Properties of interstellar dust responsible for extinction laws with unusually low total-to-selective extinction ratios of R=1−2

Nozawa, Takaya

doi:10.1016/j.pss.2016.08.006

Cited by 17 publications

(16 citation statements)

References 45 publications

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“…Another possible interpretation is that the low RV values are caused by dust in the interstellar (IS) medium. This would require IS clouds in the SN host galaxies to be characterized by smaller dust grains compared to those seen in our Galaxy (Gao et al 2015;Nozawa 2016), possibly as a consequence of cloud-cloud collisions induced by the SN radiation pressure (Hoang 2017). Evidences supporting the IS scenario were given by Phillips et al (2013) who found a strong correlation between the extinction of SNe Ia and the strength of a diffuse interstellar band at 5870Å.…”

Section: Introductionmentioning

confidence: 78%

Shedding light on the Type Ia supernova extinction puzzle: dust location found

Bulla

Goobar

Dhawan

2018

Monthly Notices of the Royal Astronomical Society

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The colour evolution of reddened Type Ia supernovae can place strong constraints on the location of dust and help address the question of whether the observed extinction stems from the interstellar medium or from circumstellar material surrounding the progenitor. Here we analyse BV photometry of 48 reddened Type Ia supernovae from the literature and estimate the dust location from their B−V colour evolution. We find a time-variable colour excess E(B − V ) for 15 supernovae in our sample and constrain dust to distances between 0.013 and 45 pc (4 × 10 16 − 10 20 cm). For the remaining supernovae, we obtain a constant E(B − V ) evolution and place lower limits on the dust distance from the explosion. In all the 48 supernovae, the inferred dust location is compatible with an interstellar origin for the extinction. This is corroborated by the observation that supernovae with relatively nearby dust ( 1 pc) are located close to the center of their host galaxy, in high-density dusty regions where interactions between the supernova radiation and interstellar clouds close by are likely to occur. For supernovae showing time-variable E(B − V ), we identify a potential preference for low R V values, unusually strong sodium absorption and blue-shifted and timevariable absorption features. Within the interstellar framework, this brings evidence to a proposed scenario where cloud-cloud collisions induced by the supernova radiation pressure can shift the grain size distribution to smaller values and enhance the abundance of sodium in the gaseous phase.

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Section: Introductionmentioning

confidence: 78%

Shedding light on the Type Ia supernova extinction puzzle: dust location found

Bulla

Goobar

Dhawan

2018

Monthly Notices of the Royal Astronomical Society

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“…polarization (λ max < 0.4 µm) for several SNe Ia 9,10 . Numerical modeling of dust extinction 11 and polarization curves 12 toward individual SNe Ia demonstrate that the anomalous values of R V and λ max can be reproduced by the enhancement in the relative abundance of small grains to large grains in the host galaxy.…”

Section: Introductionmentioning

confidence: 93%

Rotational disruption of dust grains by radiative torques in strong radiation fields

et al. 2019

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Massive stars, supernovae, and kilonovae are among the most luminous radiation sources in the universe. Observations usually show near-to mid-infrared (NIR-MIR, λ ∼ 1 − 5 µm) emission excess from H II regions around young massive star clusters (YMSCs). Early phase observations in optical to NIR wavelengths of type Ia supernovae also reveal unusual properties of dust extinction and dust polarization. The popular explanation for such NIR-MIR excess and unusual dust properties is the predominance of small grains (size a 0.05 µm) relative to large grains (a 0.1 µm) in the local environment of these strong radiation sources.The question of why small grains are predominant in these environments remains a mystery. Here we report a new mechanism of dust destruction based on centrifugal stress within extremely fast-rotating grains spun-up by radiative torques, which we term the RAdiative Torque Disruption (RATD) mechanism. We find that RATD can disrupt large grains located 1 arXiv:1810.05557v2 [astro-ph.GA] 7 May 2019 within a distance of ∼ 1 pc from a massive star of luminosity L ∼ 10 4 L or a supernova. This effect increases the abundance of small grains relative to large grains and successfully reproduces the observed NIR-MIR excess and anomalous dust extinction/polarization. We apply the RATD mechanism for kilonovae and find that dust within ∼ 0.1 pc would be dominated by small grains. Small grains produced by RATD can also explain the steep far-UV rise in extinction curves toward starburst and high redshift galaxies, and the decrease of the escape fraction of Lyα photons from H II regions surrounding YMSCs.

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“…Another possibility for this dispersion is grain growth. The ratio of total-to-selective extinction, R V , is generally correlated with grain size (Nozawa 2016;Cardelli et al 1988). Estimates of R V for the low-extinction line-of-sight sample (Table 1) are found using spectral classifications (Wright et al 2003) and optical and NIR photometry (Høg et al 2000;Skrutskie et al 2006).…”

Section: Dispersion In λ Max (A V )mentioning

confidence: 99%

Probing Interstellar Grain Growth through Polarimetry in the Taurus Cloud Complex

Vaillancourt

Andersson

Clemens

et al. 2020

ApJ

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The optical and near-infrared (OIR) polarization of starlight is typically understood to arise from the dichroic extinction of that light by dust grains whose axes are aligned with respect to a local magnetic field. The size distribution of the aligned grain population can be constrained by measurements of the wavelength dependence of the polarization. The leading physical model for producing the alignment is that of radiative alignment torques (RAT), which predicts that the most efficiently aligned grains are those with sizes larger than the wavelengths of light composing the local radiation field. Therefore, for a given grain size distribution, the wavelength at which the polarization reaches a maximum (λ max) should correlate with the characteristic reddening along the line of sight between the dust grains and the illumination source. A correlation between λ max and reddening has been previously established for extinctions up to A V ≈ 4 mag. We extend the study of this relationship to a larger sample of stars in the Taurus cloud complex, including extinctions A V > 10 mag. We confirm the earlier results for A V < 4 mag, but find that the λ max vs. A V relationship bifurcates above A V ≈ 4 mag, with part of the sample continuing the previously observed relationship. The remaining sample exhibits a steeper rise in λ max vs. A V. We propose that the data exhibiting the steep rise represent lines of sight of high-density "clumps", where grain coagulation has taken place. We present RAT-based modeling supporting these hypotheses. These results indicate that multi-band OIR polarimetry is a powerful tool for tracing grain growth in molecular clouds, independent of uncertainties in the dust temperature and emissivity.

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Properties of interstellar dust responsible for extinction laws with unusually low total-to-selective extinction ratios of R=1−2

Cited by 17 publications

References 45 publications

Shedding light on the Type Ia supernova extinction puzzle: dust location found

Shedding light on the Type Ia supernova extinction puzzle: dust location found

Rotational disruption of dust grains by radiative torques in strong radiation fields

Probing Interstellar Grain Growth through Polarimetry in the Taurus Cloud Complex

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