# The stability around Chariklo and the confinement of its rings

S. Giuliatti Winter, G. Madeira, T. Ribeiro, O. Winter, G. Barbosa, G.

Borderes-Motta

► To cite this version:

S. Giuliatti Winter, G. Madeira, T. Ribeiro, O. Winter, G. Barbosa, et al. The stability around Chariklo and the confinement of its rings. Astronomy & Astrophysics - A&A, 2023, 679, pp.A62. 10.1051/0004-6361/202345864. hal-04273165

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Submitted on 8 Nov 2023

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# The stability around Chariklo and the confinement of its rings

S. M. Giuliatti Winter<fnref n="1" />, G. Madeira<fnref n="2" />,<fnref n="1" />, T. Ribeiro<fnref n="1" />, O. C. Winter<fnref n="1" />, G. O. Barbosa<fnref n="1" />,<fnref n="3" />, and G. Borderes-Motta<fnref n="4" />

Received 8 January 2023 / Accepted 5 July 2023

## ABSTRACT

**Context.** Chariklo has two narrow and dense rings, C1R and C2R, located at 391 km and 405 km, respectively.

**Aims.** In the light of new stellar occultation data, we study the stability around Chariklo. We also analyse three confinement mechanisms that prevent the spreading of the rings, based on shepherd satellites in resonance with the edges of the rings.

**Methods.** This study was performed through a set of numerical simulations and the Poincaré surface of section technique.

**Results.** From the numerical simulation results, and from the current parameters referring to the shape of Chariklo, we verify that the inner edge of the stable region is much closer to Chariklo than the rings. The Poincaré surface of sections allows us to identify periodic and quasi-periodic orbits of the first kind, and also the resonant islands corresponding to the 1:2, 2:5, and 1:3 resonances. We construct a map of $a_{eq}$ versus $e_{eq}$ space that gives the location and width of the stable region and the 1:2, 2:5, and 1:3 resonances.

**Conclusions.** We find that the first kind periodic orbit family can be responsible for a stable region whose location and size meet that of C1R, for specific values of the ring particle eccentricities. However, C2R is located in an unstable region if the width of the ring is assumed to be about 120 m. After analysing different systems, we propose that the best confinement mechanism is composed of three satellites: two satellites shepherding the inner edge of C1R and the outer edge of C2R, and the third satellite trapped in the 1:3 resonance.

**Key words.** minor planets, asteroids: general – celestial mechanics – planets and satellites: rings

## 1. Introduction

The amazing rings of Saturn were discovered in the seventeenth century by Galileo Galilei, although he died before knowing he had discovered a unique planetary ring system. Only three centuries later, the rings around the giant planets Jupiter, Uranus, and Neptune were revealed by the spacecraft Voyager I and II and by stellar occultations.

A new class of objects sheltering a ring system was discovered in 2014 by Braga Ribas and colleagues (Braga-Ribas et al. 2014) [BR14 hereafter] through stellar occultation. They discovered a ring system around the largest Centaur (10199) Chariklo. This Centaur object could have originated in the trans-Neptunian region and could have been deflected to the Centaur region, probably due to a close encounter with Neptune within the last 20 Myr (Wood et al. 2017).

The two dense rings, 2013C1R and 2013C2R, in orbit around Charilko are very narrow rings with widths of about 7 km and 3 km and optical depths of 0.4 and 0.06, respectively (BR14). They are located very close to Chariklo; their orbital radii are 391 km and 405 km. BR14 speculated three scenarios for the origin of the two rings, one of them relies on a collision of a satellite onto the surface of Chariklo. This collision could have released material from Chariklo and formed the rings, or the impactor satellite could have been destroyed and originated the rings. Regarding the composition of the rings, Duffard et al. (2014) obtained that silicates, tholins, and water ice may be present in C1R and C2R, while Sicardy (2020) claimed that the presence

of icy water, shown in the spectrum of the rings, may be caused by Chariklo.

A set of five stellar occultations presented in Leiva et al. (2017) between 2013 and 2016 helped to constrain the size and shape of Chariklo. The shape of an object can help to analyse the dynamical behaviour of nearby particles, and in this particular case could help us to explain the origin and evolution of the rings. They considered four possible models for Chariklo: a sphere with radius equal to 129 km; a MacLaurin spheroid with about $a = b = 143$ km and $c = 96$ km; a triaxial ellipsoid with $a = 157$ km, $b = 132$ km, and $c = 102$ km; and a Jacobi ellipsoid with $a = 157$ km, $b = 139$ km and $c = 86$ km, where *a*, *b*, and *c* are the semi-axes. With the derived mass range for Chariklo of $6–8 \times 10^{18}$ kg, they pointed out that the 1:3 resonance between the rotation of Chariklo and the orbital motion of the particles is at $408 \pm 20$ km, close to the location of the rings.

A paper by Morgado et al. (2021; hereafter M21) presents new stellar occultation data obtained between 2017 and 2020. These new data helped to constrain the Chariklo and the ring parameters. The parameters of C1R and C2R are listed in Table 1. They also concluded that these rings may contain particles larger than 1 µm in size. An important result concerns the shape of Chariklo; from these stellar occultation data Chariklo is consistent with a triaxial ellipsoid with semi-axes $a = 143.8$ km, $b = 135.2$ km, and $c = 99.1$ km (M21).

The relation between the inner ring of Chariklo and the 1:3 spin-orbit resonance (the resonance between Chariklo's rotation period and the mean motion of the particles) was explored in

<footnote n="1">¹ Grupo de Dinâmica Orbital & Planetologia, São Paulo State University – UNESP, Av. Ariberto Pereira da Cunha, 333, Guaratinguetá, SP 12516-410, Brazil
e-mail: giuliatti.winter@unesp.br</footnote>

<footnote n="2">² Université de Paris, Institut de Physique du Globe de Paris, CNRS, 75005 Paris, France</footnote>

<footnote n="3">³ Eldorado Research Institute, Av. Prof. Alan Turing 275, Cidade Universitária, Campinas, SP 13083-898, Brazil</footnote>

<footnote n="4">⁴ Swedish Institute of Space Physics – IRF, Box 812, 98128 Kiruna, Sweden</footnote>
<table><caption>**Table 1.** Orbital radii, width, and optical depth of both rings, C1R and C2R.</caption><thead><tr><th></th><th>C1R</th><th>C2R</th></tr></thead><tbody><tr><td>Orbital radii (km)</td><td>385.9</td><td>399.8</td></tr><tr><td>Width (km)</td><td>4.8–9.1</td><td>0.117</td></tr><tr><td>Optical depth</td><td>0.4</td><td>0.06</td></tr><tr><td></td><td colspan="2" style="text-align: center;">Chariklo</td></tr><tr><td>a × b × c (km)</td><td colspan="2">143.8 × 135.2 × 99.1</td></tr><tr><td>Mass (kg)</td><td colspan="2">6.3 × 10<sup>18</sup></td></tr><tr><td>Rotation period (h)</td><td colspan="2">7.004</td></tr></tbody></table>

**Notes.** Also included are the semi-axes (a, b, and c), the mass, and the rotation period of Chariklo (BR14; Leiva et al. 2017; M21).

Madeira et al. (2022) by assuming Chariklo as a spherical body with a mass anomaly at its equator. This assumption is based on observational data that suggests the presence of topographic features in the Centaur (Sicardy et al. 2019). Through a set of Poincaré surface of sections, Madeira et al. (2022) obtain that the non-spherical shape of Chariklo is responsible for an unstable region extending from its surface to an orbital radius of ~320 km, far inside the ring system. Despite the proximity between the 1:3 spin-orbit resonance and the inner ring, the authors verify that this resonance could be responsible for eccentricities ~10⁻², higher than expected for the ring particles. Their results show that the Chariklo rings are probably associated with orbits of the first kind.

Several papers have analysed the rings dynamics. El Moutamid et al. (2014) and Melita et al. (2017) discuss the possibility that the ring was formed from the disruption of an old satellite, which can occur if the satellite crosses the Roche limit of Chariklo. The location of the Roche limit depends on the physical parameters of both objects, and for this to match the current locations of the rings, the satellite must be porous, with a density much lower than Chariklo. In addition, the satellite must have a minimum radius of ~7 km (Melita et al. 2017). However, a problem with this hypothesis is the absence of mechanisms to bring the satellite to this limit. Tidal dissipation, the primary mechanism that could be responsible for this, is not a plausible option. Chariklo's corotation radius is within the locations of the rings. Therefore, a satellite beyond the Roche limit would migrate farther away from Chariklo unless it rotated much more slowly in the past.

Another possibility ruled out by Melita et al. (2017) is that the disruption is caused by a destructive impact of an old satellite with an external projectile, because the estimated timescale for such an event to occur is longer than Chariklo's lifetime. The authors also analysed the impactor flux in the Chariklo region and conclude that the ring formation due to an impact of a projectile with Chariklo is improbable.

