2009/02/28 by M. S. Pshirkov · 7 citations
Engineering · Physics and Astronomy · #Binary pulsar #Cosmology and Gravitation Theories #Geophysics and Sensor Technology #Gravitational wave #Gravitational wave background #Limit (mathematics) #Millisecond pulsar #Pulsar #Pulsars and Gravitational Waves Research #Range (aeronautics) #Rotational energy #Rotational symmetry #astro-ph.CO #astro-ph.IM
paper · pdf · doi:10.1111/j.1365-2966.2009.15221.x
published in Monthly Notices of the Royal Astronomical Society 398(4), 1932-1935 (Oxford University Press) · 5 pages, submitted to MNRAS; changes of content in Section 3, reference added for section 1; changes in content in Section 3, refernce added, generally matches MNRAS version
openalex publication_date 2009/08/31 · arxiv created 2009/10/08 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
A method is suggested with which to explore the gravitational wave background (GWB) in the frequency range 10−12–10−8 Hz. This method is based on the precise measurements of pulsar rotational parameters: the influence of gravitational waves (GWs) in this frequency range will affect these parameters and therefore some conclusions about the energy density of the GWB can be made using analysis of the derivatives of pulsar rotational frequency. The calculated values of the second derivative from a number of pulsars limit the density of the GWB, Ωgw, as follows: Ωgw < 2 × 10−6. Also, the time series of the frequency ν of different pulsars in a pulsar array can be cross-correlated pairwise in the same manner as in anomalous residuals analysis, thus providing the possibility of GWB detection in the ultra-low-frequency range.