Could Solar Radiation Pressure Explain 'Oumuamua's Peculiar Acceleration?

Abstract

'Oumuamua (1I/2017 U1) is the first object of interstellar origin observed in the Solar system. Recently, Micheli et al. (2018) reported that 'Oumuamua showed deviations from a Keplerian orbit at a high statistical significance. The observed trajectory is best explained by an excess radial acceleration \(\Delta a \propto r^{-2}\), where \(r\) is the distance of 'Oumuamua from the Sun. Such an acceleration is naturally expected for comets, driven by the evaporating material. However, recent observational and theoretical studies imply that 'Oumuamua is not an active comet. We explore the possibility that the excess acceleration results from Solar radiation pressure. The required mass-to-area ratio is \(m/A\approx 0.1\) g cm\(^{-2}\). For a thin sheet, this requires a width of \(w \approx 0.3-0.9\) mm. We find that although extremely thin, such an object would survive an interstellar travel over Galactic distances of \(\sim 5\) kpc , withstanding collisions with gas and dust-grains as well as stresses from rotation and tidal forces. We discuss the possible origins of such an object.