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The common-envelope phase is one of the most poorly understood phases of(binary) stellar evolution, in spite of its importance in the formation of awide-range of astrophysical phenomena ranging from cataclysmic variables tocosmologically important supernova type Ia, and even recently discoveredgravitational wave producing black hole mergers. The central star of theplanetary nebula NGC~2346 has long been held as one of the longest periodpost-common-envelope systems known with a published period of approximately 16days, however the data presented were also consistent with much shorter periodsof around 1 day (a more typical period among the known sample ofpost-common-envelope binary central stars). Here, using the modernhigh-stability, high-resolution spectrograph HERMES, we conclusively show theperiod to, indeed, be 16 days while also revising the surface gravity to avalue typical of a sub-giant (rather than main-sequence) resulting in anintrinsic luminosity consistent with the recently published GAIA parallaxdistance. Intriguingly, the implied mass for the secondary ($\gtrsim$3.5M$_\odot$) makes it, to our knowledge, the most massive post-common-envelopesecondary known, whilst also indicating that the primary may be a post-RGBstar.

On the post-common-envelope central star of the planetary nebula NGC 2346