Detecting dark matter oscillations with gravitational waveforms
We consider the phase shift in the gravitational wave signal induced by fast oscillations of scalar dark matter surrounding binary systems, which could be probed by the future experiments LISA and DECIGO. This effect depends on the local matter density and the mass of the dark matter particle. We co...
| Autores: | , , , |
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| Tipo de recurso: | artículo |
| Fecha de publicación: | 2024 |
| País: | España |
| Institución: | Universidad Complutense de Madrid (UCM) |
| Repositorio: | Docta Complutense |
| Idioma: | inglés |
| OAI Identifier: | oai:docta.ucm.es:20.500.14352/110433 |
| Acceso en línea: | https://hdl.handle.net/20.500.14352/110433 |
| Access Level: | acceso abierto |
| Palabra clave: | 52-33 530.12 Binary population Astrofísica 2212 Física Teórica 2212.14 Teoría de la Relatividad 2101 Cosmología y Cosmogonía |
| Sumario: | We consider the phase shift in the gravitational wave signal induced by fast oscillations of scalar dark matter surrounding binary systems, which could be probed by the future experiments LISA and DECIGO. This effect depends on the local matter density and the mass of the dark matter particle. We compare it to the phase shift due to a standard dynamical friction term, which should generically be present. We find that the effect associated with the oscillations only dominates over the dynamical friction for dark matter masses below 10-21 eV, with masses below 10-23 eV implying cloud sizes that are too large to be realistic. Moreover, for masses of the order of 10-21 eV, LISA and DECIGO would only detect this effect for dark matter densities greater than that in the solar system by a factor 105 or 104 respectively. We conclude that this signal can be ignored for most dark matter scenarios unless very dense clouds of very light dark matter are created early in the Universe at a redshift z similar to 104. |
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