destroyed by the reverse shock. In either case, grain destruction proceeds thereafter by thermal sputtering in the hot shocked smooth ejecta. Results. We find that 11.8 and 15.9 percent of silicate and carbon dust, respectively, survive the passage of the reverse shock by the time the shock has reached the centre of the remnant. These fractions depend on the morphology of the ejecta and the medium into which the remnant is expanding, as well as the composition and size distribution of the grains that formed in the ejecta. Results will therefore differ for different types of supernovae.

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Section: Introductionsupporting

confidence: 54%

Dust destruction by the reverse shock in the Cassiopeia A supernova remnant

Micelotta

Dwek

Slavin

2016

A&A

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149

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“…For example, it is possible that the efficiency of dust destruction depends on environment in a more complex manner than we have represented in our model. Furthermore, there might be a metallicity dependence to the efficiency of dust destruction (Yamasawa et al 2011). Temim et al (2015 found the dust destruction rate in the Large Magellanic cloud to be lower than in the Small Magellanic Cloud.…”

Section: Insights From Comparing Model Variantsmentioning

confidence: 99%

The dust content of galaxies from z = 0 to z = 9

Popping

Somerville

Galametz

2017

Monthly Notices of the Royal Astronomical Society

238

326

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We study the dust content of galaxies from z = 0 to z = 9 in semi-analytic models of galaxy formation that include new recipes to track the production and destruction of dust. We include condensation of dust in stellar ejecta, the growth of dust in the interstellar medium (ISM), the destruction of dust by supernovae and in the hot halo, and dusty winds and inflows. The rate of dust growth in the ISM depends on the metallicity and density of molecular clouds. Our fiducial model reproduces the relation between dust mass and stellar mass from z = 0 to z = 7, the number density of galaxies with dust masses less than 10 8.3 M , and the cosmic density of dust at z = 0. The model accounts for the double power-law trend between dust-togas (DTG) ratio and gas-phase metallicity of local galaxies and the relation between DTG ratio and stellar mass. The dominant mode of dust formation is dust growth in the ISM, except for galaxies with M * < 10 7 M , where condensation of dust in supernova ejecta dominates. The dust-to-metal ratio of galaxies depends on the gasphase metallicity, unlike what is typically assumed in cosmological simulations. Model variants including higher condensation efficiencies, a fixed timescale for dust growth in the ISM, or no growth at all reproduce some of the observed constraints, but fail to simultaneously reproduce the shape of dust scaling relations and the dust mass of high-redshift galaxies.

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“…To match the observed dust mass function at z > 1, we might need a prescription for dust production and destruction that allows more variation with galaxy properties, therefore evolving with time. For example, dust production in the ejecta of SN may be higher at early times (Dwek et al 2014), or destruction rate varies with the ambient gas density and metallicity (Temim et al 2015).…”

Section: Dust Mass Functionmentioning

confidence: 99%

The origin of dust in galaxies across cosmic time

Triani

Sinha

Croton

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the dust evolution in galaxies by implementing a detailed dust prescription in the SAGE semi-analytical model for galaxy formation. The new model, called Dusty SAGE, follows the condensation of dust in the ejecta of type II supernovae and asymptotic giant branch (AGB) stars, grain growth in the dense molecular clouds, destruction by supernovae shocks, and the removal of dust from the ISM by star formation, reheating, inflows and outflows. Our model successfully reproduces the observed dust mass function at redshift z = 0 and the observed scaling relations for dust across a wide range of redshifts. We find that the dust mass content in the present Universe is mainly produced via grain growth in the interstellar medium (ISM). By contrast, in the early Universe, the primary production mechanism for dust is the condensation in stellar ejecta. The shift of the significant production channel for dust characterises the scaling relations of dust-to-gas (DTG) and dust-to-metal (DTM) ratios. In galaxies where the grain growth dominates, we find positive correlations for DTG and DTM ratios with both metallicity and stellar mass. On the other hand, in galaxies where dust is produced primarily via condensation, we find negative or no correlation for DTM and DTG ratios with either metallicity or stellar mass. In agreement with observation showing that the circumgalactic medium (CGM) contains more dust than the ISM, our model also shows the same trend for z < 4. Our semi-analytic model is publicly available at https://github.com/dptriani/dusty-sage.

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Dust Destruction Rates and Lifetimes in the Magellanic Clouds

Cited by 72 publications

References 98 publications

Dust destruction by the reverse shock in the Cassiopeia A supernova remnant

Dust destruction by the reverse shock in the Cassiopeia A supernova remnant

The dust content of galaxies from z = 0 to z = 9

The origin of dust in galaxies across cosmic time

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