The Formation of Bimodal Dust Species in Nova Ejecta I: Chemical Conditions

Abstract

The formation of bimodal dust species (that is, both of silicate and amorphous carbon dust grains are observed in a nova eruption) in nova ejecta is still debated. Using the Modules for Experiments in Stellar Astrophysics code and considering the effects of WD's mass, mass-accretion rate and the chemical profiles of WD which are described by new parameter --- mixing depth on the chemical abundances of nova ejecta, we investigate the possibility that bimodal dust species are produced in a nova eruption. We find that $C/O$ (the ratio of carbon number density to oxygen number density) of nova ejecta is affected by the mixing depth. For the model with a small mixing depth, the $C/O$ of nova ejecta can evolute from lager than 1.0 to smaller than 1.0 in a whole eruption, which provides the chemical condition for the formation of bimodal dust species.

13 pages, 7 figures, 4 Tables, accepted for publication in MNRAS

References in corpus (4)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Evolution of interstellar dust and stardust in the solar neighbourhood
• Population synthesis for symbiotic stars with white dwarf accretors
• Mid-infrared Spectroscopic Observations of the Dust-forming Classical Nova V2676 Oph

Cited by in corpus (5)

• Formation and Destiny of White Dwarf and Be Star Binaries
• Possible Formation Scenarios of ZTF J153932.16+502738.8-A Gravitational Source Close to the Peak of LISA's Sensitivity
• The Formation of Bimodal Dust Species in Nova Ejecta
• Optical Properties of C$-$rich (${}^{12}$C, SiC and FeC) Dust Layered Structure of Massive Stars
• Formation, diffusion and accreting pollution of DB white dwarfs