Hypermassive neutron stars: from numerical relativity simulations to gamma-ray data
APA
Chirenti, C. (2023). Hypermassive neutron stars: from numerical relativity simulations to gamma-ray data. Perimeter Institute. https://pirsa.org/23020029
MLA
Chirenti, Cecilia. Hypermassive neutron stars: from numerical relativity simulations to gamma-ray data. Perimeter Institute, Mar. 09, 2023, https://pirsa.org/23020029
BibTex
@misc{ pirsa_PIRSA:23020029, doi = {10.48660/23020029}, url = {https://pirsa.org/23020029}, author = {Chirenti, Cecilia}, keywords = {Strong Gravity}, language = {en}, title = {Hypermassive neutron stars: from numerical relativity simulations to gamma-ray data}, publisher = {Perimeter Institute}, year = {2023}, month = {mar}, note = {PIRSA:23020029 see, \url{https://pirsa.org}} }
Gamma ray bursts (GRBs) are the most luminous electromagnetic events in the universe. Short GRBs, typically lasting less than 2 seconds, have already been associated with binary neutron star (BNS) mergers, which are also sources of gravitational waves (GWs). The ultimate fate of a BNS, after coalescence, is usually expected to be a black hole (BH) with 2-3 solar masses. However, numerical relativity simulations indicate the possible formation of a short-lived hypermassive neutron star (HMNS), lasting for tens to hundreds of milliseconds after the BNS merger and before gravitational collapse forms a BH. The HMNS is expected to emit GWs with kHz frequencies that will be detectable by third generation ground-based GW detectors in the 2030s. I will present results from a recent analysis that revealed evidence for HMNSs by looking for kHz quasiperiodic oscillations in gamma-ray observations obtained in the 1990s with the Compton Gamma Ray Observatory.
Zoom link: https://pitp.zoom.us/j/96687956901?pwd=MkgrUGlqY3IyRCs2bXJYVkhUVEpPZz09