Abstract
Gravitational waves have been detected in the past few years from several transient events such as merging stellar mass black holes, binary neutron stars, etc. These waves have frequencies in a band ranging from a few hundred hertz to around a kilohertz to which LIGO type instruments are sensitive. LISA would be sensitive to much lower range of frequencies from SMBH mergers. Apart from these cataclysmic burst events, there are innumerable sources of radiation which are continuously emitting gravitational waves of all frequencies. These include a whole mass range of compact binary and isolated compact objects as well as close planetary stellar entities. In this work, quantitative estimates are made of the gravitational wave background produced in typical frequency ranges from such sources emitting over a Hubble time and the fluctuations in the h values measured in the usual devices. Also estimates are made of the high frequency thermal background gravitational radiation from hot stellar interiors and newly formed compact objects.
Highlights
Gravitational waves (GW) as predicted by Einstein over a century ago, were first detected by LIGO in 2016 [1]
Gravitational wave detectors like LIGO are hunting for waves from compact binary inspirals, which are produced by orbiting pairs of massive, compact objects like neutron stars (NS) and black holes (BH)
Primordial black holes (PBHs) are hypothetical type of black holes that are formed not by the gravitational collapse of a star but by the extreme densities of matter present during early Universe [11]. As these PBHs evaporate through Hawking radiation, part of the energy could be released in the form of thermal gravitational waves [5]
Summary
Gravitational waves (GW) as predicted by Einstein over a century ago, were first detected by LIGO in 2016 [1]. Apart from black hole mergers, in 2017, LIGO detected gravitational waves from the collision of two neutron stars. Unlike the black hole mergers which are only detectable gravitationally, this event (GW170817) was detected electromagnetically [2] These are long wavelength, low frequency gravitational waves. Compact stellar objects can generate high frequency thermal gravitational radiation, which in the case of hot neutron stars can be high. A study is made of the thermal gravitational wave emission from all of the above sources, and the background flux is estimated. The integrated thermal gravitational flux as the Universe expands is estimated and compared with that from all the discrete sources discussed above. Possible schemes to detect such sources of high frequency thermal gravitational radiation are discussed and the physical principles involved are elaborated
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