Synthetic observables from tECSN models show slower early red-color decline due to higher Ti/Cr and a late-time 12.8 μm Ne II line that strengthens over time, unlike comparable CO deflagration models.
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Efficient mass transfer in binaries naturally limits the mass of the first-born black hole and produces a sharp drop above 45 solar masses that mimics the pair-instability gap.
Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.
Enhanced mass transfer stability explains the observed deficit of post-common-envelope binaries with solar-type companions, with inefficient common envelope evolution (alpha_CE=0.25) providing the best match when combined with magnetic braking and selection effects.
Multi-survey analysis of 157 hot subdwarf binaries yields 23 orbital solutions (11 new) whose mass-period distribution matches post-common-envelope systems, supporting a common-envelope origin.
Enhanced angular momentum loss via outer Lagrangian point mass ejection in the Roche lobe overflow channel alters ELM WD structure and reproduces observed shorter orbital periods.
Reconstruction of GRO J1655-40, SAX J1819.3-2525 and 4U 1543-47 requires CE efficiencies α_0.5U ≳6.7, α_U ≳4.2, α_H ≳1.7 with no solutions below unity, implying need for additional energy or formalism changes plus natal kicks ≳50 km/s for 4U 1543-47.
Gaia astrometry remains consistent with a binary origin for long secondary periods once sample contamination by semi-regular variables is accounted for.
The review identifies and discusses key unsolved problems in planetary nebulae such as 3D morphology, multipolar origins, dust distribution, binarity, and the abundance discrepancy, along with suggested future directions.
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Binary Evolution Can Mimic the Pair-Instability Mass Gap in Black Hole Mergers
Efficient mass transfer in binaries naturally limits the mass of the first-born black hole and produces a sharp drop above 45 solar masses that mimics the pair-instability gap.