Forward and Inverse Modeling for Jovian Seismology

Abstract

Jupiter is expected to pulsate in a spectrum of acoustic modes and recent re-analysis of a spectroscopic time series has identified a regular pattern in the spacing of the frequencies \citep{gaulme2011}. This exciting result can provide constraints on gross Jovian properties and warrants a more in-depth theoretical study of the seismic structure of Jupiter. With current instrumentation, such as the SYMPA instrument \citep{schmider2007} used for the \citet{gaulme2011} analysis, we assume that, at minimum, a set of global frequencies extending up to angular degree $\ell =25$ could be observed. In order to identify which modes would best constrain models of Jupiter's interior and thus help motivate the next generation of observations, we explore the sensitivity of derived parameters to this mode set. Three different models of the Jovian interior are computed and the theoretical pulsation spectrum from these models for $\ell \le 25$ is obtained. We compute sensitivity kernels and perform linear inversions to infer details of the expected discontinuities in the profiles in the Jovian interior. We find that the amplitude of the sound-speed jump of a few percent in the inner/outer envelope boundary seen in two of the applied models should be reasonably inferred with these particular modes. Near the core boundary where models predict large density discontinuities, the location of such features can be accurately measured, while their amplitudes have more uncertainty. These results suggest that this mode set would be sufficient to infer the radial location and strength of expected discontinuities in Jupiter's interior, and place strong constraints on the core size and mass. We encourage new observations to detect these Jovian oscillations.

arXiv comment31 pages, 12 figures, accepted to Icarus

References in corpus (12)

• Helioseismology
• The Interiors of Giant Planets: Models and Outstanding Questions
• The Interior Structure, Composition, and Evolution of Giant Planets
• Shock Compression of Deuterium and the Interiors of Jupiter and Saturn
• A new vision on giant planet interiors: the impact of double diffusive convection
• Ab initio Equation of State data for hydrogen, helium, and water and the internal structure of Jupiter
• A Massive Core in Jupiter Predicted From First-Principles Simulations
• The underlying physical meaning of the ${\nu }_{\max }-{\nu }_{\mathrm{c}}$ relation
• Jupiter models with improved ab initio hydrogen EOS (H-REOS.2)
• Detection of Jovian seismic waves: a new probe of its interior structure
• Predictions on the core mass of Jupiter and of giant planets in general
• A procedure for the inversion of f-mode travel times for solar flows

Cited by in corpus (7)

• Saturn Ring Seismology: Evidence for Stable Stratification in the Deep Interior of Saturn
• Giant Planets
• The effect of Jupiter oscillations on Juno gravity measurements
• Seismology of Giant Planets
• Pulsation Frequencies and Modes of Giant Exoplanets
• An Analysis of Stochastic Jovian Oscillation Excitation by Moist Convection
• A Possible Mechanism for Driving Oscillations in Hot Giant Planets