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

Prior to the incineration of a white dwarf (WD) that makes a Type Iasupernova (SN Ia), the star "simmers" for ~1000 years in a convecting, carbonburning region. We have found that weak interactions during this time increasethe neutron excess by an amount that depends on the total quantity of carbonburned prior to the explosion. This contribution is in addition to themetallicity (Z) dependent neutronization through the 22Ne abundance (as studiedby Timmes, Brown, & Truran). The main consequence is that we expect a floor tothe level of neutronization that dominates over the metallicity contributionwhen Z/Z_\odot<2/3, and it can be important for even larger metallicities ifsubstantial energy is lost to neutrinos via the convective Urca process. Thiswould mask any correlations between SN Ia properties and galactic environmentsat low metallicities. In addition, we show that recent observations of thedependences of SNe Ia on galactic environments make it clear that metallicityalone cannot provide for the full observed diversity of events.

Neutronization During Type Ia Supernova Simmering