Ultra-low-frequency gravitational waves from cosmological and astrophysical processes

被引：47

作者：

Moore, Christopher J. ^{[1
]}

Vecchio, Alberto

机构：

[1] Univ Birmingham, Inst Gravitat Wave Astron, Birmingham, W Midlands, England

来源：

NATURE ASTRONOMY | 2021年 / 5卷 / 12期

关键词：

BLACK-HOLE BINARIES; RADIATION; PROPAGATION; SYSTEMS; LIMITS;

D O I：

10.1038/s41550-021-01489-8

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Gravitational waves at ultra-low frequencies (less than or similar to 100 nHz) are key to understanding the assembly and evolution of astrophysical black hole binaries with masses similar to 10(6)-10(9) M-circle dot at low redshifts(1-3). These gravitational waves also offer a unique window into a wide variety of cosmological processes(4-11). Pulsar timing arrays(12-14) are beginning to measure(15) this stochastic signal at similar to 1-100 nHz and the combination of data from several arrays(16-19) is expected to confirm a detection in the next few years(20). The dominant physical processes generating gravitational radiation at nHz frequencies are still uncertain. Pulsar timing array observations alone are currently unable(21) to distinguish a binary black hole astrophysical foreground(22) from a cosmological background due to, say, a first-order phase transition at a temperature similar to 1-100 MeV in a weakly interacting dark sector(8-11). This letter explores the extent to which incorporating integrated bounds on the ultra-low-frequency gravitational wave spectrum from any combination of cosmic microwave background(23,24), big bang nucleosynethesis(25,26) or astrometric(27,28) observations can help to break this degeneracy.

引用

页码：1268 / 1274

页数：7

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