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

The identity of the progenitor systems of SNe Ia is still uncertain. In thesingle-degenerate (SD) scenario, the interaction between the SN blast wave andthe outer layers of a main sequence (MS) companion star strips off H-richmaterial which is then mixed into the ejecta. Strong contamination of the SNejecta with stripped material could lead to a conflict with observations of SNeIa. This constrains the SD progenitor model. In this work, our previoussimulations based on simplified progenitor donor stars have been updated byadopting more realistic progenitor-system models that result from fullydetailed, state-of-the-art binary evolution calculations. We use Eggleton'sstellar evolution code including the optically thick accretion wind model andthe possibility of the effects of accretion disk instabilities to obtainrealistic models of companions for different progenitor systems. The impact ofthe SN blast wave on these companion stars is followed in three-dimensionalhydrodynamic simulations employing the SPH code GADGET3. We find that thestripped masses range from 0.11 to 0.18 M_sun. The kick velocity is between 51and 105 km/s. We find that the stripped mass and kick velocity depend on theratio of the orbital separation to the radius of a companion. They can befitted by a power law for a given companion model. However, the structure ofthe companion star is also important for the amount of stripped material. Withmore realistic companion star models than in previous studies, our simulationsshow that the H masses stripped from companions are inconsistent with the bestobservational limits (< 0.01 M_sun) derived from nebular spectra. However, arigorous forward modeling based on impact simulations with radiation transferis required to reliably predict observable signatures of the stripped H and toconclusively assess the viability of the considered SN Ia progenitor scenario.

Three-dimensional simulations of the interaction between Type Ia supernova ejecta and their main sequence companions