Dust in Supernovae and Supernova Remnants II: Processing and Survival

Micelotta, Elisabetta R.; Matsuura, M.; Sarangi, Aditya Narayan

doi:10.1007/s11214-018-0484-7

Cited by 26 publications

(11 citation statements)

References 198 publications

(459 reference statements)

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“…The collisional processing of PAHs by ions is present in interstellar shocks (Micelotta et al 2010). For supernovae remnants, such processing also occurs, and it has been studied for large dust grains (Micelotta et al 2018). Our results suggest that the non-dissociative multiple ionization is significantly more efficient upon the interaction with 2500 eV photons than by collision with protons and α-particles, and should take place in regions isolated from the hot gas of these shock waves.…”

Section: Production Of Multiply Charged Pahsmentioning

confidence: 69%

Destruction and multiple ionization of PAHs by X-rays in circumnuclear regions of AGNs

Monfredini

Quitián-Lara

Fantuzzi

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The infrared signatures of polycyclic aromatic hydrocarbons (PAHs) are observed in a variety of astrophysical objects, including the circumnuclear medium of active galactic nuclei (AGNs). These are sources of highly energetic photons (0.2 to 10 keV), exposing the PAHs to a harsh environment. In this work, we examined experimentally the photoionization and photostability of naphthalene (C 10 H 8 ), anthracene (C 14 H 10 ), 2methyl-anthracene (C 14 H 9 CH 3 ) and pyrene (C 16 H 10 ) upon interaction with photons of 275, 310 and 2500 eV. The measurements were performed at the Brazilian Synchrotron Light Laboratory using time-of-flight mass-spectrometry (TOF-MS). We determined the absolute photoionization and photodissociation cross sections as a function of the incident photon energy; the production rates of singly, doubly and triply charged ions; and the molecular half-lives in regions surrounding AGNs. Even considering moderate X-ray optical depth values (τ = 4.45) due to attenuation by the dusty torus, the halflives are not long enough to account for PAH detection. Our results suggest that a more sophisticated interplay between PAHs and dust grains should be present in order to circumvent molecular destruction. We could not see any significant difference in the half-life values by increasing the size of the PAH carbon backbone, N C , from 10 to 16. However, we show that the multiple photoionization rates are significantly greater than the single ones, irrespective of the AGN source. We suggest that an enrichment of multiply charged ions caused by X-rays can occur in AGNs.

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Section: Production Of Multiply Charged Pahsmentioning

confidence: 69%

Destruction and multiple ionization of PAHs by X-rays in circumnuclear regions of AGNs

Monfredini

Quitián-Lara

Fantuzzi

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…In the following, we compare our results to previous studies of dust destruction in the ISM that mainly model dust sputtering in single SN shocks in a homogeneous ISM (see Micelotta, Matsuura & Sarangi 2018, for a review). Their estimates of M cl can be directly compared to our single SN results described in Sect.3.2.2.…”

Section: Comparison With Previous Workmentioning

confidence: 83%

Thermal and non-thermal dust sputtering in hydrodynamical simulations of the multiphase interstellar medium

Zhukovska

Somerville

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study the destruction of interstellar dust via sputtering in supernova (SN) shocks using three-dimensional hydrodynamical simulations. With a novel numerical framework, we follow both sputtering and dust dynamics governed by direct collisions, plasma drag and betatron acceleration. Grain-grain collisions are not included and the grain-size distribution is assumed to be fixed. The amount of dust destroyed per SN is quantified for a broad range of ambient densities and fitting formulae are provided. Integrated over the grain-size distribution, nonthermal (inertial) sputtering dominates over thermal sputtering for typical ambient densities. We present the first simulations that explicitly follow dust sputtering within a turbulent multiphase interstellar medium. We find that the dust destruction timescales τ are 0.35 Gyr for silicate dust and 0.44 Gyr for carbon dust in solar neighborhood conditions. The SN environment has an important impact on τ . SNe that occur in preexisting bubbles destroy less dust as the destruction is limited by the amount of dust in the shocked gas. This makes τ about 2.5 times longer than the estimate based on results from a single SN explosion. We investigate the evolution of the dust-to-gas mass ratio (DGR), and find that a spatial inhomogeneity of ∼ 14% develops for scales below 10 pc. It locally correlates positively with gas density but negatively with gas temperature even in the exterior of the bubbles due to incomplete gas mixing. This leads to a ∼ 30% lower DGR in the volume filling warm gas compared to that in the dense clouds.

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“…We note that the formal significance of theLakićević et al (2015) results is marginal and may be affected by warm dust preventing any cold dust present to be detected(Micelotta et al 2018). The short dust lifetimes obtained byTemim et al (2015) are based on the formalism ofDwek et al (2007) to calculate SN dust destruction efficiencies as a function of SN shock velocity.…”

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confidence: 99%

Maximally Dusty Star-forming Galaxies: Supernova Dust Production and Recycling in Local Group and High-redshift Galaxies

Gall

Hjorth

2018

ApJ

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Motivated by recent observations suggesting that core-collapse supernovae may on average produce ∼0.3 M of dust, we explore a simple dust production scenario which applies to star-forming galaxies in the local environment (the Magellanic Clouds and possibly the Milky Way) as well as to high redshift (sub-millimeter, QSO, Lyman break) galaxies. We assume that the net dust destruction (due to supernova reverse shock, shocks in the interstellar medium, or astration) is negligible on a timescale of 1 Gyr, in which case the dust mass can be estimated as 0.004 times the star-formation rate (for a Chabrier IMF) multiplied by the duration of the star-formation episode. The model can account for observed dust masses over four orders of magnitude and across the redshift range 0-8.4, with dust production rates spanning five orders of magnitudes. This suggests that starforming galaxies may be seen as maximally dusty, in the sense that a dominant fraction of the dust-forming elements forged in a supernova eventually will go into the solid phase. In turn, this indicates little destruction of supernova dust or almost complete replenishment, on a short time scale, of any dust that is destroyed.

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Dust in Supernovae and Supernova Remnants II: Processing and Survival

Cited by 26 publications

References 198 publications

Destruction and multiple ionization of PAHs by X-rays in circumnuclear regions of AGNs

Destruction and multiple ionization of PAHs by X-rays in circumnuclear regions of AGNs

Thermal and non-thermal dust sputtering in hydrodynamical simulations of the multiphase interstellar medium

Maximally Dusty Star-forming Galaxies: Supernova Dust Production and Recycling in Local Group and High-redshift Galaxies

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