Temperature Distributions in the Protosatellite Disks of Uranus, Jupiter, Neptune and Saturn and Common Structure in Their Satellite Systems

TL;DR

This paper proposes a unified model explaining the formation and structure of satellite systems around Uranus, Jupiter, Neptune, and Saturn, based on resonant radiative interactions in their protosatellite disks that influence temperature distributions and orbital radii.

Contribution

It introduces a novel resonance model involving stimulated radiative molecular association to explain satellite orbital radii and temperature distributions across different planetary systems.

Findings

Similar orbital structures suggest a common formation mechanism.

Resonance through SRMA reactions explains specific satellite and ring placements.

Temperature distributions correlate with satellite orbital radii.

Abstract

We observe similar structures in the orbital radii of satellite and ring systems of Uranus, Jupiter and Neptune. This stimulates an investigation that the evolution of these systems and Saturn's system is initiated by a common mechanism that involves the interaction of radiation with their subnebulae (protosatellite disks). A model is presented that is characterized by resonance created through stimulated radiative molecular association (SRMA) reactions. In this model thermal energy is extracted from a protoplanetary disk at specific distances from the protoplanet wherever there is a match between the local thermal energy of the disk and the energy of photons impinging on the disk. Radiation is supplied by a portion of the hydrogen molecule's spectrum for the Uranian, Jovian and Neptunian disks and a portion of the hydrogen atom's spectrum for the Saturnian disk. Findings shed light on the early evolution and structure of satellite systems including the complicated ring system of Saturn. They also link satellite orbital radii size distributions to shapes of temperature distributions (TD's) in protosatellite disks. Theoretically determined TD's in the protosatellite disks of Uranus (Mousis 2004) and Saturn (Mousis Gautier and Bockelee-Moran, 2002) are essential to the present investigation.