(ed.). Gravitational waves (IOP, 2001)(422s).

viiiContents11.3 Gravitational wave radiation in the JBD theory 15911.3.1 Scalar and Tensor GWs in the JBD Theory 16011.3.2 Power emitted in GWs 16111.3.3 Power emitted in scalar GWs 16211.3.4 Scalar GWs 16411.3.5 Detectability of the scalar GWs 16511.4 The hollow sphere 16811.5 Scalar–tensor cross sections 170Acknowledgments 176References 176PART 3The Stochastic Gravitational-Wave BackgroundD Babusci, S Foffa, G Losurdo, M Maggiore, G Matone and R Sturani 17912 Generalities on the stochastic GW background 18112.1 Introduction 18112.2 Definitions 18412.2.1 gw ( f ) and the optimal SNR 18412.2.2 The characteristic amplitude 18712.2.3 The characteristic noise level 18912.3 The overlap reduction function 19112.3.1 Two interferometers 19312.3.2 Interferometer—bar 19612.3.3 Interferometer—sphere 19612.4 Achievable sensitivities to the SGWB 19712.4.1 Single detectors 19712.4.2 Two detectors 19912.4.3 More than two detectors 20412.5 Observational bounds 20713 Sources of SGWB 21113.1 Topological defects 21113.1.1 Strings 21413.1.2 Hybrid defects 22113.2 Inflation 22313.2.1 Classical picture 22413.2.2 Calculation of the spectrum 22513.3 String cosmology 22913.3.1 The model 23013.3.2 Observational bounds to the spectrum 23413.4 First-order phase transitions 23513.5 Astrophysical sources 237References 239