The mass, location, and heating of the dust in the Cassiopeia A supernova remnant

Priestley, F. D.; Barlow, M. J.

doi:10.1093/mnras/stz414

Cited by 45 publications

(104 citation statements)

References 77 publications

(180 reference statements)

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“…Compared to the heavy element mass predicted by nucleosynthesis models (0.42 M , for a 11 M progenitor star, Woosley & Weaver 1995), the modelled dust masses for "a-C" grains correspond to a dust condensation efficiency of 8-12%. The inferred dust condensation efficiency is consistent with estimates of the dust condensation efficiency for Cassiopeia A (0.1-0.17, Nozawa et al 2010;Raymond et al 2018;Priestley et al 2019).…”

Section: Supernova Dust Emission and Extinctionsupporting

confidence: 83%

The dust content of the Crab Nebula

Looze

Barlow

Bandiera

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We have modelled the near-infrared to radio images of the Crab Nebula with a Bayesian SED model to simultaneously fit its synchrotron, interstellar and supernova dust emission. We infer an interstellar dust extinction map with an average A V = 1.08 ± 0.38 mag, consistent with a small contribution ( 22%) to the Crab's overall infrared emission. The Crab's supernova dust mass is estimated to be between 0.032 and 0.049 M (for amorphous carbon grains) with an average dust temperature T dust =41±3 K, corresponding to a dust condensation efficiency of 8-12%. This revised dust mass is up to an order of magnitude lower than some previous estimates, which can be attributed to our different interstellar dust corrections, lower SPIRE flux densities, and higher dust temperatures than were used in previous studies. The dust within the Crab is predominantly found in dense filaments south of the pulsar, with an average V band dust extinction of A V = 0.20 − 0.39 mag, consistent with recent optical dust extinction studies. The modelled synchrotron power-law spectrum is consistent with a radio spectral index α radio =0.297±0.009 and an infrared spectral index α IR =0.429±0.021. We have identified a millimetre excess emission in the Crab's central regions, and argue that it most likely results from two distinct populations of synchrotron emitting particles. We conclude that the Crab's efficient dust condensation (8-12%) provides further evidence for a scenario where supernovae can provide substantial contributions to the interstellar dust budgets in galaxies.

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Section: Supernova Dust Emission and Extinctionsupporting

confidence: 83%

The dust content of the Crab Nebula

Looze

Barlow

Bandiera

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…. 10 −5 Hou et al 2019) and super novae ejecta (Priestley et al 2019). The dustto-gas ratio changes with temperature for systems in thermal equilibrium and the maximum values in thermal equilibrium are (ρ d /ρ) ThE ≈ 0.004 .…”

Section: Mapping Seed Formation Mean Grain Sizes and Dust-to-gas Ratiosmentioning

confidence: 95%

Understanding the atmospheric properties and chemical composition of the ultra-hot Jupiter HAT-P-7b

Helling

Iro

Corrales

et al. 2019

A&A

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Context. Of the presently known ≈ 3900 exoplanets, sparse spectral observations are available for ≈ 100. Ultra-hot Jupiters have recently attracted interest from observers and theoreticians alike, as they provide observationally accessible test cases. Aims. We aim to study cloud formation on the ultra-hot Jupiter HAT-P-7b, the resulting composition of the local gas phase, and how their global changes affect wavelength-dependent observations utilised to derive fundamental properties of the planet. Methods. We apply a hierarchical modelling approach as a virtual laboratory to study cloud formation and gas-phase chemistry. We utilise 97 vertical 1D profiles of a 3D GCM for HAT-P-7b to evaluate our kinetic cloud formation model consistently with the local equilibrium gas-phase composition. We use maps and slice views to provide a global understanding of the cloud and gas chemistry. Results. The day/night temperature difference on HAT-P-7b (∆T ≈ 2500 K) causes clouds to form on the nightside (dominated by H 2 /He) while the dayside (dominated by H/He) retains cloud-free equatorial regions. The cloud particles vary in composition and size throughout the vertical extension of the cloud, but also globally. TiO 2 [s]/Al 2 O 3 [s]/CaTiO 3 [s]-particles of cm-sized radii occur in the higher dayside-latitudes, resulting in a dayside dominated by gas-phase opacity. The opacity on the nightside, however, is dominated by 0.01 . . . 0.1 µm particles made of a material mix dominated by silicates. The gas pressure at which the atmosphere becomes optically thick is ∼ 10 −4 bar in cloudy regions, and ∼ 0.1 bar in cloud-free regions. Conclusions. HAT-P-7b features strong morning/evening terminator asymmetries, providing an example of patchy clouds and azimuthally-inhomogeneous chemistry. Variable terminator properties may be accessible by ingress/egress transmission photometry (e.g., CHEOPS and PLATO) or spectroscopy. The large temperature differences of ≈2500 K result in an increasing geometrical extension from the night-to the dayside. The chemcial equilibrium H 2 O abundance at the terminator changes by < 1 dex with altitude and 0.3 dex (a factor of 2) across the terminator for a given pressure, indicating that H 2 O abundances derived from transmission spectra can be representative of the well-mixed metallicity at P 10 bar. We suggest the atmospheric C/O as an important tool to trace the presence and location of clouds in exoplanet atmospheres. The atmospheric C/O can be sub-and supersolar due to cloud formation. Phase curve variability of HAT-P-7b is unlikely to be caused by dayside clouds.

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“…In our model, we initially assume a homogeneous dust distribution within the clump, while the ambient medium is dust-free. The gas-to-dust mass ratio in the clump is set to ∆ gd = 10 which was obtained from SED modelling of the infra-red continuum emission of Cas A (Priestley et al 2019b).…”

Section: The New External Dust-processing Code Paperboatsmentioning

confidence: 99%

Dust survival rates in clumps passing through the Cas A reverse shock – I. Results for a range of clump densities

Kirchschlager

Schmidt

Barlow

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The reverse shock in the ejecta of core-collapse supernovae is potentially able to destroy newly formed dust material. In order to determine dust survival rates, we have performed a set of hydrodynamic simulations using the grid-based code AstroBEAR in order to model a shock wave interacting with clumpy supernova ejecta. Dust motions and destruction rates were computed using our newly developed external, postprocessing code Paperboats, which includes gas drag, grain charging, sputtering and grain-grain collisions. We have determined dust destruction rates for the oxygen-rich supernova remnant Cassiopeia A as a function of initial grain sizes and clump gas density. We found that up to 30 % of the carbon dust mass is able to survive the passage of the reverse shock if the initial grain size distribution is narrow with radii around ∼ 10 − 50 nm for high gas densities, or with radii around ∼ 0.5 − 1.5 µm for low and medium gas densities. Silicate grains with initial radii around 10 − 30 nm show survival rates of up to 40 % for medium and high density contrasts, while silicate material with micron sized distributions is mostly destroyed. For both materials, the surviving dust mass is rearranged into a new size distribution that can be approximated by two components: a power-law distribution of small grains and a log-normal distribution of grains having the same size range as the initial distribution. Our results show that grain-grain collisions and sputtering are synergistic and that grain-grain collisions can play a crucial role in determining the surviving dust budget in supernova remnants.

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The mass, location, and heating of the dust in the Cassiopeia A supernova remnant

Cited by 45 publications

References 77 publications

The dust content of the Crab Nebula

The dust content of the Crab Nebula

Understanding the atmospheric properties and chemical composition of the ultra-hot Jupiter HAT-P-7b

Dust survival rates in clumps passing through the Cas A reverse shock – I. Results for a range of clump densities

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