Pan & Wu (2016) proposed that the close encounter that brought Chariklo to the Centaur region would enormously increase its temperature, being responsible for the sublimation of CO material. They estimated that Chariklo re-accretes part of this material, while the rest settles in the equatorial plane after multiple collisions. The rest of the material has various dust sizes which mechanically sticks together, forming a material disc that spreads out and forms the Chariklo system. More data on the Chariklo composition are needed to verify if such a process can produce the amount of material observed in the rings.

Hyodo et al. (2016) propose that the ring material may have formed by the partial tidal disruption of Chariklo during an

extreme close encounter. Their model assumed a differentiated Chariklo with an ice mantle, and it was analysed using hydrodynamical simulations. According to them, the planet's tidal effects instantly remove material from Chariklo's surface. Over time, such material settles in the equatorial plane mainly within the Roche limit and viscously spreads out. Finally, the material outside the Roche limit accretes into moons that destructively collide with each other, forming the rings and shepherd satellites (Hyodo & Ohtsuki 2015). This model has the advantage of explaining the ice composition of the rings (Duffard et al. 2014), and does not require the presence of an old satellite; however, it does require extremely rare close encounters (Araujo et al. 2016; Wood et al. 2017). Furthermore, the Chariklo composition is uncertain and more data is needed to verify the most plausible mechanism for the formation of the Chariklo system.

While several relevant works have analysed possible scenarios for the origin of the Chariklo rings, our focus in this work is to analyse the stability of the region in the light of the new parameters obtained for Chariklo (M21) in order to verify if the rings are located in a stable region and/or close to a resonance. This analysis was performed through a set of numerical simulations and also through the powerful technique of the Poincaré surface of section. Furthermore, we explore several confinement models for constrain these rings.

Our paper is divided into six sections. Section 2 deals with the dynamical system and also presents the results obtained from the numerical simulations, while Sect. 3 deals with the periodic and quasi-periodic orbits, studied in the light of the Poincaré surface of sections. In Sect. 4, we analyse the location of the rings in the $a_{eq}$ versus $e_{eq}$ map. In Sect. 5, we discuss different confinement models to constrain the rings. The conclusions on this work are presented in Sect. 6.

## 2. Dynamical system

The equations of motion of a massless particle around Chariklo, considering a body-fixed frame (Oxy) uniformly rotating with the same spin period of Chariklo, can be given by (Hu & Scheeres 2004)

$$ \ddot{x} - 2\omega\dot{y} = \omega^2 x + U_x \quad (1) $$

and

$$ \ddot{y} + 2\omega\dot{x} = \omega^2 y + U_y, \quad (2) $$

where $U_x$ and $U_y$ are the gravitational potential partial derivatives for Chariklo and $\omega$ is its spin velocity. Here we assume Chariklo is represented by a second-degree and second-order gravity field. The oblateness ($C_{20}$) and the ellipticity ($C_{22}$) are gravitational potential coefficients whose values can be computed from the ellipsoidal semi-axes (a, b, c) as (Balmino 1994)

$$ C_{20} = (2c^2 - a^2 - b^2)/10R_e^2 \quad (3) $$

and

$$ C_{22} = (a^2 - b^2)/20R_e^2, \quad (4) $$

where $a > b > c$ and $R_e = (ab/c)^{1/3}$. The gravitational potential can be expressed as (Hu & Scheeres 2004)

$$ U(x, y) = \frac{\mu}{r} \left( 1 - \left( \frac{R_e}{r} \right)^2 \left[ \frac{C_{20}}{2} - \frac{3C_{22}}{r^2} (x^2 - y^2) \right] \right), \quad (5) $$
<figure><img src="image_2.png" /><figcaption>**Fig. 1.** Snapshots of the orbital evolution (in the rotational frame with Chariklo) of a set of test particles under the effects of $C_{20}$ and $C_{22}$, the gravitational coefficients of Chariklo (black circle). The blue circle shows the location of the corotation radius, while the green and red circles show the semi-major axes of the 1:2 and 1:3 resonances, respectively.</figcaption></figure>

where $\mu$ is the gravity parameter and $r = \sqrt{x^2 + y^2}$. We note that the physical major axis of the body is aligned with the Ox axis of the rotating system.

In this section the Chariklo ring particle system described by Eqs. (1) and (2) is analysed into two different ways: i) through a set of numerical simulation and ii) through the technique of Poincaré surface of sections.

## 2.1. Numerical results

Our first goal is to find the inner edge of the stable region around Chariklo. For this we performed numerical simulations using a disc of non-interacting massless particles moving around Chariklo. In the gravitational potential of Chariklo, we take into account the contributions of its oblateness ($J_2$) and ellipticity ($C_{22}$). After some changes to include the $C_{22}$ contribution in the equations of motion (Celletti et al. 2017), an N-body simulation in the Rebound package (Rein & Liu 2012) with the IAS15 integrator (Rein & Spiegel 2015) was used to numerically integrate the system.

The particles were distributed with random values of the true longitude between 0°–360° from the equivalent radius ($R_{eq}$) of the central body (≈124 km) to the position of its main ring (≈400 km). Knowing that the inner edge of the disc undergoes large perturbations due to the azimuthal asymmetry of the central body, the amount of initial particles in this region is low since most of them are ejected or collide with the central body, consuming unnecessary computing resources. This region that

extends from the $R_{eq}$ to the corotational radius (≈189 km, Sicardy et al. 2019) has a set of 1000 particles, while the remaining part of the disc is composed of 40 000 particles.

All adopted parameters of Chariklo are given in Table 1. A collision is detected when the orbital radius of the particle is smaller than the equivalent radius of Chariklo, while those particles with a semi-major axis larger than five times the orbital radius of the main ring are removed from the system. The numerical simulation was carried out for 10 000 yr.

Figure 1 shows the initial positions of the particles (0 h), and the positions after 15 h, 15 days, 30 days, 1000 days, and after the complete time span of the numerical simulation (10 000 days). One day corresponds approximately to 3.43 Chariklo rotation periods. The blue circle shows the corotation semi-major axis, the green and the red circles show the location of the 1:2 and 1:3 spin-orbit resonances, respectively.

Under the effects of Chariklo's non-axisymmetric gravity field, the particles are removed from the inner region through collisions with Chariklo and ejections from the system. As can be seen, after 10 000 days, Chariklo's elongation clears a region up to the location of the 1:2 spin-orbit resonance (green circle) where the stable region begins.

This result shows the size of the unstable region for the recent refined physical parameters of Chariklo (M21). Comparing our results with those presented by Sicardy et al. (2019), there is a difference in the location of the inner edge of the stable region. This is mainly due to the assumed value of $C_{22}$, which is derived from the semi-axes ($a, b$, and $c$). The value of $C_{22}$ obtained from
the semi-axes given by M21 is almost half of the value assumed by Sicardy et al. (2019), which can explain the decrease in the unstable region.

## 2.2. Poincaré surface of section

It is known that the system has an integral of motion, the Jacobi constant ($C_j$). This conserved quantity, given by (Hu & Scheeres 2004)

$$C_j = \omega^2(x^2 + y^2) + 2U(x, y) - \dot{x}^2 - \dot{y}^2, \quad (6)$$

is used in the construction of the Poincaré surface of section. In order to unequivocally determine a particle in the phase space it is necessary to have four elements: two for the position $(x, y)$ and two for the velocity $(\dot{x}, \dot{y})$. Fixing a value for the Jacobi constant $C_j$ it becomes necessary to have just three of the four elements, for example, $x, y$, and $\dot{x}$. Defining the section as being $y = 0$, all points of the trajectory that cross this section in a given direction $(\dot{y}_0 < 0)$ can be plotted in the plane $(x, \dot{x})$, producing the Poincaré surface of section. Several works also used the Poincaré surface of section technique to study a two-body problem system with a central body with non-spherical distribution of mass (Scheeres et al. 1996; Jiang et al. 2016; Feng & Hou 2017; Borderes-Motta & Winter 2018; Winter et al. 2019; Madeira et al. 2022).

This is a numerical procedure where the equations of motion (1) and (2) were integrated using the Bulirsh–Stoer integrator (Bulirsch & Stoer 1966). The Newton-Raphson method was used to obtain the points of the trajectory that cross the section defined by $y = 0$, with an error of at most $10^{-13}$. For each Jacobi constant, $C_j$, we considered between 20 and 30 initial conditions. The choice of initial conditions is carried out in two stages. Firstly, we distribute a set of initial conditions equally spaced on the $Ox$ axis, with $x = 0$ and $\dot{y} > 0$. The $\dot{y}$ velocity is calculated using Eq. (6). These first initial conditions can generate the chaotic regions, the family of the first type orbits and the families of resonant orbits that have islands passing through the $\dot{x} = 0$ axis on the Poincaré surface of section. A second distribution of initial conditions equally spaced in $x \neq 0$ is needed for the resonant orbits that do not have islands crossing the $\dot{x} = 0$ axis in the Poincaré surface of section. This distribution occurs in the region where the resonance is found in the Poincaré surface of section.

The results of a surface of section are geometrically interpreted in a simple way, since periodic orbits produce a number of fixed points, while quasi-periodic orbits generate islands (closed curves) around the fixed points. Points spread over an area of the section are identified as chaotic trajectories.

As a reminder, we considered the Jacobi ellipsoid shape model proposed by M21 (see Table 1). Since $C_{22}$ is different from zero, resonances between the spin of Chariklo and the orbital motion of the particle appear in the system.

The 1:3 spin-orbit resonance is of particular interest once it is close to the location of the ring (Leiva et al. 2017). Through the Poincaré surface of sections, we explored a wide range of $C_j$ values in order to identify the islands associated with the 1:3 resonance. These islands exist for $7.337 \times 10^{-3} \text{ km}^2 \text{ s}^{-2} < C_j < 7.525 \times 10^{-3} \text{ km}^2 \text{ s}^{-2}$. The 1:3 resonance is shown in the plots of Fig. 2 (in green and purple).

It is important to note that, formally, this 1:3 resonance is a fourth-order 2:6 resonance since the potential (Eq. (5)) is invariant under a rotation of $\pi$ (Sicardy et al. 2019; Sicardy 2020), which is a doubled resonance that produces a pair of periodic orbits and their associated quasi-periodic orbits. Consequently,

there are two pairs of mirrored sets of islands in the Poincaré surface of sections (one pair in green and a second pair in purple) since each of the periodic orbits generates two fixed points with their islands of quasi-periodic orbits around them. From now on we refer to 1:3 resonance instead of 2:6 resonance. It is also valid for the 1:2 (2:4) resonance. Once this resonance is doubled in the phase space, a separatrix appears between the two families of periodic/quasi-periodic orbits, producing a chaotic region whose size depends on the Jacobi constant value.

In the Poincaré surface of sections (see Fig. 2) pairs of islands in green and pairs of islands in purple indicate the quasi periodic orbits associated with the 1:3 resonance. For $C_j = 7.337 \times 10^{-3} \text{ km}^2 \text{ s}^{-2}$ these islands are small and distant from the red islands' centre. As the value of $C_j$ increases their size increases and they move closer to the red islands' centre. The green and purple islands are bigger for $C_j \sim 7.374 \times 10^{-3} \text{ km}^2 \text{ s}^{-2}$, when they are near the red islands. As the $C_j$ value keeps increasing, the 1:3 resonance islands start to decrease in size and they move closer to the red islands' centre, being surrounded by red islands ($C_j = 7.525 \times 10^{-3} \text{ km}^2 \text{ s}^{-2}$). The evolution continues as they approach the red islands' centre, always getting smaller. A family of periodic orbits of the first kind (Poincaré 1895) is responsible for the red islands. This is discussed in detail in the following section.

## 3. Periodic orbits

Traditionally, periodic orbits in the planar, circular, restricted three-body problem have been classified as periodic orbits of the first kind and of the second kind (Poincaré 1895; Szebehely 1967). The resonant periodic orbits are the periodic orbits of the second kind whose particles are in eccentric orbits in a mean motion resonance. The less well-known periodic orbits are of the first kind, which are those that originated from particles initially in circular orbits in the unperturbed system (simple two-body problem).

Families of periodic orbits of the first kind have been studied in several systems. For example, in the restricted three-body problem, Broucke (1968) considered the Earth-Moon case, Winter & Murray (1997) studied in the Sun-Jupiter system, and Giuliatti Winter et al. (2013) found them in the Pluto-Charon system. Considering the restricted two-body problem, where the primary is a rotating non-spherical triaxial body, Borderes-Motta & Winter (2018) and Winter et al. (2019) show examples of both kinds of periodic orbits.

From the set of Poincaré surface of sections shown in Fig. 2, the dynamical structure of the region where the rings of Chariklo are located is determined by two families of 1:3 resonant periodic orbits (in purple and in green) and by a family of periodic orbits of the first kind (in red). We explore some features of these periodic orbits here.

Since the 1:3 resonance is doubled, we selected just one of the resonant periodic orbits to study. The other orbit is a mirrored image of this one. Considering the Jacobi constant $C_j = 7.337 \times 10^{-3} \text{ km}^2 \text{ s}^{-2}$, a 1:3 resonant periodic orbit is shown in Fig. 3. This is the periodic orbit shown in the Poincaré surface of section in Fig. 2 (first plot), which corresponds to the points at the centre of the islands shown in purple.

The top plot shows the trajectory in the rotating frame. The numbers indicate the time evolution of the trajectories, and show the locations equally spaced in time. In the rotating frame the trajectory is retrograde and symmetric with respect to the line $x = 0$, where the pericentre (P) and apocentre (A) of the trajectory
<figure><img src="image_3.png" /><figcaption>**Fig. 2.** Set of Poincaré surface of sections covering the whole 1:3 resonance evolution. There are two families of 1:3 resonant periodic orbits, indicated in purple and green. A family of first kind periodic orbits is responsible for the quasi-periodic orbits shown as red islands.</figcaption></figure>

are located. The period of this periodic orbit is $T = 21.01$ h, which is very close to three periods of rotation of Chariklo. In the inertial frame, the trajectory is prograde (middle). The temporal evolution of the orbital radii of the trajectory (bottom) also helps to visualise the trajectory shape.

The angle of the 1:3 resonance is given by $\phi_{1:3} = \lambda_C - 3\lambda + 2\omega$, where $\omega$ and $\lambda$ are the longitude of the pericentre and mean longitude of the particle, respectively, and $\lambda_C$ is the orientation angle of Chariklo. For all resonant trajectories shown in Fig. 2, the resonant angle oscillates around $\pi$ (orbits in purple) or $-\pi$ (orbits in green).

In Fig. 4, we present an example of a periodic orbit of the first kind, with $C_j = 7.337 \times 10^{-3} \text{ km}^2 \text{s}^{-2}$. Through a careful analysis, we verified that the trajectory of a particle in the rotating frame always follows a shape similar to the shape of Chariklo. The closest points of the trajectory (labelled 2 and 4) are aligned with the short axis of Chariklo, while the furthest points of the trajectory (labelled 1 and 3) are aligned with its long axis.

The period of this periodic orbit is $T = 11.5$ h, a little more than 1.5 times the spin period of Chariklo. We note that at the same time it completes one period in the rotating frame, the trajectory completes only a little more than half of its orbit around Chariklo in the inertial frame. The temporal evolution of the radial distance (bottom plot of Fig. 4) clearly shows that the trajectory has a pair of minima and a pair of maxima. This trajectory is not a usual Keplerian ellipse, with the central body

at one of the foci. The trajectory is actually like an ellipse with the central body at its centre.

A comparison between the radial amplitudes of oscillation of this periodic orbit of the first kind (bottom plot of Fig. 4) and the resonant periodic orbit given in the bottom plot of Fig. 3 shows a huge difference. We note that the resonant periodic orbit shows a radial oscillation of more than 190 km, while the periodic orbit of the first kind oscillates less than 1 km. This difference is analysed for the whole set of periodic orbits in the next section.

A striking difference between a periodic orbit of the first kind and a resonant periodic orbit is that the period (in the rotating frame) of a periodic orbit of the first kind varies significantly in a range that might cross several values that are commensurable without becoming resonant. The period of the periodic orbits in the rotating frame as a function of their Jacobi constant, $C_j$, is shown in Fig. 5. We note that the resonant periodic orbits 1:3 (in purple) exist only nearby the period commensurable with the spin period of Chariklo, while the period of the periodic orbits of the first kind covers a wide range of values (in red), crossing some periods that are commensurable with the spin period of Chariklo.

## 4. Location of the rings

Following the approach developed by Winter et al. (2019), we look for a correlation between the locations and sizes of the rings
<figure><img src="image_4.png" /></figure>

**Fig. 3.** Example of a 1:3 resonant periodic orbit whose Jacobi constant value is $C_j = 7.337 \times 10^{-3} \text{ km}^2 \text{s}^{-2}$ and whose period in the rotating frame is $T = 21.01$ h. The points at the centre of the islands in purple, shown in the Poincaré surface of section of Fig. 2 (first plot), correspond to this periodic orbit. The trajectory in the rotating frame is in the top plot, while the trajectory in the inertial frame is shown in the middle plot. The temporal evolution of the orbital radius is shown in the bottom plot. The numbers in the top and middle plots show the locations equally spaced in time, indicating the time evolution of the trajectory. The letters *P* and *A* indicate the location of the pericentre and the apocentre, respectively.

of Chariklo and the locations of the stable regions associated with the periodic orbits analysed in the last section.

As seen in Fig. 4, in the rotating frame, the first kind periodic orbits have an ellipsoidal shape with Chariklo at its centre, with a radial extent going from a minimum ($r_{\min}$) to a maximum ($r_{\max}$) radial distance from Chariklo. This same radial extent can be

<figure><img src="image_5.png" /></figure>

**Fig. 4.** Example of a first kind periodic orbit with $C_j = 7.337 \times 10^{-3} \text{ km}^2 \text{s}^{-2}$ and the period of the periodic orbit in the rotating frame is $T = 11.5$ h. The point at the centre of the islands in red, shown in the Poincaré surface of section of Fig. 2 (first plot), corresponds to this periodic orbit. The trajectory in the rotating frame is shown in the top plot, while the trajectory in the inertial frame is in the middle plot. The temporal evolution of the orbital radius is shown in the bottom plot. The numbers in the top and middle plots show the locations equally spaced in time, indicating the time evolution of the trajectory.

obtained by a Keplerian ellipse with a pair of equivalent semi-major axis and eccentricity ($a_{eq}$, $e_{eq}$), where $a_{eq} = (r_{\min} + r_{\max})/2$ and $e_{eq} = 1 - (r_{\min}/a_{eq})$ (Winter et al. 2019).

Adopting this same idea, each of the rings of Chariklo can be represented by a set of Keplerian ellipses with equivalent semi-major axis, $a_{eq}$ and eccentricity, $e_{eq}$, covering the same radial extent of the ring. Figure 6 (top panel) shows a comparison of
<figure><img src="image_6.png" /><figcaption>Fig. 5. Period of the periodic orbits in the rotating frame as a function of their Jacobi constant, $C_j$. In red are shown the periods for the first kind periodic orbits, while in purple are the values for the 1:3 resonant periodic orbits. Some periods that are commensurable with Chariklo's spin period ($T_{Chariklo}$), in the rotating frame, are indicated by the black straight lines.</figcaption></figure>

this region covered by these Keplerian ellipses and our results on the stable region around Chariklo, adopting the Jacobi ellipsoid shape model proposed by M21. The pink colour refers to the region of periodic and quasi-periodic orbits of the first kind (red islands in the Poincaré surface of sections in Fig. 2). This region is bounded by two red lines, one at the bottom, which corresponds to the semi-major axis and eccentricity of periodic orbits of the first kind, and one at the top, which refers to the quasi-periodic orbits of largest libration for each value of $C_j$. The yellow, blue, and green regions correspond to the widths of the 1:2, 2:5, and 1:3 resonances, respectively. Resonance width limits are obtained by calculating the pair ($a_{eq}$, $e_{eq}$) of the quasi-periodic orbits with the largest libration for each value of $C_j$. The black dashed lines indicate the centre of each of these resonances.

Additionally, the dark blue and coral regions indicate the equivalent region covered by C1R and C2R, respectively. The width of each ring was derived from the observations (M21) and they are represented by dashed lines (assuming the upper limit of C1R width provided by M21, $W = 9.1$ km). A particle located on the inner or outer edge of the C1R can assume any value of the eccentricity and semi-major axis defined in the dark blue region, which guarantees that the width of C1R will be about 9 km (M21).

The width of the dark blue region changes because a ring particle with a non-zero value of eccentricity needs to be located in a particular semi-major axis in order to keep the width of the ring (shown as dashed lines in dark blue and coral representing C1R and C2R, respectively). As the eccentricity of the particle increases, the values of the semi-major axis that this particle can be located decrease. For larger values of $e$ (>0.015) the excursions of the ring particle lead to a value larger than the width of the ring. Figure 6 (bottom panel) shows a zoomed-in image of the C1R region, with the horizontal dotted lines placing the limits of C1R eccentricity obtained by M21, and with eccentricities equal to 0.005 and 0.022.

From a certain value of the eccentricity (0.0006), it can be seen that the dark blue region enters the stable region of the orbits of the first kind, indicating that the C1R particles need to have a minimum value of eccentricity to be located in a stable

region. The upper limit of eccentricity (0.022), in turn, is outside the dark blue region. This value was obtained by M21 by adjusting the observed data from the Chariklo centre, corresponding to the upper bound for a three-sigma confidence level. For a one-sigma confidence level, the upper bound is 0.014, a value quite similar to the maximum eccentricity in the dark blue region (0.012). Therefore, our equivalent region of stability is consistent with the observed location of C1R. It should be noted that for a particle on the outer or inner edge of a ring located in the 1:3 resonance region, for example, for the values $e = 0.0205$ and $a = 392.55$ km (bottom point of the green area), the radial excursion of the particle would be very large, about 16 km.

For C2R the situation is different. Since it has a very small width, around 0.117 km (M21), the eccentricity of the particles must be very small (<0.00013). However, for C2R to be in a stable region (pink region), its eccentricity must be larger than 0.0006. Consequently, its width has to be larger than ~120 m (M21). This poses a problem with the stability of this ring.

## 5. Chariklo rings

The dynamics of the Chariklo rings have been discussed since their discovery; the similarities of these rings with the narrow rings of Saturn (e.g. Titan, Maxwell, Huygens ringlets; Colwell et al. 2009) and Uranus (e.g. $\alpha$, $\beta$, $\eta$ rings, French et al. 1991) have been highlighted by several works. The most recent data on the Chariklo system (M21) show that C1R and the Uranus $\epsilon$ ring share the characteristics of being narrow, dense, and eccentric. These analogies are positive as they enable us to build on our prior knowledge of narrow rings, being a good start to understanding the Chariklo inner ring.

In Sect. 5.1, we use classic planetary ring theory to extract some quantities about the Chariklo rings, while in Sect. 5.2 we estimate the timescale of material removal in the ring in the absence of confinement. In Sect. 5.3, we propose some confinement models for the rings.

### 5.1. Structure of the rings

Data from M21 show that C1R and C2R are both dense narrow rings; C1R corresponds to an eccentric structure, while C2R is probably a low eccentricity ring. In the C2R case the maximum eccentricity of the particles can be estimated as the ring half width over its radial location. From this calculation we obtained $e \sim 1.5 \times 10^{-4}$.

Now, C1R must have a positive eccentricity gradient ($\delta e$), and some kind of alignment of the pericentres of both edges is necessary in order to maintain its observed eccentric configuration. Assuming the simplest streamline mode for C1R and an initial alignment of the apse in the ring, the minimum $W_-$ and maximum $W_+$ radial widths of the ring are given by (Nicholson et al. 1978)

$$W_{\mp} = \delta a(1 \pm q), \qquad (7)$$

where $\delta a$ is the semi-major axis width of the ring (or mean width) and $q$ is the dimensionless eccentricity gradient. Taking the limit values obtained by M21 (Table 1), we find $\delta a = 6.95$ km and $q = 0.31$. From $q \approx a \delta e / \delta a$ (French et al. 1986) we obtain a positive eccentric gradient for the ring of $\delta e = 0.0056$.

Observational data from the narrow rings of Uranus and Saturn show that these structures show apse alignment, possibly caused by a combination of internal torques in the ring (Goldreich & Tremaine 1979a; Borderies et al. 1983;
<figure><img src="image_7.png" /></figure>

<figure><img src="image_8.png" /><figcaption>Fig. 6. Map of the stable region around Chariklo in $a_{eq}$ vs $e_{eq}$ space shown on the top plot. The stable region indicated by the pink colour is due to the first kind orbits. This region is limited by two red lines. The bottom line corresponds to the semi-major axis and eccentricity of the first kind periodic orbits, and the top line refers to quasi-periodic orbits. The yellow, blue, and green regions are related to 1:2, 2:5, and 1:3 resonances, respectively. The black dashed lines indicate the centres of each resonance, determined through the geometry of the resonant orbits. The dark blue and coral regions show the ranges ($a_{eq}$, $e_{eq}$) that correspond to the locations of the inner (C1R) and outer (C2R) rings of Chariklo, respectively. The dashed dark blue and coral lines show the edges of the rings. A zoom-in on the bottom plot shows two horizontal lines which indicate the limits of the eccentricities given by M21.</figcaption></figure>

Chiang & Goldreich 2000; Mosqueira & Estrada 2002; Papaloizou & Melita 2005). When the ring is narrower in periapse than in apoapse (which is true for $\delta e > 0$), the self-gravity effects are increased in the periapse. In this position, the outer half of the ring would be radially pulled by the inner half, resulting in a differential precession that (almost) cancels out the effect caused by the central body. Consequently, the ring would have a rigid precession, as a single entity (Goldreich & Tremaine 1979a; Borderies et al. 1983).

Additionally, a large number of collisions occurs at each orbital period in the ring, producing impulses that contribute to the differential precession. Inside the ring, the timescale of precession caused by collisions is much longer than that caused by the central body, and can be disregarded. However, if shepherd satellites are confining the ring, they generate pressure-induced acceleration in the particles, producing a double-peak profile in the ring (Chiang & Goldreich 2000).

Melita & Papaloizou (2020) obtain a double-peak profile for the rings of Chariklo, which is roughly consistent with the W-shape of C1R observed by M21. Furthermore, Melita & Papaloizou (2020) found that the Chariklo rings require surface densities of ~$10^2$ kg m$^{-2}$, one order of magnitude lower than the values estimated by BR14, and a minimum eccentricity gradient of $q = 0.01$. This value is smaller than the value we obtained, indicating that C1R is more eccentric than predicted by the theory.

We get an estimate of the ring surface density by invoking the fact that a collisional disc under the effects of pressure, self-gravity, and rotation is stable when its Toomre parameter is of the order of unity. The Toomre parameter is given by (Toomre 1964)

$$Q = \frac{\Omega_k c_s}{\pi G \Sigma}, \qquad (8)$$

where $\Omega_k$ is the angular frequency, $c_s$ is the dispersion velocity in the disc, $G$ is the gravitational constant, and $\Sigma$ is the surface density.

The dispersion velocity is related to the ring scale height $H$ by $c_s = H\Omega_k$ (Adachi et al. 1976); we take the latter as a radially dependent function $H = r_{orb} \sin i$, where $r_{orb}$ is the orbital radius at Chariklo and $i$ is the inclination of the rings, taken as $i = 5 \times 10^{-4}$ deg. This value was chosen to obtain rings of few metres in height, as proposed by BR14. Taking $Q = 1$, we find the following relation for surface density:

$$\Sigma \approx \frac{\Omega_k^2 r_{orb} \sin i}{\pi G}. \qquad (9)$$

We obtain $\Sigma \approx 110$ kg m$^{-2}$ for the Chariklo rings, which is in agreement with the values obtained by Melita & Papaloizou (2020).

The surface density for each ring is given in Table 2 along with the other values that are estimated in this section. It should be noted that all quantities presented in Table 2 were obtained following classic prescriptions that assume a spherical central body. Therefore, they must be interpreted as very rough estimates as we are not aware of how these prescriptions are affected by the shape of Chariklo.

With the surface density in hand, we can estimate the ring mass $m_r$ by (Goldreich & Tremaine 1979c)

$$m_r = 2\pi r_c W \Sigma, \qquad (10)$$

where $r_c$ is the ring's central position and $W$ is its width<fnref n="1" />. As a result, we obtain that if each ring originated from the disruption of an ancient body made of ice, it must have a radius of at least $R_{pb} = 780$ m and 200 m to produce the masses of C1R and C2R, respectively.

Another quantity that can be obtained is the mean radius $\bar{s}$ of the particles in the ring (Goldreich & Tremaine 1982)

$$\bar{s} = \frac{3\Sigma}{4\rho\tau}, \qquad (11)$$

where $\rho$ is the density of the particles assumed to be made of ice ($\rho = 10^3$ kg m$^{-3}$) and $\tau$ is the optical depth. The radius $\bar{s}$ corresponds to the radius of the ring particles if they all had a single

<footnote n="1">¹ To obtain the quantities shown in Table 2, we assumed the width of C1R as the mean width $\delta a$.</footnote>
<table><caption>**Table 2.** Quantities $\Sigma$, $m_r$, $\bar{s}$, $\tau_{dp}$, $\tau_{dp}$, and $\tau_{pr}$ estimated for C1R and C2R.</caption><thead><tr><th></th><th>Symbol</th><th>C1R</th><th>C2R</th><th>Comments</th></tr></thead><tbody><tr><td>Surface density (kg m<sup>-2</sup>)</td><td>Σ</td><td>118</td><td>109</td><td>see Eq. (9)</td></tr><tr><td>Ring mass (kg)</td><td>m<sub>r</sub></td><td>2 × 10<sup>12</sup></td><td>3 × 10<sup>10</sup></td><td>see Eq. (10)</td></tr><tr><td>Mean radius of particles (cm)</td><td>r&#773;</td><td>22</td><td>140</td><td>see Eq. (11)</td></tr><tr><td>Differential precession timescale (yr)</td><td>τ<sub>dp</sub></td><td>0.001</td><td>0.06</td><td>see Eq. (12)</td></tr><tr><td>Inter-particle collisions timescale (yr)</td><td>τ<sub>ic</sub></td><td>4000</td><td>7.3</td><td>see Eq. (13)</td></tr><tr><td>Poynting-Robertson timescale (yr)</td><td>τ<sub>pr</sub></td><td>10<sup>9</sup></td><td>10<sup>8</sup></td><td>see Eq. (14)</td></tr></tbody></table>

size. This quantity will be used as a fiducial value in later relations that require particle radius. We find $\bar{s} = 22$ cm and 140 cm for C1R and C2R, respectively.

These quantities can be used to evaluate the necessity for confinement, which we discuss below. This can be done by estimating the spreading timescales of a ring, which must be equal to or greater than the age of the Solar System. If the spreading timescale is less than the age of the Solar System, the ring is either a recent feature or it is confined by some effect that prevents the spreading. The first possibility is very unlikely since it would mean that we are at a privileged moment in the Solar System's history, making the second possibility the most likely.

## 5.2. Ring timescales

Several effects spread an unconstrained ring, such as differential precession, inter-particle collisions, and Poynting-Robertson drag. For each of these effects, we obtain a typical timescale that is used to assess the need for confinement mechanisms. Due to the lack of data, other effects that may contribute to the ring spreading are not considered, such as plasma drag, Yarkovsky effects and tidal dissipation.

Differential precession results from the effects of the non-sphericity of the central body on the ring particles. Despite the difficulty of working with the classic osculating orbital elements in a system around a prolate body (Ribeiro et al. 2021), we do a simple estimation of differential precession timescale $\tau_{dp}$ by assuming the apsidal precession of the orbits caused by Chariklo oblateness (modified from Murray & Dermott 2000)

$$ \tau_{dp} = \frac{2\pi}{3J_2\Omega_k R_c^2} \left(\frac{r_c^2 - \frac{w^2}{4}}{r_c W}\right)^2, \qquad (12) $$

where $J_2$ is the first seasonal harmonic ($C_{20}$). For Chariklo case, we estimate $J_2 \approx 0.13$, giving a precession timescale for the Chariklo rings of a few days.

The loss of energy due to collisions causes the continuous diffusion of particles, and the inter-particle collisions timescale $\tau_{ic}$ can be estimated as the time for a particle to move across the ring under the gravitational effect of other ring particles (Brahic 1977; Borderies et al. 1985; Salmon et al. 2010):

$$ \tau_{ic} \approx \frac{\Omega_k}{\tau} \left( \frac{\rho W}{c_s} \right)^2. \qquad (13) $$

We find $\tau_{ic} \sim 10^3$ yr and $\sim 10$ yr for C1R and C2R, respectively.

A ring particle constantly absorbs radiation from the Sun and re-emits part of it. Due to the particle's orbital motion, the re-emission is not isotropic, which gives rise to a drag force that causes the particle's orbital decay. The Poynting-Robertson drag

timescale $\tau_{pr}$ for a ring is given by (Goldreich & Tremaine 1979c; Burns et al. 1979)

$$ \tau_{pr} = \frac{W}{r_c} \frac{4\rho sc^2}{9\Phi}, \qquad (14) $$

where $s$ is the particle radius, $c$ is the speed of light, and $\Phi$ is the solar density flux at Chariklo. For C1R and C2R, we obtain $\tau_{pr} \sim 10^5 \times s(\mu\text{m})$ yr and $10^4 \times s(\mu\text{m})$ yr, respectively.

When we assume $\bar{s} = s$, we find $\tau_{pr}$ of the order of the age of the Solar System (Table 2), meaning that the rings could survive in the absence of confinement when only under the Poynting-Robertson effect. However, in the real ring, where there are particles of various sizes, micrometre and subcentimetre particles would be removed on much smaller timescales and only larger particles would remain in the ring after a few million years. By analysing mostly the differential precession and inter-particle collisions, the outer ring would spread on a timescale much shorter than the Solar System age, demonstrating that the Chariklo rings must in fact be confined by any physical process.

The shape and dynamics of a ring are strongly affected by the mass distribution of the central body (Tiscareno 2013), so it would be natural to assume the non-spherical shape of Chariklo as a possible confinement source for the system. Chariklo mass distribution is responsible for material depletion in Chariklo vicinity region; however, the depletion does not extend to the ring location, as verified in Sect. 4 and also in Sicardy et al. (2019).

The simplest known confinement mechanism is the confinement of particles around the Lagrangian points of a satellite, in the context of the restricted planar three-body problem (Brown 1911). Such a mechanism actually corresponds to a 1:1 mean motion resonance (MMR), and here we are interested in the horseshoe orbits, which are orbits that surround the satellite's $L_3$, $L_4$, and $L_5$ Lagrangian points. The total radial width, $W_{hso}$, of the region where particles are confined in horseshoe orbits is (Weissman & Wetherill 1974)

$$ W_{hso} = a_s \left( \frac{m_s}{M} \right)^{1/3}, \qquad (15) $$

where $a_s$ and $m_s$ are the semi-major axis and mass of the satellite, respectively, and $M$ is the central body mass.

Around the horseshoe orbits there is a region where the particles exhibit chaotic behaviour and are lost by collisions. The chaos in the system arises from the overlap of first-order MMRs with the satellite (Wisdom 1980), and may be a possible explanation for the apparent gap between C1R and C2R. The width of the gap $W_{gap}$ corresponds to (Duncan et al. 1989)

$$ W_{gap} = 2.6a_s \left( \frac{m_s}{M} \right)^{2/7}. \qquad (16) $$
Another mechanism that can confine an eccentric ring, especially its edges, is the eccentric resonance (ER) with a satellite. This type of resonance corresponds to an e-type MMR and is responsible for the exchange of angular momentum between satellite and particle. In the case of an isolated particle, the ER reduces to the Lindblad resonance, for which angular momentum variations are responsible for affecting the particle's eccentricity (Madeira & Giuliatti Winter 2020, 2022). When we are dealing with a ring as an entity, the variations in the angular momentum act by balancing the viscous effects resulting from particle collisions. Thus, the ER acts by preventing the segment from spreading.

First-order resonances are stronger than higher-order resonances, and are more likely to confine the rings. The leading term of the torque of a circular satellite $\mathcal{T}_{\text{ER}}$ on particles in an isolated $m + 1:m$ ER is given by (Goldreich & Tremaine 1979b; Longaretti 2018)

$$ \mathcal{T}_{\text{ER}} = \mp 3.76 \left(\frac{m_s}{M}\right)^2 \left|\frac{a_s}{x_e}\right|^2 \Omega_k^2 r_c^4 \Sigma, \quad (17) $$

where the upper and lower signs apply to the case where the satellite is internal and external to the ring particles, respectively, and $x_e$ is the distance between the satellite and the ring edge. To confine the ring segment the torque must be at least equal to the viscous torque $\mathcal{T}_{\text{vis}}$ given by (Lissauer et al. 1981)

$$ \mathcal{T}_{\text{vis}} = 3\pi\Sigma \left(\frac{\Omega_k r_c \Sigma}{\rho}\right)^2, \quad (18) $$

and the minimum satellite mass that confines the ring edge is (Longaretti 2018)

$$ m_s = 1.58 \frac{\Sigma}{a_s \rho} \left| \frac{x_e}{a_s} \right|^4 M. \quad (19) $$

As we approach the ring, we have the overlap of the first-order ERs with the ring edge; a satellite in this region would give rise to a chaotic region, as already discussed. The torque produced by a circular satellite in this condition is given by (Goldreich & Tremaine 1980; Longaretti 2018)

$$ \mathcal{T}_{\text{ER,c}} = \mp 3.35 \left(\frac{m_s}{M}\right)^2 \left|\frac{a_s}{x_e}\right|^4 \Omega_k^2 r_c^4 \Sigma. \quad (20) $$

We can obtain, by assuming the satellite inside the ring, that the mass for the object to keep open a gap of width $W$ in the ring is (Longaretti 2018)

$$ m_s = 1.19 \frac{\Sigma}{a_s \rho} \left(\frac{W}{a_s}\right)^{3/2} M. \quad (21) $$

In the following section we make use of these confinement mechanisms to analyse and propose confinement models for the Chariklo rings.

## 5.3. Confinement models

### 5.3.1. Confinement by one pair of shepherd satellites

Figure 7 (top panel) shows an envisioned confinement model for the rings, in which the same inner satellite confines the inner edges of both rings and an outer satellite confines the outer edges. To obtain the radius and position of the shepherd satellites, we followed an approach similar to that used in

<table><caption>**Table 3.** Locations of hypothetical satellites that may hold an edge of a Chariklo ring, due to ER.</caption><thead><tr><th>a<sub>s</sub> (km)</th><th>m + 1:m</th><th>R<sub>s</sub> (m)</th><th>Shepherding</th></tr></thead><tbody><tr><td>314.7</td><td>4:3</td><td>540</td><td>C1R inner edge</td></tr><tr><td>348.2</td><td>8:7</td><td>420</td><td>C1R inner edge</td></tr><tr><td>364.1 <sup>(1)</sup></td><td>16:15</td><td>330</td><td>C1R inner edge</td></tr><tr><td>366.0 <sup>(2)</sup></td><td>8:7</td><td>390</td><td>C2R inner edge</td></tr><tr><td>368.0</td><td>18:17</td><td>320</td><td>C1R inner edge</td></tr><tr><td></td><td>21:20</td><td>300</td><td>C1R inner edge</td></tr><tr><td></td><td>9:8</td><td>380</td><td>C2R inner edge</td></tr><tr><td>407.7 <sup>(3)</sup></td><td>12:13</td><td>320</td><td>C1R outer edge</td></tr><tr><td></td><td>25:26</td><td>230</td><td>C2R outer edge</td></tr><tr><td>408.6</td><td>23:24</td><td>240</td><td>C2R outer edge</td></tr><tr><td>415.8 <sup>(4)</sup></td><td>14:15</td><td>290</td><td>C2R outer edge</td></tr><tr><td>429.3</td><td>8:9</td><td>350</td><td>C2R outer edge</td></tr><tr><td></td><td>4:5</td><td>450</td><td>C1R outer edge</td></tr><tr><td>447.6</td><td>5:6</td><td>410</td><td>C2R outer edge</td></tr></tbody></table>

**Notes.** From left to right are shown the semi-major axis $a_s$ of the satellites, $m + 1:m$ ER which they are involved in, their minimum radius $R_s$, and which edge they confine. The satellites that can simultaneously confine a C1R edge and a C2R edge are in italics. <sup>(1)</sup>This configuration is shown by the green dot in Fig. 7 (top panel). <sup>(2)</sup>This configuration is shown by the green dot in Fig. 7 (bottom panel). <sup>(3)</sup>This configuration is shown by the blue dot in Fig. 7 (top panel). <sup>(4)</sup>This configuration is shown by the blue dot in Figs. 7 (middle and bottom panels)

Murray & Thompson (1990) and calculated the location of the $m + 1:m$ ERs associated with a hypothetical satellite, checking if any match the edges of the rings. For the inner edges, we looked for resonances in the range $1 \le m \le 30$ and varied the satellite position from $a_s = 160$ km until the C1R inner edge, keeping a semi-major axis interval of 100 m. For the outer edges, we assumed the range of $-30 \le m \le -1$, with the satellite position varying by steps of 100 m from the C2R outer edge until $a_s = 500$ km.

The resonance location is obtained numerically following the prescription given in Sicardy (2020) for an ellipsoidal object, with the resonance condition given by

$$ m(\Omega_{k,s} - \Omega_k) = \kappa, \quad (22) $$

where $\Omega_{k,s}$ is the angular frequency of the satellite and $\kappa$ is the radial frequency at the edge. After identifying a resonance between satellite and edge, we calculate the satellite's mass using Eq. (19). For simplicity, we assume a satellite with the same bulk density as the ring particles, that is, a satellite made of ice ($\rho = 10^3$ kg m$^{-3}$). For denser materials (e.g. silicates) without porosity, satellites smaller in radius are able to confine the ring, which means that our results correspond to an upper limit on the size of a possible shepherd satellite.

Table 3 shows some possible locations for the shepherd satellites, along with the ER that confines the edge, the minimum satellite radius, and which edge is confined. Due to the proximity between first- and second-order resonances for larger values of $m$, there is a possibility that $m + 2:m$ ERs with the shepherd satellites reside within the ring. These resonances are also responsible for angular momentum exchanges and, if they are inside a ring, they act to excite the particles. Given this, we present in Table 3 only the cases where the satellite generates a second-order resonance residing within C1R. In italics we flag the hypothetical satellites that could confine two edges simultaneously due to discrete ERs, corresponding to cases that could
<figure><img src="image_9.png" /></figure>

**Fig. 7.** Confinement models for the Chariklo rings. Top panel: model in which the inner and outer edges of the two rings are held by the same inner and outer shepherd satellite, respectively. Middle panel: satellite confining C1R in its horseshoe region and holding the C2R inner edge, while a shepherd satellite confines the C2R outer edge. Bottom panel: model with the innermost and outermost edges of the system confined by a pair of satellites and the gap maintained by a third satellite. Satellites are shown as dots with colours matching those of the edges they confine, while the grey regions represent the width of the rings (for location and physical radius of the satellites, see Table 3).

produce the confinement envisioned in this subsection. In Fig. 7 (top panel), we present only one of the possible satellite configurations capable of confining the rings. The inner edges of C1R and C2R are supported by a 390 m satellite due to a 16:15 and 8:7 ERs, respectively; the outer edges are confined by a satellite of 320 m of radius due to 12:13 (C1R) and 25:26 (C2R) ERs.

Cordelia and Ophelia straddle the $\epsilon$ ring, but also confine the $\delta$ (23:22 ER) and $\gamma$ (6:5 ER) rings, respectively (French et al. 1991; Nicholson et al. 2018). It is interesting to see that a similar mechanism can occur for the Chariklo rings. Based on the numerical simulations of Hänninen & Salo (1994, 1995), Goldreich et al. (1995) show that extremely narrow rings can be held by a single satellite in eccentric resonance, which we can envision to be the mechanism confining C2R. In this case, we would need only one satellite simultaneously in ER with one edge of each ring.

This single-sided shepherding is the mechanism that confine some ringlets of the C ring (Lewis et al. 2011) and occurs when the satellite torque is sufficient to reverse the angular momentum integrated over the ring streamlines (see Borderies et al. 1989).

Sickafoose & Lewis (2019) explored the single-sided shepherd-ing for the Chariklo rings and obtained encouraging results indicating that a single satellite might model both rings.

Rappaport (1998) showed that the torque originating from a dense narrow ring can confine the edge of another ring, which can lead us to speculate more complex confinement scenarios, such as satellites confining C2R and the inner edge C1R, while C2R holds the outer edge of C1R. However, such scenarios are only possible under specific conditions, and the confinement by a pair of satellites is a more credible mechanism.

The confinement by only one pair of shepherd satellites has the facility to spare a satellite in comparison to the classic model discussed in Sect. 5.3.3. However, it leaves the system without a mechanism for removing material from the gap. The absence of material between the rings can be explained without additional effects only if the two rings formed independently. If they formed in a single event, an additional mechanism must have acted in the system to remove material, helping to define the sharp edges of both rings.

### 5.3.2. Confinement by a co-orbital satellite

In this section we recovered the works of Dermott et al. (1979, 1980) for narrow rings and proposed a model where C1R would be confined to the horseshoe region of a satellite. The interesting point is that such a model has the convenience of explaining the eccentric shape of C1R since the ring will have the same eccentricity as the satellite (Dermott et al. 1979). From Eq. (15) we obtain that C1R is confined by a satellite with 2 km of radius, shown in Fig. 7 (middle panel) by the red dot. An external satellite is required to hold the C2R outer edge. In the figure, the blue dot corresponds to a satellite holding C2R at 14:15 ER (Table 3).

A satellite with a 2 km radius would be responsible for generating a chaotic region of half-width of 15 km (Eq. (16)). Given that the gap has an extension of 13.9 km, the C2R would thus be wholly embedded in the chaotic region, which could be an argument for invalidating this model. However, we recall that the recipe to get the chaotic region was developed assuming objects such as mass point. When considering Chariklo as a non-spherical body and the gravitational effects of other nearby satellites, the extension of the chaotic region may change, perhaps allowing a regular motion in the C2R region. Continuing this line of thought, the C2R would reside at the edge of the chaotic region, and therefore a single satellite would confine C1R and produce the gap.

### 5.3.3. Classic confinement model

An already classic confinement model for the Chariklo rings was proposed in BR14, where the C1R inner edge and the C2R outer edge would be confined by an ER with an inner and outer shepherd satellites, respectively. Additionally, a third satellite would be responsible for the gap between the structures, in analogy, for example, to the satellite Daphnis, responsible for maintaining the Keeler Gap in the A ring of Saturn (Weiss et al. 2009).

We qualitatively explore this model using the most recent observational data provided in M21, first estimating the mass needed for a satellite to hold the gap. Assuming an object made of ice and located at $a_s = 392.9$ km, we obtain from Eq. (21) a radius of ~150 $m^2$.

Equation (21) gives the width of the gap opened by a satellite in a ring implying that C1R and C2R in the past were a single

<footnote n="2">² For our calculation we assumed $\Sigma$ as the surface density of C1R.</footnote>
ring that were separated by this satellite. This is compatible, for example, with a scenario in which the disruption of an object originated a ring of material, with the satellite being the largest fragment, or a scenario where the satellite was formed in situ from material from an ancient ring.

As shown in Sect. 4, the 1:3 spin-orbit resonance with Chariklo is located between the two rings for large values of eccentricity. A satellite trapped in this resonance can open a gap between the rings and prevent them from spreading. If it is in 1:3 spin-orbit resonance, a satellite in the gap has a minimum eccentricity of 0.02 and a maximum eccentricity of 0.29 (Fig. 6), and this can contribute to the C1R eccentricity (Colwell et al. 2009). Therefore, it is possible that the inner edge of C1R and the outer edge of C2R are being held by shepherd satellites, while a satellite in 1:3 spin-orbit resonance with Chariklo maintains the gap between the rings.

An example of a system in this confinement model is shown in Fig. 7 (bottom panel). The innermost satellite (green dot) has a 320 m radius and confines the C1R inner edge (solid green line) due to a 18:17 ER. The outer edge of C2R (solid blue line) in the figure is confined by 14:15 ER with a 290 m satellite (blue dot), while the C1R outer edge and C2R inner edge (red solid lines) result from the gap caused by a 500 m satellite (red dot).

The fact that the satellites involved in the confinement have radii of less than one kilometre makes the classic model quite attractive since a set of reasonable origins can be imagined for these satellites. Some examples are the capture or disruption of an ancient satellite. The detection by occultation of angularly tiny objects near a ring is highly unlikely (Sicardy et al. 2015), explaining why these objects were not detected if they actually exist. Finally, the possibility of C1R and C2R having been a single entity in the past is a very appealing point for formation models.

A pragmatic analysis of the models presented here requires more extensive investigation, as it is still unknown how the physical processes discussed here are affected by the ellipsoidal shape of Chariklo. Our intention in this section is not to explain the dynamics of the Chariklo rings, but only to present some discussions that can be useful for future works on rings around non-axisymmetric bodies.

## 6. Discussion

The discovery of Chariklo's rings (C1R and C2R) brought new insight into planetary ring dynamics. A set of particles orbiting around small objects (compared to the giant planets) asymmetrically shaped is a new topic to be explored. According to the most recent data (M21), the mean width of C1R is about 7 km (a narrow ring), while its eccentricity is between 0.005 to 0.022. C2R is an even narrower ring, 120 m. Our work aims to bring new insights into the dynamics of this unusual ring system. Through a set of numerical simulations and an analysis of periodic and quasi-periodic orbits, we derived the following main results. The width of the unstable region, due to the irregular shape of Chariklo, is smaller when compared with the results presented in Sicardy et al. (2019). This difference is caused by the new parameters derived for the shape of Chariklo.

The presence of gravitational interaction between the ring particles will cause larger damping due to collisions, making the disc more circular (decreasing in eccentricity), although it probably will not change the size of the unstable region. The analysis of massive bodies with self-gravity is ongoing.

Through a detailed analysis of a sample of Poincaré surface of sections we derived the size and location of the stable region in a diagram $a_{eq}$ versus $e_{eq}$. For a given ring width (9 km for C1R), we computed values of $e$ and $a$ that a particle located on the inner or outer edge of the ring could assume. This places the inner ring (C1R) in the stable region if its eccentricity is larger than $6 \times 10^{-4}$, which agrees with the recent results. However, C2R is located outside the stable region. To be in the stable region, C2R needs to have a higher eccentricity value, and consequently a larger width. Therefore, the last data regarding the width of C2R needs to be revisited.

Three confinement mechanisms are discussed in the light of the theory of the known narrow planetary rings of the giant planets. The classical confinement model seems to be the most suitable. This model requires three small moonlets to confine the edges of the rings. Two small moonlets, interior to the inner edge of C1R and exterior to the outer edge of C2R, prevent the spreading in the rings through ERs (mean motion resonance). The gap between the rings would be opened by a third satellite located in the 1:3 spin-orbit resonance.

Due to the small satellites sizes required by the confinement models, it is possible to form the shepherd satellites in situ from an old ring or directly by disruption of an older object, which would also give rise to a ring of material. Both scenarios share similarities of requiring an ancient ring from which C1R and C2R were carved due to satellites gravitational effects. The eccentric and narrow shape of the Chariklo rings seems to indicate that the system around Centaur is more complex than we know, probably hosting shepherd satellites.

During the review of this paper two rings (Q1R and Q2R) were discovered by Morgado et al. (2023) and Pereira et al. (2023) around the trans-Neptunian object (5000) Quaoar located at 43.3 au. In addition to the rings, the satellite Weywot orbits Quaoar at about 24 radii of the central body. Both rings are well located interior to the orbit of Weywot. Q1R, at 7.4 radii from Quaoar, is a dense and irregular ring, resembling the clumpy F ring of Saturn (Morgado et al. 2023). The intriguing fact regarding this system is that Quaoar's rings are outside its Roche limit, where dense rings are expected to accrete into satellites. Morgado et al. (2023) claimed that collisions may keep the ring even outside the Roche limit.

More data on rings around Centaurs are needed to assess whether Chariklo is a rule or an exception among this class of objects, which will allow us to trace the plausibility of the mechanisms discussed. New data regarding different ring systems around different primary bodies will help us to unravel the dynamics involved in each system.

