The Formation of Bimodal Dust Species in Nova Ejecta

Abstract

The formation of bimodal dust species (namely the silicate and amorphous carbon dust grains coexistent) in a nova eruption is an open problem. According to the nova model simulated by Modules for Experiments in Stellar Astrophysics code, we calculate the formation and growth carbon (C) and forsterite (Mg 2 SiO 4 ) dust grains in nova ejecta for the free-expansion model and the radiative shock model, respectively. In the free-expansion model, the nova ejecta is not an idea environment for dust nucleation. However, it can efficiently produce dust in the radiative shock model. We estimate that every nova can produce C grains with an average mass of about 10 −9 and 10 −8 M ⊙ , and Mg 2 SiO 4 grains with an average mass of about 10 −8 and 10 −7 M ⊙ . Based on the mass of ejected gas, the ratio of dust to gas is about 1%. The C grains form first after several or tens of days of nova eruption. After that, the Mg 2 SiO 4 grains begin to grow in tens of days, which is consistent with observations.

Radiation Spectral Analysis of 3D Dust Molecular Clusters (PAHs) and Peptoids under Ionization and Electric Field in ISM

“…During the post-asymptotic giant branch (post-AGB) stellar period, traces of PAHs can be found in the stellar spectrum as the stellar temperature increases. The reason is that PAHs require energy provided by ultraviolet (UV) or optical radiation to support their radiation energy to form the infrared spectrum (Tielens 2008;Zhu et al 2013;Sarangi et al 2018;Duolikun et al 2019;Marassi et al 2019;Zhu et al 2019;Rho et al 2021;Wu et al 2021;Cinquegrana & Karakas 2022).…”

Optical Properties of C-rich (12C, SiC and FeC) Dust Layered Structure of Massive Stars*

“…It absorbs optical and ultraviolet (UV) radiation and emit into infrared, and it also affects the spectral energy distribution in the cosmic environment (e.g., Gould et al 1963;Cazaux & Tielens 2004). Dust is known to form in supernova remnant (SNR) that is rich in heavy elements, in the stellar wind of asymptotic giant branch (AGB) stars, and in nova ejecta for theoretical research (Zhu et al 2013;Iliadis et al 2018;Bose & Starrfield 2019;Duolikun et al 2019;Zhu et al 2019;Gail et al 2020;Lugaro et al 2020). Recent years observations indicate that dust can be effectively formed in supernovae (SN) ejecta (Barlow et al 2010;Dwek et al 2010;Gomez et al 2012;Indebetouw et al 2014;Bevan & Barlow 2016;De Looze et al 2017;Sarangi et al 2018;Rho et al 2021), a large number of observation strategies have obtained the high dust mass between ∼0.1M e and 1M e (Dunne et al 2009;Sibthorpe et al 2010;Bevan et al 2017;De Looze et al 2017;Priestley et al 2019).…”

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

“…It absorbs optical and ultraviolet (UV) radiation and emit into infrared, it also affects the spectral energy distribution in the cosmic environment (e. g., Gould et al 1963;Cazaux & Tielens 2004). Dust is known to form in supernova remnant (SNR) that is rich in heavy elements, in the stellar wind of asymptotic giant branch (AGB) stars, and in nova ejecta for theoretical research (Zhu et al 2013;Iliadis et al 2018;Bose & Starrfield 2019;Zhu et al 2019;Duolikun et al 2019;Gail et al 2020;Lugaro et al 2020). Recent years observations indicate that dust can be effectively formed in supernovae (SN) ejecta (Barlow et al 2010;Dwek et al 2010;Gomez et al 2012;Indebetouw et al 2014;Bevan & Barlow 2016;De Looze et al 2017;Sarangi et al 2018;Rho et al 2021), a large number of observation strategies have obtained the high dust mass between ∼ 0.1M ⊙ and 1M ⊙ (Dunne et al 2009;Sibthorpe et al 2010;De Looze et al 2017;Bevan et al 2017;Priestley et al 2019).…”

“…Here, we simulate the nano−layered structure of FeC and SiC in 0D, 1D and 2D in the SNR, the structures of dust including metallic needles (Dwek 2004), multi−layered particles (Voshchinnikov et al 2017), hydrogenated nanotubes (HNT) molecular growth (Chen & Li 2019), spherical (Fischera 2004;Demyk et al 2017;Gail et al 2020). Marassi et al (2019) and Optical Properties of C−rich Dust 3 Kirchschlager et al (2020) groups have studied the dust mass in the SNR, furthermore, some groups research the spectral of the iron and silicates dust (Maldoni et al 2005;Gail et al 2020).…”