Giovanni Mirouh
Gather.town id
CCE20
Poster Title
Detailed equilibrium and dynamical tides : impact on populations, cluster ages, and transient rates
Institution
University of Surrey
Abstract (short summary)
Binary stars evolve into chemically-peculiar objects or binary compact objects, releasing significant amounts of enriched gas, making them the main driver of the Galactic enrichment in heavy elements (and for some of those, the only driver). During their evolution, they go through a series of interactions, among which tides are the most common kind.
To pin down tidal interactions and the evolution of binary stars, we implement an updated prescription in the stellar population code binary_c. Relying on Zahn's theory of tides, and on grids of MESA main-sequence models covering an extensive mass range (0.1 to 320Msun), we use detailed structural quantities to derive the parameters lambda and E2 that rule equilibrium and dynamical tides respectively. We augment the ubiquitous BSE implementation by adding those parameters in the binary_c code.
I will present a few applications of this new determination of circularisation and synchronisation timescales: rates of stellar mergers, gamma-ray bursts and gravitational wave progenitors are updated, while the comparison between the derived and observed period-eccentricity diagrams for clusters provides an accurate estimate of their ages.
To pin down tidal interactions and the evolution of binary stars, we implement an updated prescription in the stellar population code binary_c. Relying on Zahn's theory of tides, and on grids of MESA main-sequence models covering an extensive mass range (0.1 to 320Msun), we use detailed structural quantities to derive the parameters lambda and E2 that rule equilibrium and dynamical tides respectively. We augment the ubiquitous BSE implementation by adding those parameters in the binary_c code.
I will present a few applications of this new determination of circularisation and synchronisation timescales: rates of stellar mergers, gamma-ray bursts and gravitational wave progenitors are updated, while the comparison between the derived and observed period-eccentricity diagrams for clusters provides an accurate estimate of their ages.
Plain text (extended) Summary
We compute stellar populations including binary systems. These systems interact, notably through tides, that can modify the orbits.
To compute these populations, we use the binary_c code which relies on a set of fitting relations to derive stellar parameters and compute evolutionary tracks at lightning speed.
Within the MINT framework, we modify this algorithm to rely on interpolations of state-of-the-art MESA grids and update tidal prescriptions.
We study circularisation for an application to stellar cluster ages. Most notably, we show a comparison with the 150-Myr cluster M35, observed by Meibom & Mathieu (2005). Our populations for which the use of our improved tides and appropriate initial distributions lead to a much improved statistical agreement with the observations. We will now benchmark our MINT prescriptions on other clusters and improve our age estimates.
To compute these populations, we use the binary_c code which relies on a set of fitting relations to derive stellar parameters and compute evolutionary tracks at lightning speed.
Within the MINT framework, we modify this algorithm to rely on interpolations of state-of-the-art MESA grids and update tidal prescriptions.
We study circularisation for an application to stellar cluster ages. Most notably, we show a comparison with the 150-Myr cluster M35, observed by Meibom & Mathieu (2005). Our populations for which the use of our improved tides and appropriate initial distributions lead to a much improved statistical agreement with the observations. We will now benchmark our MINT prescriptions on other clusters and improve our age estimates.
URL
g.mirouh@surrey.ac.uk
Poster file