Amplitudes of Solar Gravity Modes: A Review

Abstract

Solar gravity modes are considered as the {\it Rosetta Stone} for probing and subsequently deciphering the physical properties of the solar inner-most layers. Recent claims of positive detection therefore shed some new light on the long-standing issue of estimating solar gravity mode amplitudes. In this article, our objective is to review the theoretical efforts intended to predict solar gravity mode amplitudes. Because most of these studies assumed analogous driving and damping properties to those for the observed acoustic modes, we also provide a short overview of our current knowledge for these modes in the Sun and solar-type stars (which show solar-like oscillations) before diving into the specific problem of solar gravity modes. Finally, taking recent estimates into account, we conclude and confirm that the low-frequency domain (typically between $10\mu$Hz and $100\mu$Hz) is certainly more suited to focus on for detecting solar gravity modes. More precisely, around $60\mu$Hz, the theoretical estimates are slightly lower than the observational detection threshold as provided by the GOLF (Global Oscillations at Low Frequencies) instrument by about a factor of two only. This is typically within the current uncertainties associated with theoretical estimates and should motivate us for improving our knowledge on turbulence in the whole solar convective region, which is key for improving the accuracy of $g$-mode amplitude estimates. The recent detection of solar inertial modes (Gizon et al. 2021) combined with the continuous development of numerical simulations provide interesting prospects for future studies.

arXiv commentAccepted for publication in Solar Physics

References in corpus (52)

• Asteroseismology of Solar-Type and Red-Giant Stars
• Influence of gravity waves on the internal rotation and Li abundance of solar-type stars
• Internal Gravity Waves in Massive Stars: Angular Momentum Transport
• Theoretical amplitudes and lifetimes of non-radial solar-like oscillations in red giants
• Structure and Evolution of Giant Cells in Global Models of Solar Convection
• Stellar Evolution with Rotation and Magnetic Fields IV: The Solar Rotation Profile
• Giant star seismology
• Oscillations of alpha UMa and other red giants
• Excitation of stellar p-modes by turbulent convection: 1. Theoretical formulation
• The Liege Oscillation Code
• Asymptotic g modes: Evidence for a rapid rotation of the solar core
• Internal Gravity Wave Excitation by Turbulent Convection
• Solar structure and evolution
• The quest for the solar g modes
• Three-Dimensional Simulations of Massive Stars: I. Wave Generation and Propagation
• Stochastic excitation of nonradial modes II. Are solar asymptotic gravity modes detectable?
• Gravity Waves in the Sun
• Theoretical seismology in 3D : nonlinear simulations of internal gravity waves in solar-like stars
• Interaction Between Convection and Pulsation
• Numerical Simulations of Penetration and Overshoot in the Sun
• Solar inertial modes: Observations, identification, and diagnostic promise
• Spectrum and amplitudes of internal gravity waves excited by penetrative convection in solar-type stars
• Numerical 3D constraints on convective eddy time-correlations : consequences for stochastic excitation of solar p modes
• Theoretical power spectra of mixed modes in low mass red giant stars
• Stochastic excitation of non-radial modes I. High-angular-degree p modes
• Observational Searches for Solar g-modes: Some Theoretical Considerations
• Generation of internal gravity waves by penetrative convection
• The Salpeter plasma correction for solar fusion reactions
• Angular momentum redistribution by mixed modes in evolved low-mass stars. I. Theoretical formalism
• Damping rates of solar-like oscillations across the HR diagram. Theoretical calculations confronted to CoRoT and Kepler observations
• Amplitudes of stochastically excited oscillations in main-sequence stars
• Fragile detection of solar g modes by Fossat et al
• Dynamic screening correction for solar p-p reaction rates
• Stellar oscillations. II The non-adiabatic case
• Solar $p$-mode damping rates: insight from a 3D hydrodynamical simulation
• Two-dimensional simulations of solar-like models with artificially enhanced luminosity -- I. Impact on convective penetration
• Searching for g modes: Part II. Unconfirmed g-mode detection in the power spectrum of the time series of round-trip travel time
• Measurement of low signal-to-noise-ratio solar p modes in spatially-resolved helioseismic data
• Convective Excitation and Damping of Solar-like Oscillations
• Two-dimensional simulations of solar-like models with artificially enhanced luminosity. II. Impact on internal gravity waves
• Dipolar modes in luminous red giants
• A Critical Evaluation of Recent Claims Concerning Solar Rotation
• Turbulent eddy-time-correlation in the solar convective zone
• Seismic Solar Models from Ledoux discriminant inversions
• Stochastic excitation of acoustic modes in stars
• Signature of solar g modes in first-order p-mode frequency shifts
• Standard solar models: a perspective from updated solar neutrino fluxes and the gravity-mode period spacing
• Amplitude of solar gravity modes generated by penetrative plumes
• Modelling the asymmetries of the Sun's radial $p$-mode line profiles
• Coupling between turbulence and solar-like oscillations: a combined Lagrangian PDF/SPH approach. I -- The stochastic wave equation
• Coupling between turbulence and solar-like oscillations: A combined Lagrangian PDF/SPH approach. II - Mode driving, damping and modal surface effect
• Velocity-intensity asymmetry reversal of solar radial p-modes

Cited by in corpus (2)

• In search of gravity mode signatures in main sequence solar-type stars observed by Kepler
• From core to envelope: revealing the deep dynamics of stars with two convective zones