Research PapersNo Access

Dark matter gravity waves at LIGO and LISA

Paul H. Frampton

Department of Mathematics and Physics “Ennio de Giorgi”, University of Salento, Lecce, Italy

E-mail Address: paul.h.frampton@gmail.com

https://doi.org/10.1142/S0217732319501244Cited by:0 (Source: Crossref)

Abstract

We study the merger rate of dark matter PIMBHs (Primordial Intermediate Mass Black Holes). We conclude that the black holes observed by LIGO in GW150914 and later events were probably not dark matter PIMBHs but rather the result of gravitational collapse of very massive stars. To study the PIMBHs by gravitational radiation will require a detector sensitive to frequencies below 10 Hz and otherwise more sensitive than LIGO. The LISA detector, expected to come online in 2034, will be useful at frequencies below 1 Hz but further gravitational wave detectors beyond LISA, sensitive up to 10 Hz, and higher strain sensitivity will be necessary to fully study dark matter.

Keywords:

References

1. LIGO and Virgo Collabs. (B. P. Abbott et al.), Phys. Rev. Lett. 116, 061102 (2016). Crossref, Web of Science, Google Scholar
2. R. A. Hulse and J. H. Taylor, Astrophys. J. 195, L51 (1975). Crossref, Web of Science, ADS, Google Scholar
3. J. H. Taylor and J. M. Weisberg, Astrophys. J. 253, 908 (1982). Crossref, Web of Science, ADS, Google Scholar
4. J. H. Taylor and J. M. Weisberg, Astrophys. J. 576, 942 (2002). Crossref, Web of Science, ADS, Google Scholar
5. J. M. Weisberg and Y. Huang, Astrophys. J. 829, 55 (2016). Crossref, Web of Science, ADS, Google Scholar
6. A. Einstein, Sitzungber. K. Preuss. Akad. Wiss. 154 (1918). Google Scholar
7. P. H. Frampton, Int. J. Mod. Phys. A 33, 1830030 (2018). Link, Web of Science, ADS, Google Scholar
8. P. H. Frampton, Mod. Phys. Lett. A 31, 1650093 (2016). Link, Web of Science, ADS, Google Scholar
9. G. F. Chapline, Nature 253, 251 (1975). Crossref, Web of Science, ADS, Google Scholar
10. G. F. Chapline and P. H. Frampton, J. Cosmol. Astropart. Phys. 11, 042 (2016). Crossref, Web of Science, ADS, Google Scholar
11. A. Einstein, Science 84, 506 (1936). Crossref, ADS, Google Scholar
12. B. Paczynski, Astrophys. J. 304, 1 (1986). Crossref, Web of Science, ADS, Google Scholar
13. The MACHO Collab. (C. Alcock et al.), Astrophys. J. 542, 281 (2000). Crossref, Web of Science, Google Scholar
14. P. C. Peters, Phys. Rev. 136, B1224 (1964). Crossref, Web of Science, ADS, Google Scholar
15. G. D. Quinlan and S. L. Shapiro, Astrophys. J. 343, 725 (1989). Crossref, Web of Science, ADS, Google Scholar
16. H. Mouri and Y. Taniguchi, Astrophys. J. 566, L17 (2002). Crossref, Web of Science, ADS, Google Scholar
17. A. G. Riess et al., Phys. Rev. Lett. 116, 201301 (2016). Crossref, Web of Science, ADS, Google Scholar
18. https://dcc.ligo.org/public/0002/T0900288/003/AdvLIGO. Google Scholar
19. T. Robson, N. Cornish and C. Liu, arXiv:1803.01944 [astro-ph.HE]. Google Scholar
20. F. Kühnel, A. Matas, G. D. Starkman and K. Freese, arXiv:1811.06387 [gr-qc]. Google Scholar
21. M. Sasaki, T. Suyama. T. Tanaka and S. Yokoyama, Class. Quantum Grav. 35, 063001 (2018). Crossref, Web of Science, Google Scholar