Identifying Thorne–Żytkow Objects through Neutrinos

Abstract

Thorne–Żytkow objects (T $\dot{{\rm{Z}}}$ Os) have been predicted to form when a neutron star is engulfed by a diffuse, convective giant envelope. Accretion onto a neutron star at a rate that is larger than 10 ^−4 M _⊙ yr ^−1 is expected to lead to significant emission of neutrinos of all flavors with energy of 1–100 MeV. Since the neutrino signal is expected to largely vary in time (from milliseconds to thousands of years), we outline detection strategies tailored to the signal duration. We find that neutrino detection from T $\dot{{\rm{Z}}}$ Os up to the Small Magellanic Cloud is within the reach of current- and next-generation neutrino observatories, such as Super- and Hyper-Kamiokande, the IceCube Neutrino Observatory, and JUNO. Interestingly, if targeted searches for neutrinos from T $\dot{{\rm{Z}}}$ O candidates (e.g., VX Sgr in our Galaxy as well as HV 2112 and HV 11417 in the Small Magellanic Cloud) should lead to positive results, neutrinos could positively identify the nature of such sources and their accretion rate. Furthermore, the diffuse supernova neutrino background may be able to rule out extreme scenarios for the formation and accretion rates of TŻOs. Our findings should serve as motivation for establishing dedicated searches for neutrino emission from T $\dot{{\rm{Z}}}$ Os. This is especially timely since it is challenging to detect TŻOs via electromagnetic radiation unambiguously, and the T $\dot{{\rm{Z}}}$ O gravitational-wave signal could be probed with next-generation detectors for sources within our Galaxy only.

Keywords

• Neutrino astronomy
• Neutrino oscillations
• Neutrino telescopes
• Common envelope binary stars
• Stellar accretion
• Neutron stars