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Home  >  Transactions of NAMP VOL 14

7. ESTIMATION OF FREQUENCY, LUMINOSITY, AND THE EXPECTED TIME OF MERGER OF GRAVITATIONAL WAVE GENERATED BY BINARY BLACK HOLES. by Bringen B., Girma D. P. and Bakwa D. D Volume 14, (January - March, 2021 Issue)
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ESTIMATION OF FREQUENCY, LUMINOSITY, AND THE EXPECTED TIME OF MERGER OF GRAVITATIONAL WAVE GENERATED BY BINARY BLACK HOLES.

1Bringen B., 2Girma D. P. and 3Bakwa D. D.

1 Department of Physics, Faculty of Science, Borno State University,

2GSS Bet-Pankshin, Plateau State

3Department of Physics, Faculty of Natural Sciences, University of Jos 

Abstract

GWs are predicted by any theory which assumes that gravitational effect propagate at finite speed. Characteristics such as the GW polarization, phase, and amplitude change depending on the theory assumed. It is for this reason that GWs can be used to test general relativity and explore the physics of objects such as black holes. The estimated values of frequency, luminosity, and time of merger of binary black holes (selected binary systems: PSR 1913+16, XTE J1118+480, 1915+105, Nova Scopii, V4641 Sgr, and VFTS 352 and their companions) obtained from different galaxies with qualitative behavior of compact binary coalescences within the post-Newtonian framework, using the parameters considered includes the distance r (observer distance), R (orbital separation), masses M (M_⨀);the results obtained from the estimation of binary black hole parameters are presented in tables 1, 2, and 3. The results indicate a high sensitivity that could be suitable within the detector’s frequency band, such as LISA. The values indicate that these BBH are suitable candidates for GW detectors. The estimated values of frequencies of 10-5 – 10-7Hz shows an excellent sensitivity for LISA. The LIGO’s system reached a peak gravitational-wave luminosity of 3.6 x 1056erg/s equivalent to 200M_⨀C2. Meanwhile the estimated values obtained as shown in figure 2 is between 145.8 x 1050 - 0.717 x1050 erg/s which gives a significant gravitational- wave luminosity of the sources BBH. Meanwhile, the estimated time of merger for the source stars indicated in table 3 reveals to be between1012 - 1020s. The LIGO observatories has a range of detectable signals of GW amplitude as h ~ 1.0 x10-21 and h ~ 3.3 x10-22 when GW150914 and GW151226 were detected. These observations were made at signal frequencies of f ~ 35 – 350 Hz and 35 – 450 Hz by the aLIGO. 

Key Words: Frequency, luminosity, merger, Gravitational wave, Binary black holes

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