English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Classical novae are explosive phenomena that take place in stellar binarysystems. They are powered by mass transfer from a low-mass, main sequence staronto a white dwarf. The material piles up under degenerate conditions and athermonuclear runaway ensues. The energy released by the suite of nuclearprocesses operating at the envelope heats the material up to peak temperaturesof ~ (1 - 4) \times 108 K. During these events, about 10-4 - 10-5 M\odot,enriched in CNO and other intermediate-mass elements, are ejected into theinterstellar medium. To account for the gross observational properties ofclassical novae (in particular, a metallicity enhancement in the ejecta abovesolar values), numerical models assume mixing between the (solar-like) materialtransferred from the companion and the outermost layers (CO- or ONe-rich) ofthe underlying white dwarf. The nature of the mixing mechanism that operates atthe core-envelope interface has puzzled stellar modelers for about 40 years.Here we investigate the role of Kelvin-Helmholtz instabilities as a naturalmechanism for self-enrichment of the accreted envelope with core material. Thefeasibility of this mechanism is studied by means of the multidimensional codeFLASH. Here, we present a series of 9 numerical simulations perfomed in twodimensions aimed at testing the possible influence of the initial perturbation(duration, strength, location, and size), the resolution adopted, or the sizeof the computational domain on the results. We show that results do not dependsubstantially on the specific choice of these parameters, demonstrating thatKelvin- Helmholtz instabilities can naturally lead to self-enrichment of theaccreted envelope with core material, at levels that agree with observations.

Mixing in classical novae: a 2-D sensitivity study