2025-10-28 カリフォルニア工科大学 (Caltech)
Artwork of a binary black hole merger. In cases like GW241011 and GW241110, where at least one black hole rotates in a peculiar direction relative to the orbital plane, the unusual spins offer hints about how the system formed.Credit: Carl Knox, OzGrav, Swinburne University of Technology
＜関連情報＞
- https://www.caltech.edu/about/news/colliding-black-holes-might-have-formed-from-earlier-cosmic-smashups
- https://iopscience.iop.org/article/10.3847/2041-8213/ae0d54
GW241011とGW241110：非対称高スピンブラックホール合体による連星形成と基礎物理学の探究 GW241011 and GW241110: Exploring Binary Formation and Fundamental Physics with Asymmetric, High-spin Black Hole Coalescences
A. G. Abac, I. Abouelfettouh, F. Acernese, K. Ackley, C. Adamcewicz, S. Adhicary, D. Adhikari, N. Adhikari, R. X. Adhikari, V. K. Adkins,…
The Astrophysical Journal Letters Published: 2025 October 28
DOI:10.3847/2041-8213/ae0d54
Abstract
We report the observation of gravitational waves from two binary black hole coalescences during the fourth observing run of the LIGO–Virgo–KAGRA detector network, GW241011 and GW241110. The sources of these two signals are characterized by rapid and precisely measured primary spins, nonnegligible spin–orbit misalignment, and unequal mass ratios between their constituent black holes. These properties are characteristic of binaries in which the more massive object was itself formed from a previous binary black hole merger and suggest that the sources of GW241011 and GW241110 may have formed in dense stellar environments in which repeated mergers can take place. As the third-loudest gravitational-wave event published to date, with a median network signal-to-noise ratio of 36.0, GW241011 furthermore yields stringent constraints on the Kerr nature of black holes, the multipolar structure of gravitational-wave generation, and the existence of ultralight bosons within the mass range 10−13–10−12 eV.
