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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We examine rare evolutionary routes of binary systems where the initiallymore massive primary star of ~5.5-8.5Mo, forms a white dwarf (WD), while thesecondary star of 4Mo < M_2,0 < M_1,0 accretes mass from the evolved primaryand later terminates as a core collapse supernova (CCSN). In such a WD-NSreverse evolution a neutron star (NS) or a potential NS-progenitor massive coreis formed after the WD. These SN explosions are likely to be preceded by stronginteraction of the WD with the giant secondary's core, leading to anIntermediate-Luminosity Optical Transient (ILOT; Red Transient; Red Nova)event, weeks to years before the explosion. The common envelope phase of the WDand the giant ends with a merger that forms an ILOT, or an envelope ejectionthat leads, after a CCSN of the giant's core, to a NS-NS or WD-NS survivingbinary. The WD could suffer a thermonuclear explosion, that might be observedas a Type Ia SN. Most of these CCSN and thermonuclear explosions will bepeculiar. We calculate the stellar evolution of representative cases usingModules for Experiments in Stellar Astrophysics (MESA). The occurrence rate ofthese systems is ~3-5 percent of that of CCSNe.

A pre-explosion optical transient event from a white dwarf merger with a giant supernova progenitor