Description du projet
Une étude pourrait nous éclairer sur la formation et l’évolution des trous noirs de taille intermédiaire
Les trous noirs de masse intermédiaire (TNMI) constituent le chaînon manquant entre les trous noirs supermassifs, situés au centre des galaxies, et les trous noirs stellaires formés par l’effondrement gravitationnel d’une étoile. Les études existantes sont limitées dans leur capacité à analyser l’espace des paramètres et à saisir la physique complexe à l’origine des TNMI. Financé par le programme Actions Marie Skłodowska-Curie, le projet GRACE-BH combinera des techniques numériques et semi-analytiques de pointe pour modéliser la survie des graines de TNMI dans différents environnements et décrire de manière plus précise les conditions qui favorisent la formation des TNMI dans les amas stellaires. Plus particulièrement, le projet s’intéressera à l’incidence des interactions dynamiques, des collisions par emballement, de l’instabilité des paires et des poussées relativistes sur la formation des TNMI.
Objectif
The discovery of gravitational waves (GWs) marks the dawn of a new era for astronomy. On 2019 May 21, the gravitational-wave (GW) detectors LIGO and Virgo observed the coalescence of a massive binary black hole: the merger remnant of GW190521 is the first intermediate-mass black hole (IMBH) observed through GWs. This opens new perspectives for the study of IMBHs, bridging the gap between stellar-mass and supermassive black holes. The interpretation of current and future observations requires a theoretical framework capable of modelling both the formation of IMBHs and their co-evolution with the host star clusters. Numerical simulations offer a unique tool to model IMBHs from the seeding phase to their full growth. However, the existing literature misses a thorough study that fully explores the parameter space and captures the complex physics behind IMBHs.
Including these aspects represents a fundamental step to bridge stellar dynamics and GW astronomy. The GRACE-BH project aims at building such a bridge providing a solution to one of the challenging questions of modern astrophysics:
What are the best conditions favouring the formation of IMBHs in star clusters?
To address this open question, I will combine forefront numerical simulations and semi-analytic techniques to probe the
parameter space, focusing on the role of stellar multiplicity and primordial mass segregation in star clusters. I will model the complex physics associated with IMBH formation, investigating the impact of dynamical interactions, runaway collisions, pair-instability and relativistic kicks on IMBH formation. The exploitation of these models will enable us to describe the survival and growth of IMBH seeds in different environments, shedding a light on the conditions that favour IMBH formation in star clusters. This will allow us to dissect the demography of GW sources powered by IMBHs and to make predictions for next-generation ground-based and spaceborne GW detectors like LISA.
Champ scientifique
- natural sciencesphysical sciencesastronomyobservational astronomygravitational waves
- natural sciencesbiological sciencesevolutionary biology
- natural sciencesphysical sciencesastronomyastrophysicsblack holes
- engineering and technologyelectrical engineering, electronic engineering, information engineeringelectronic engineeringcomputer hardwaresupercomputers
- natural sciencesphysical sciencesastronomystellar astronomy
Programme(s)
Régime de financement
MSCA-IF - Marie Skłodowska-Curie Individual Fellowships (IF)Coordinateur
67100 L'Aquila
Italie