1 code implementation • 4 Mar 2021 • Federico García, Adolfo Simaz Bunzel, Sylvain Chaty, Edward Porter, Eric Chassande-Mottin
All the progenitors follow a similar evolutionary path, starting from binaries with initial separations in the $30-200~R_\odot$ range, experiencing a stable mass transfer interaction before the formation of the first BH, and a second unstable mass-transfer episode leading to a CE ejection that occurs either when the secondary star crosses the Hertzsprung gap or when it is burning He in its core.
High Energy Astrophysical Phenomena Solar and Stellar Astrophysics
no code implementations • 18 Dec 2020 • Federico García, Mariano Méndez, Konstantinos Karpouzas, Tomaso Belloni, Liang Zhang, Diego Altamirano
The data show a strong type-B QPO at ~4. 5 Hz with increasing fractional rms amplitude with energy and positive lags with respect to a reference band at 2-2. 5 keV.
High Energy Astrophysical Phenomena
