Neutron star as a mirror for gravitational waves
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ORIGINAL ARTICLE
Neutron star as a mirror for gravitational waves Hao Wei1
· Da-Chun Qiang1 · Zhong-Xi Yu1 · Hua-Kai Deng1
Received: 23 June 2020 / Accepted: 3 September 2020 © Springer Nature B.V. 2020
Abstract Gravitational wave (GW) has become one of the most active fields in physics and astronomy since the first direct detection of GW event in 2015. As is well known, multiple images of GW events are possible through the gravitational lenses. Here, we propose a novel mirror imaging mechanism for GW events different from the gravitational lens. In the literature, the superconductor was predicted to be highly reflective mirror for GWs. It is well known that neutron stars exhibit superconductivity and superfluidity. In this work, we predict that there are two types of GW mirror imaging phenomena caused by the neutron star located in Milky Way or the same host galaxy of GW source, which might be detected within a life period of man (namely the time delay t can be a few years to a few tens of years). It is expected to witness this predicted GW mirror imaging phenomenon in the near future. In the long term, the observations of this novel GW mirror imaging phenomenon might help us to find numerous neutron stars unseen by other means, and learn more about the complicated internal structures of neutron stars, as well as their equations of state. Keywords Neutron star · Gravitational wave · Mirror imaging phenomenon · Gravitational lens · Superconductor
Gravitational wave (GW) is a long-standing prediction of general relativity (GR) since 1916 (Einstein 1916; Einstein 1918; Einstein and Rosen 1937; Cervantes-Cota et al. 2016). The debate about the physical reality of GW was mainly settled during the Chapel Hill conference in 1957 (Cervantes-
B H. Wei
[email protected]
1
School of Physics, Beijing Institute of Technology, Beijing 100081, China
Cota et al. 2016; Saulson 2011). In 1974, Hulse and Taylor discovered the first indirect evidence for the existence of GW from the binary pulsar PSR B1913+16 (Taylor et al. 1979; Taylor and Weisberg 1982; Lorimer 2008), and hence they earned the 1993 Nobel Prize. In 2015, the LIGO/Virgo Collaboration made the first direct observation of GW event (GW150914) from a binary black hole merger (Abbott et al. 2016a; Abbott et al. 2016b), and then earned the 2017 Nobel Prize. From the first multi-messenger observations of a binary neutron star merger (GW170817) (Abbott et al. 2017a; Abbott et al. 2017b), the speed of GW was confirmed to be the speed of light c (Abbott et al. 2017c). Nowadays, GW becomes one of the most active fields in physics and astronomy. As is well known, most objects (e.g. earth) are nearly transparent to GWs. On the other hand, the gravitational lenses (e.g. massive galaxies) can deflect GW as well as light (Schneider et al. 1992; Schneider et al. 2006). Therefore, multiple images of GW events are possible through the gravitational lenses. Here, we propose a novel mirror imaging mechanism for GW events different from the gravitational lens. We note that in M
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