A Sublime Opportunity: The Dynamics of Transitioning Cometary Bodies and the Feasibility of In Situ Observations of the Evolution of Their Activity

Abstract

The compositional and morphological evolution of minor bodies in the solar system is primarily driven by the evolution of their heliocentric distances, as the level of incident solar radiation regulates cometary activity. We investigate the dynamical transfer of Centaurs into the inner solar system, facilitated by mean motion resonances with Jupiter and Saturn. The recently discovered object P/2019 LD2 will transition from the Centaur region to the inner solar system in 2063. In order to contextualize LD2, we perform N-body simulations of a population of Centaurs and Jupiter-family comets. Objects between Jupiter and Saturn with Tisserand parameter T J ∼ 3 are transferred onto orbits with perihelia q < 4 au within the next 1000 yr with notably high efficiency. Our simulations show that there may be additional LD2-like objects transitioning into the inner solar system in the near future, all of which have low ΔV with respect to Jupiter. We calculate the distribution of orbital elements resulting from a single Jovian encounter and show that objects with initial perihelia close to Jupiter are efficiently scattered to q < 4 au. Moreover, approximately 55% of the transitioning objects in our simulated population experience at least one Jovian encounter prior to reaching q < 4 au. We demonstrate that a spacecraft stationed near Jupiter would be well positioned to rendezvous, orbit-match, and accompany LD2 into the inner solar system, providing an opportunity to observe the onset of intense activity in a pristine comet in situ. Finally, we discuss the prospect of identifying additional targets for similar measurements with forthcoming observational facilities.

The Volatile Carbon-to-oxygen Ratio as a Tracer for the Formation Locations of Interstellar Comets

“…The current larger census of comets can be sorted into two populations: ecliptic comets, a subset of which are Jupiter family comets (JFCs), and long-period comets (LPCs), which have isotropic distributions of inclination. It is generally believed that the JFCs originate in the trans-Neptunian region (Leonard 1930;Edgeworth 1943Edgeworth , 1949Kuiper 1951;Cameron 1962;Whipple 1964;Everhart 1972;Vaghi 1973;Delsemme 1973;Joss 1973;Fernandez 1980;Duncan et al 1988;Quinn et al 1990;Jewitt & Luu 1993;Prialnik et al 2020) and migrate into the inner solar system via the Centaur region (Hahn & Bailey 1990;Levison & Duncan 1997;Tiscareno & Malhotra 2003;Di Sisto & Brunini 2007;Bailey & Malhotra 2009;Di Sisto et al 2009;Nesvorný et al 2017;Fernández et al 2018;Sarid et al 2019;Seligman et al 2021a), while the LPCs come from the Oort cloud (Oort 1950).…”

Inferring Late Stage Enrichment of Exoplanet Atmospheres from Observed Interstellar Comets

“…The short period comets (SPCs), or ecliptic comets with low inclina-tions, originate in the Kuiper belt and are subsequently perturbed onto orbits interior to the orbit of Neptune (Leonard 1930;Edgeworth 1943;Kuiper 1951;Fernandez 1980;Duncan et al 1988;Quinn et al 1990). They temporarily reside in the Centaur region on giant planet crossing orbits, until reaching the inner Solar System and becoming Jupiter Family Comets (JFCs) (Hahn & Bailey 1990; Levison & Duncan 1997;Tiscareno & Malhotra 2003;Di Sisto & Brunini 2007;Bailey & Malhotra 2009;Di Sisto et al 2009;Nesvorný et al 2017;Fernández et al 2018;Seligman et al 2021a). Because the escape velocity of Jupiter is larger than its orbital velocity, close encounters with the giant planet typically scatter comets back into the Centaur region or into the inner Solar System, instead of resulting in a collision.…”

“…A common definition of a JFC is an object with Tisserand parameter with respect to Jupiter, 2 < T J < 3(Levison 1996). See Table1inSeligman et al (2021a) for an exhaustive list of literature definitions.…”

Inferring Late-stage Enrichment of Exoplanet Atmospheres from Observed Interstellar Comets

“…Short-period comets (SPCs), or ecliptic comets with low inclinations, originate in the Kuiper Belt and are subsequently perturbed onto orbits interior to the orbit of Neptune (Leonard 1930;Edgeworth 1943;Kuiper 1951;Fernandez 1980;Duncan et al 1988;Quinn et al 1990). They temporarily reside in the Centaur region on giant-planet-crossing orbits until they reach the inner solar system and become Jupiter Family Comets (JFCs) (Hahn & Bailey 1990; Levison & Duncan 1997;Tiscareno & Malhotra 2003;Di Sisto & Brunini 2007;Bailey & Malhotra 2009;Di Sisto et al 2009;Nesvorný et al 2017;Fernández et al 2018;Seligman et al 2021a). Because the escape velocity of Jupiter is larger than its orbital velocity, close encounters with the giant planet typically scatter comets back into the Centaur region or into the inner solar system, instead of resulting in a collision.…”

“…A common definition of a JFC is an object with a Tisserand parameter with respect to Jupiter 2 < T J < 3(Levison 1996). See Table1inSeligman et al (2021a) for an exhaustive list of literature definitions.…”