Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.
The Binding Energy Parameter for Common Envelope Evolution
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abstract
The binding energy parameter $\lambda$ plays a vital role in common envelope evolution. Though it is well known that $\lambda$ takes different values for stars with different masses and varies during stellar evolution, it has been erroneously adopted as a constant in most of the population synthesis calculations. We have systematically calculated the values of $\lambda$ for stars of masses $1-60\,M_{\odot}$ by use of an updated stellar evolution code, taking into account contribution from both gravitational energy and internal energy to the binding energy of the envelope. We adopt the criterion for the core-envelope boundary advocated by \citet{Ivanova2011}. A new kind of $\lambda$ with the enthalpy prescription is also investigated. We present fitting formulae for the calculated values of various kinds of $\lambda$, which can be used in future population synthesis studies.
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UNVERDICTED 2representative citing papers
A review summarizing established modeling techniques, open questions, and research directions for three classes of LISA gravitational wave sources.
citing papers explorer
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Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models
Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.
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Astrophysics with the Laser Interferometer Space Antenna
A review summarizing established modeling techniques, open questions, and research directions for three classes of LISA gravitational wave sources.