Optical Properties of C$-$rich (${}^{12}$C, SiC and FeC) Dust Layered Structure of Massive Stars

Abstract

The composition and structure of interstellar dust are important and complex for the study of the evolution of stars and the \textbf{interstellar medium} (ISM). However, there is a lack of corresponding experimental data and model theories. By theoretical calculations based on ab-initio method, we have predicted and geometry optimized the structures of Carbon-rich (C-rich) dusts, carbon (${}^{12}$C), iron carbide (FeC), silicon carbide (SiC), even silicon (${}^{28}$Si), iron (${}^{56}$Fe), and investigated the optical absorption coefficients and emission coefficients of these materials in 0D (zero$-$dimensional), 1D, and 2D nanostructures. Comparing the \textbf{nebular spectra} of the supernovae (SN) with the coefficient of dust, we find that the optical absorption coefficient of the 2D ${}^{12}$C, ${}^{28}$Si, ${}^{56}$Fe, SiC and FeC structure corresponds to the absorption peak displayed in the infrared band (5$-$8) $\mu$$m$ of the spectrum at 7554 days after the SN1987A explosion. And it also corresponds to the spectrum of 535 days after the explosion of SN2018bsz, when the wavelength in the range of (0.2$-$0.8) and (3$-$10) $\mu$$m$. Nevertheless, 2D SiC and FeC corresponds to the spectrum of 844 days after the explosion of SN2010jl, when the wavelength is within (0.08$-$10) $\mu$$m$. Therefore, FeC and SiC may be the second type of dust in SN1987A corresponding to infrared band (5$-$8) $\mu$$m$ of dust and may be in the ejecta of SN2010jl and SN2018bsz.

References in corpus (23)

• The dust mass in Cassiopeia A from a spatially resolved Herschel analysis
• Excitation of Polycyclic Aromatic Hydrocarbon (PAH) Emission: Dependence on Size Distribution, Ionization, and Starlight Spectrum and Intensity
• Modelling Dust Evolution in Galaxies with a Multiphase, Inhomogeneous ISM
• Dust yields in clumpy SN shells: SN 1987A revisited
• Cassiopeia A: dust factory revealed via submillimetre polarimetry
• Dust masses for SN 1980K, SN1993J and Cassiopeia A from red-blue emission line asymmetries
• Near-Infrared and Optical Observations of Type Ic SN2020oi and broad-lined Ic SN2020bvc: Carbon Monoxide, Dust and High-Velocity Supernova Ejecta
• Low-temperature MIR to submillimeter mass absorption coefficient of interstellar dust analogues II: Mg and Fe-rich amorphous silicates
• The mass, location and heating of the dust in the Cassiopeia A supernova remnant
• Origin of large meteoritic SiC stardust grains in metal-rich AGB stars
• Condensation of SiC Stardust in CO Nova Outbursts
• Interstellar-Medium Mapping in M82 Through Light Echoes Around Supernova 2014J
• Formation of interstellar complex polycyclic aromatic hydrocarbons: Insights from molecular dynamics simulations of dehydrogenated benzene
• XSHOOTER spectroscopy of the enigmatic planetary nebula Lin49 in the Small Magellanic Cloud
• DFT study of five-membered ring PAHs
• Mid-infrared extinction and fresh silicate dust towards the Galactic Center
• TEM analyses of unusual presolar silicon carbide: Insights into the range of circumstellar dust condensation conditions
• SN 2018bsz: significant dust formation in a nearby superluminous supernova
• The Formation of Bimodal Dust Species in Nova Ejecta I: Chemical Conditions
• The Formation of Bimodal Dust Species in Nova Ejecta
• Heavy element contributions of rotating massive stars to Interstellar Medium
• Correlation among extinction efficiency and other parameters in an aggregate dust model
• Graphene Molecule Compared With Fullerene C60 As Circumstellar Carbon Dust Of Planetary Nebula

Cited by in corpus (1)

• Catalytic role of HI in the interstellar synthesis of complex organic molecule