At lower frequencies, the space-based laser interferometer LISA is firmly planned to cover the 0.1–10 mHz band, targeting, for example, black-hole and white-dwarf binaries. Since in principle, GWs can be emitted at any frequency, they are expected over many decades of frequency below the audio band, but also above it. Coalescences of compact objects such as black holes and neutron stars have been detected, and spinning neutron stars, supernovae and stochastic signals are likely future sources. Based on these two quantities and the abundance of sources across the full gravitational-wave spectrum, as well as the availability of technology, it becomes clear that different parts of the gravitational-wave spectrum are more accessible than others.Ĭurrent ground-based detectors are sensitive in the frequency band from about 10 Hz to 10 kHz where the intersection of efforts in the development of the technology and the abundance of sources facilitated the first detections. ![]() ![]() GWs are spacetime perturbations predicted by the theory of general relativity that propagate with the speed of light and can be predominantly characterised by their frequency f and the dimensionless (characteristic) amplitude \(h_c\). With the first detections of gravitational waves (GWs) by the ground-based laser interferometers LIGO and VIRGO, a new tool for astronomy, astrophysics and cosmology has been firmly established.
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |