Did a stellar fly-by shape the planetary system around Pr 0211 in the cluster M44?

Abstract

Aims. Out of the ∼ 3000 exoplanets detected so far, only fourteen planets are members of open clusters: among them an exoplanet system around Pr 0211 in the cluster M44 which consists of at least two planets with the outer planet moving on a highly eccentric orbit at 5.5 AU. One hypothesis is that a close fly-by of a neighbouring star was responsible for the eccentric orbit. We test this hypothesis. Methods. First we determine the type of fly-by that would lead to the observed parameters and then use this result to determine the history of such fly-bys in simulations of the early dynamics in an M44-like environment. Results. We find that although very close fly-bys are required to obtain the observed properties of Pr 0211c, such fly-bys are relatively common due to the high stellar density and longevity of the cluster. About 10% of stars actually experience a fly-by that would lead to such a small system-size as observed for Pr0211 or even smaller. Such close fly-bys are most frequent during the first 1-2 Myr after cluster formation, corresponding to a cluster age ≤ 3 Myr. It is unclear whether planets generally form on such short timescales. However, afterwards the close fly-by rate is still 0.2-0.5 Myr −1 , which means extrapolating this to the age of M44 12%-20% of stars would experience such close fly-bys over this timespan. Conclusions. Our simulations show that the fly-by scenario is a realistic option for the formation of eccentricity orbits of the planets in M44. The occurance of such events is relatively high leading to the expectation that similar systems are likely common in open clusters in general.

Stellar clustering shapes the architecture of planetary systems

“…Exoplanets that remain at wider separations may also have been dynamically perturbed, as has been suggested to explain the highly eccentric orbit of Pr 0211c in Praesepe (with orbital eccentricity e ≈ 0.7, semi-major axis a p ≈ 5.5 AU, and mass M p sin i ≈ 7.8 M J , where M J is the mass of Jupiter; refs. 111 , 112 ), as well as the peculiar orbits of trans-Neptunian objects orbiting the Sun 113 .…”

Fly-by encounters between two planetary systems II: Exploring the interactions of diverse planetary system architectures

“…And it has been estimated that the occurrence rate in open cluster M 67 is similar to that in the field (Brucalassi et al 2017). This seems to suggest that planetary formation process is not disrupted much within a few tens of au in open clusters (for example, Adams et al 2006;Pfalzner et al 2018;Winter et al 2018).…”

Stellar clustering shapes the architectures of planetary systems

“…Exoplanets that remain at wider separations may also have been dynamically perturbed, as has been suggested to explain the highly eccentric orbit of Pr 0211c in Praesepe (with orbital eccentricity e ≈ 0.7, semi-major axis a p ≈ 5.5 au, and mass M p sin i ≈ 7.8 M J ; refs. 111,112 ), as well as the peculiar orbits of trans-Neptunian objects orbiting the Sun 113 .…”