Enhanced angular-momentum loss via outer-Lagrangian mass ejection shifts the ELM white-dwarf mass–period relation downward and reproduces most observed short-period systems.
Reconstructing the evolution of double helium white dwarfs: envelope loss without spiral-in
4 Pith papers cite this work, alongside 44 external citations. Polarity classification is still indexing.
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abstract
The unique core-mass - radius relation for giants with degenerate helium cores enables us to reconstruct the evolution of three observed double helium white dwarfs with known masses of both components. The last mass transfer phase in their evolution must have been a spiral-in. In the formalism proposed by Webbink (1984), we can constrain the efficiency of the deposition of orbital energy into the envelope to be $1 \la \alpha \la 6$, for an envelope structure parameter $\lambda=0.5$. We find that the two standard mass transfer types (stable mass transfer and spiral-in) are both unable to explain the first phase of mass transfer for these three binaries. We use a parametric approach to describe mass transfer in low-mass binaries, where both stars are of comparable mass and find that the orbital characteristics of the observed double helium white dwarfs can be well reproduced if the envelope of the primary is lost with ~1.5 times the specific angular momentum of the initial binary. In this case no substantial spiral-in occurs.
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astro-ph.SR 4years
2026 4representative citing papers
Binary evolution modeling constrains donor masses of 14-23 solar masses for two luminous red novae and shows dust masses are 1-5 orders of magnitude below total ejected envelope masses.
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.
citing papers explorer
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Formation of Extremely Low-mass White Dwarf Binaries Undergoing Enhanced Angular Momentum Loss
Enhanced angular-momentum loss via outer-Lagrangian mass ejection shifts the ELM white-dwarf mass–period relation downward and reproduces most observed short-period systems.
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Comparative Study of Two Luminous Red Novae I. Progenitor Modeling and Dust Formation
Binary evolution modeling constrains donor masses of 14-23 solar masses for two luminous red novae and shows dust masses are 1-5 orders of magnitude below total ejected envelope masses.
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A Path to Constraints on Common Envelope Ejection in Massive Binaries: Full Evolutionary Reconstruction of Three Black Hole X-ray Binaries
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.
- The Best Guess: Testing new and old formalisms for the common envelope against observations