Cronomoons: origin, dynamics, and light-curve features of ringed exomoons

Author:

Sucerquia Mario12ORCID,Alvarado-Montes Jaime A34,Bayo Amelia12ORCID,Cuadra Jorge52ORCID,Cuello Nicolás6ORCID,Giuppone Cristian A7ORCID,Montesinos Matías82,Olofsson J129ORCID,Schwab Christian34,Spitler Lee3410,Zuluaga Jorge I11ORCID

Affiliation:

1. Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, 5030 Casilla, Valparaíso, Chile

2. Núcleo Milenio Formación Planetaria - NPF, Universidad de Valparaíso, Av. Gran Bretaña 1111, Valparaíso, Chile

3. Department of Physics & Astronomy, Macquarie University – Sydney, NSW 2109, Australia

4. Centre for Astronomy, Astrophysics and Astrophotonics, Macquarie University – Sydney, NSW 2109, Australia

5. Departamento de Ciencias, Facultad de Artes Liberales, Universidad Adolfo Ibáñez, Avenida Padre Hurtado 750, Viña del Mar, Chile

6. Univ. Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

7. Universidad Nacional de Córdoba, Observatorio Astronómico - IATE. Laprida 854, 5000 Córdoba, Argentina

8. Escuela de Ciencias, Universidad Viña del Mar, Viña del Mar, Chile

9. Max Planck Institute for Astronomy, Künigstuhl 17, D-69117 Heidelberg, Germany

10. Australian Astronomical Optics, 105 Delhi Rd, North Ryde, NSW 2113, Australia

11. SEAP research group, Instituto de Física, FCEN, Universidad de Antioquia – Calle 70 No. 52-21, Medellín, Colombia

Abstract

Abstract In recent years, technical and theoretical work to detect moons and rings around exoplanets has been attempted. The small mass/size ratios between moons and planets means this is very challenging, having only one exoplanetary system where spotting an exomoon might be feasible (i.e. Kepler-1625b i). In this work, we study the dynamical evolution of ringed exomoons, dubbed cronomoons after their similarity with Cronus (Greek for Saturn), and after Chronos (the epitome of time), following the Transit Timing Variations (TTV) and Transit Duration Variation (TDV) that they produce on their host planet. Cronomoons have extended systems of rings that make them appear bigger than they actually are when transiting in front of their host star. We explore different possible scenarios that could lead to the formation of such circumsatellital rings, and through the study of the dynamical/thermodynamic stability and lifespan of their dust and ice ring particles, we found that an isolated cronomoon can survive for time-scales long enough to be detected and followed up. If these objects exist, cronomoons’ rings will exhibit gaps similar to Saturn’s Cassini Division and analogous to the asteroid belt’s Kirkwood gaps, but instead raised due to resonances induced by the host planet. Finally, we analyse the case of Kepler-1625b i under the scope of this work, finding that the controversial giant moon could instead be an Earth-mass cronomoon. From a theoretical perspective, this scenario can contribute to a better interpretation of the underlying phenomenology in current and future observations.

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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