Two Hyperbolic Baldheads in the Solar System: 2017 U7 and 2018 C2

Abstract

We present a study of two newly discovered heliocentric hyperbolic objects -- 2017 U7 and 2018 C2. Both are possibly thermally evolved comets. Observations of the latter in 2018 March from Xingming Observatory revealed that it has a color similar to those of the long-period comets, Trojans, and D-type asteroids: $m_B - m_V = 0.75 \pm 0.03$, $m_V - m_R = 0.41 \pm 0.02$, and $m_R - m_I = 0.37 \pm 0.03$. A possible extremely faint coma of $\sim$9$"$ across was observed. The radial profile of 2018 C2 in comparison with those of the field stars helps confirm its cometary nature. Based on our convolution model, its mass-loss rate is estimated to be $0.7 \pm 0.2$ kg s$^{-1}$. Assuming geometric albedo $p_R = 0.04$, its effective radius is $4.4 \pm 0.5$ km, which means that the fraction of active area is merely $\sim$10$^{-5}$-10$^{-4}$. Our N-body dynamical simulations show that both objects are most likely dynamically old members from the Oort cloud. 2017 U7 has a $\sim$60% chance to escape the solar system in the 1.5 Myr following its current perihelion passage due to a moderate close encounter with Jupiter in 2020 May. On the condition that no disintegration occurs, 2018 C2 will revisit the inner solar system 0.13-0.14 Myr later, with perihelion distance $\sim$2 AU.