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

Close binary systems undergoing mass transfer or common envelope interactionscan account for the morphological properties of some planetary nebulae. Thesearch for close binary companions in planetary nebulae is hindered by thedifficulty of detecting cool, late-type, main sequence companions in binarysystems with hot pre-white dwarf primaries. However, models of binary PNprogenitor systems predict that mass accretion or tidal interactions can inducerapid rotation in the companion, leading to X-ray-emitting coronae. To testsuch models, we have searched for, and detected, X-ray emission from threebinary central stars within planetary nebulae: the post-common envelope closebinaries in HFG 1 and DS 1 consisting of O-type subdwarfs with late-type, mainsequence companions, and the binary system in LoTr 5 consisting of O-typesubdwarf and rapidly rotating, late-type giant companion. The X-ray emission ineach case is best characterized by spectral models consisting of twooptically-thin thermal plasma components with characteristic temperatures ofabout 10 MK and 15-40 MK, and total X-ray luminosities about 10^30 erg/s. Weconsider the possible origin of the X-ray emission from these binary systemsand conclude that the most likely origin is, in each case, a corona around thelate-type companion, as predicted by models of interacting binaries.

X-ray Emission from the Binary Central Stars of the Planetary Nebulae HFG 1, DS 1, and LoTr 5