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

A number of metal-rich white dwarfs (WDs) are known to host compact, denseparticle disks, which are thought to be responsible for metal pollution ofthese stars. In many such systems the inner radii of disks inferred from theirspectra are so close to the WD that particles directly exposed to starlightmust be heated above 1500 K and are expected to be unstable againstsublimation. To reconcile this expectation with observations we exploreparticle sublimation in H-poor debris disks around WDs. We show that because ofthe high metal vapor pressure the characteristic sublimation temperature inthese disks is 300-400 K higher than in their protoplanetary analogues,allowing particles to survive at higher temperatures. We then look at thestructure of the inner edges of debris disks and show that they shouldgenerically feature superheated inner rims directly exposed to starlight withtemperatures reaching 2500-3500 K. Particles migrating through the rim towardsthe WD (and rapidly sublimating) shield the disk behind them from strongstellar heating, making the survival of solids possible close to the WD. Ourmodel agrees well with observations of WD+disk systems provided that diskparticles are composed of Si-rich material such as olivine, and have sizes inthe range ~(0.03-30) cm.

Inner edges of compact debris disks around metal-rich white dwarfs