**Acknowledgements.** We are grateful to the referee for the comments and suggestions which helped us to improve the manuscript. This study was financed in part by the Aperfeiçoamento de Pessoal de Nível Superior (CAPES, Finance Code 001), Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP, Proc. 2016/24561-0, Proc. 2018/23568-6, Proc. 2021/07181-7, and Proc. 2023/09881-1), and Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq, Proc. 305210/2018-1 and Proc. 313043/2020-5). Thanks to the Brazilian Federal Agency for Support and Evaluation of Graduate Education (CAPES), in the scope of the Program CAPES-PrInt, process number 88887.310463/2018-00, International Cooperation Project number 3266. G.M. thanks to the Centre National d'Études Spatiales (CNES) and European Research Council (ERC). Numerical computations were partly performed on the S-CAPAD/DANTE platform, IPGP, France.

## References

Adachi, I., Hayashi, C., & Nakazawa, K. 1976, Progr. Theor. Phys., 56, 1756
Araujo, R. A. N., Sfair, R., & Winter, O. C. 2016, ApJ, 824, 80
Balmino, G. 1994, Celest. Mech. Dyn. Astron., 60, 331

Borderes-Motta, G., & Winter, O. C. 2018, MNRAS, 474, 2452

Borderies, N., Goldreich, P., & Tremaine, S. 1983, AJ, 88, 1560

Borderies, N., Goldreich, P., & Tremaine, S. 1985, Icarus, 63, 406

Borderies, N., Goldreich, P., & Tremaine, S. 1989, Icarus, 80, 344

Braga-Ribas, F., Sicardy, B., Ortiz, J. L., et al. 2014, Nature, 508, 72

Brahic, A. 1977, A&A, 54, 895

Broucke, A. 1968, Jet Propulsion Laboratory, (Pasadena: California Inst. Technol.), 32

Brown, E. W. 1911, Science, 33, 79

Bulirsch, R., & Stoer, J. 1966, Numer. Math., 8, 1

Burns, J. A., Lamy, P. L., & Soter, S. 1979, Icarus, 40, 1

Celletti, A., Efthymiopoulos, C., Gachet, F., Galeş, C., & Pucacco, G. 2017, Int. J. Non-Linear Mech., 90, 147

Chiang, E. I., & Goldreich, P. 2000, ApJ, 540, 1084

Colwell, J. E., Nicholson, P. D., Tiscareno, M. S., et al. 2009, in Saturn from Cassini-Huygens (Springer), 375

Colwell, J. E., Nicholson, P. D., Tiscareno, M. S., et al. 2009, The Structure of Saturn's Rings, eds. M. K. Dougherty, L. W. Esposito, & S. M. Krimigis, 375

Dermott, S. F., Gold, T., & Sinclair, A. T. 1979, AJ, 84, 1225

Dermott, S. F., Murray, C. D., & Sinclair, A. T. 1980, Nature, 284, 309

Duffard, R., Pinilla-Alonso, N., Ortiz, J. L., et al. 2014, A&A, 568, A79

Duncan, M., Quinn, T., & Tremaine, S. 1989, Icarus, 82, 402

El Moutamid, M., Kral, Q., Sicardy, B., et al. 2014, in AAS/Division of Dynamical Astronomy Meeting, 45, 402.05

Feng, J., & Hou, X. 2017, AJ, 154, 21

French, R. G., Elliot, J. L., & Levine, S. E. 1986, Icarus, 67, 134

French, R. G., Nicholson, P. D., Porco, C. C., & Marouf, E. A. 1991, Dynamics and Structure of the Uranian Rings, eds. J. T. Bergstrahl, E. D. Miner, & M. S. Matthews, 327

Giuliatti Winter, S., Winter, O., Vieira Neto, E., & Sfair, R. 2013, MNRAS, 430, 1892

Goldreich, P., & Tremaine, S. 1979a, AJ, 84, 1638

Goldreich, P., & Tremaine, S. 1979b, ApJ, 233, 857

Goldreich, P., & Tremaine, S. 1979c, Nature, 277, 97

Goldreich, P., & Tremaine, S. 1980, ApJ, 241, 425

Goldreich, P., & Tremaine, S. 1982, ARA&A, 20, 249

Goldreich, P., Rappaport, N., & Sicardy, B. 1995, Icarus, 118, 414

Hänninen, J., & Salo, H. 1994, Icarus, 108, 325

Hänninen, J., & Salo, H. 1995, Icarus, 117, 435

Hu, W., & Scheeres, D. 2004, Planet. Space Sci., 52, 685

Hyodo, R., & Ohtsuki, K. 2015, Nat. Geosci., 8, 686

Hyodo, R., Charnoz, S., Genda, H., & Ohtsuki, K. 2016, ApJ, 828, L8

Jiang, Y., Baoyin, H., Wang, X., et al. 2016, Nonlinear Dyn., 83, 231

Leiva, R., Sicardy, B., Camargo, J. I. B., et al. 2017, AJ, 154, 159

Lewis, M., Stewart, G., Leezer, J., & West, A. 2011, Icarus, 213, 201

Lissauer, J. J., Shu, F. H., & Cuzzi, J. N. 1981, Nature, 292, 707

Longaretti, P. Y. 2018, Theory of Narrow Rings and Sharp Edges, eds. M. S. Tiscareno, & C. D. Murray, 225

Madeira, G., & Giuliatti Winter, S. M. 2020, Eur. Phys. J. Spec. Top., 229, 1527

Madeira, G., & Giuliatti Winter, S. M. 2022, MNRAS, 513, 297

Madeira, G., Giuliatti Winter, S. M., Ribeiro, T., & Winter, O. C. 2022, MNRAS, 510, 1450

Melita, M. D., & Papaloizou, J. C. B. 2020, Icarus, 335, 113366

Melita, M. D., Duffard, R., Ortiz, J. L., & Campo-Bagatin, A. 2017, A&A, 602, A27

Morgado, B., Sicardy, B., Braga-Ribas, F., et al. 2021, A&A, 652, A141

Morgado, B., Sicardy, B., Braga-Ribas, F., et al. 2023, Nature, 614, 239

Mosqueira, I., & Estrada, P. R. 2002, Icarus, 158, 545

Murray, C. D., & Dermott, S. F. 2000, Solar System Dynamics

Murray, C. D., & Thompson, R. P. 1990, Nature, 348, 499

Nicholson, P. D., Persson, S. E., Matthews, K., Goldreich, P., & Neugebauer, G. 1978, AJ, 83, 1240

Nicholson, P. D., De Pater, I., French, R. G., & Showalter, M. R. 2018, The Rings of Uranus, eds. M. S. Tiscareno, & C. D. Murray, 93

Pan, M., & Wu, Y. 2016, ApJ, 821, 18

Papaloizou, J. C. B., & Melita, M. D. 2005, Icarus, 175, 435

Pereira, C., Sicardy, B., Morgado, B., et al. 2023, A&A, 673, A4

Poincaré, H. 1895, Gauthier-Villars et Is. Paris, 3

Rappaport, N. 1998, Icarus, 132, 36

Rein, H., & Liu, S.-F. 2012, A&A, 537, A128

Rein, H., & Spiegel, D. S. 2015, MNRAS, 446, 1424

Ribeiro, T., Winter, O. C., Mourão, D., Boldrin, L. A. G., & Carvalho, J. P. S. 2021, MNRAS, 506, 3068

Salmon, J., Charnoz, S., Crida, A., & Brahic, A. 2010, Icarus, 209, 771

Scheeres, D., Ostro, S., Hudson, R., & Werner, R. 1996, Icarus, 121, 67

Sicardy, B. 2020, AJ, 159, 102

Sicardy, B., Buie, M. W., Benedetti-Rossi, G., et al. 2015, in AAS/Division for Planetary Sciences Meeting Abstracts, 47, 104.01

Sicardy, B., Leiva, R., Renner, S., et al. 2019, Nat. Astron., 3, 146

Sickafoose, A., & Lewis, M. 2019, in EPSC-DPS Joint Meeting 2019

Szebehely, V. 1967, Theory of Orbits. The Restricted Problem of Three Bodies (New York: Academic Press)

Tiscareno, M. S. 2013, Planetary Rings, eds. T. D. Oswalt, L. M. French, & P. Kalas, 309

Toomre, A. 1964, ApJ, 139, 1217

Weiss, J. W., Porco, C. C., & Tiscareno, M. S. 2009, AJ, 138, 272

Weissman, P. R., & Wetherill, G. W. 1974, AJ, 79, 404

Winter, O., & Murray, C. 1997, A&A, 319, 290

Winter, O. C., Borderes-Motta, G., & Ribeiro, T. 2019, MNRAS, 484, 3765

Wisdom, J. 1980, AJ, 85, 1122

Wood, J., Horner, J., Hinse, T. C., & Marsden, S. C. 2017, AJ, 153, 245