First ALMA observations of the Arches cluster yield mass-loss rates for WN and O stars plus evidence for radially decreasing wind clumping from combined radio-mm spectral indices.
@doi [ ] 10.1051/0004-6361/201731902, https://ui.adsabs.harvard.edu/abs/2017A&A...607L...8V 607
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Binary population synthesis predicts several thousand intermediate-mass helium stars in the Milky Way, mostly in binaries, with metallicity and common-envelope ejection efficiency as the dominant shaping factors.
Population synthesis of helium star-NS systems yields DNS delay time distributions that peak between 80-250 Myr across metallicities, with 15% merging within 80 Myr and over 20% after 1 Gyr.
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.
Population synthesis of pulsar-massive star binaries yields an estimate for the number of observable VHE gamma-ray sources in the Galaxy, incorporating anisotropic wind-interaction zones.
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How many VHE gamma-ray binaries with young pulsars can be observed?
Population synthesis of pulsar-massive star binaries yields an estimate for the number of observable VHE gamma-ray sources in the Galaxy, incorporating anisotropic wind-interaction zones.