The quest for the solar g modes

  title={The quest for the solar g modes},
  author={Thierry Appourchaux and K'evin Belkacem and A-M. Broomhall and William J. Chaplin and Douglas O. Gough and G{\"u}nter Houdek and Janine Provost and Fr'ed'eric Baudin and Patrick Boumier and Yvonne P. Elsworth and R. A. Garcı́a and Bo Nyborg Andersen and Wolfgang Finsterle and Claus Fr{\"o}hlich and Alan H. Gabriel and G{\'e}rard Grec and Antonio J. Jimenez and Alexander G. Kosovichev and Takashi Sekii and Thierry Toutain and S. Turck-chi{\`e}ze},
  journal={The Astronomy and Astrophysics Review},
Solar gravity modes (or g modes)—oscillations of the solar interior on which buoyancy acts as the restoring force—have the potential to provide unprecedented inference on the structure and dynamics of the solar core, inference that is not possible with the well-observed acoustic modes (or p modes). The relative high amplitude of the g-mode eigenfunctions in the core and the evanesence of the modes in the convection zone make the modes particularly sensitive to the physical and dynamical… Expand
Signature of solar g modes in first-order p-mode frequency shifts
Context. Solar gravity modes (g modes) are buoyancy waves that are trapped in the solar radiative zone and have been very difficult to detect at the surface. Solar g modes would complement solarExpand
New insights on the solar core
Since the detection of the asymptotic properties of the dipole gravity modes in the Sun, the quest to find individual gravity modes has continued. An extensive and deeper analysis of 14 years ofExpand
Asymptotic g modes: Evidence for a rapid rotation of the solar core
We present the identification of very low frequency g modes in the asymptotic regime and two important parameters that have long been waited for: the core rotation rate, and the asymptoticExpand
Characterizing the propagation of gravity waves in 3D nonlinear simulations of solar-like stars
The revolution of helio- and asteroseismology provides access to the detailed properties of stellar interiors by studying the star's oscillation modes. Among them, gravity (g) modes are formed byExpand
Detecting individual gravity modes in the Sun
Many questions are still open regarding the structure and the dynamics of the solar core. By constraining more this region in the solar evolution models, we can reduce the incertitudes on someExpand
Nonparametric and Parametric Methods for Solar Oscillation Spectra
The study of the systematic oscillations of the Sun has led to better understanding of the Sun’s inner structure and dynamics, and may help to resolve inconsistencies between observations and theExpand
Detecting individual gravity modes in the Sun: Chimera or reality?
Abstract Over the past 15 years, our knowledge of the interior of the Sun has tremendously progressed by the use of helioseismic measurements. However, to go further in our understanding of the solarExpand
Theory of Stellar Oscillations
In recent years, astronomers have witnessed major progresses in the field of stellar physics. This was made possible thanks to the combination of a solid theoretical understanding of the phenomena ofExpand
The observational signatures of convectively excited gravity modes in main-sequence stars
We predict the flux and surface velocity perturbations produced by convectively excited gravity modes (g-modes) in main-sequence stars. Core convection in massive stars can excite g-modes toExpand
Theoretical seismology in 3D: nonlinear simulations of internal gravity waves in solar-like stars
Internal gravity waves (hereafter IGWs) are studied for their impact on the angular momentum transport in stellar radiation zones and the information they provide about the structure and dynamics ofExpand


On the Characteristics of the Solar Gravity Mode Frequencies
Gravity modes are the best probes for studying the dynamics of the solar radiative zone, and especially the nuclear core. This paper shows how specific physical processes influence the theoreticalExpand
Sensitivity of helioseismic gravity modes to the dynamics of the solar core
Context. The dynamics of the solar core cannot be properly constrained through the analysis of acoustic oscillation modes. Gravity modes are necessary to understand the structure and dynamics of theExpand
Probing the internal solar magnetic field through g modes
The observation of g-mode candidates by the Solar and Heliospheric Observatory (SOHO) mission opens the possibility of probing the internal structure of the solar radiative zone (RZ) and the solarExpand
Solar Oscillations and Convection. II. Excitation of Radial Oscillations
Solar p-mode oscillations are excited by the work of stochastic, nonadiabatic, pressure fluctuations on the compressive modes. We evaluate the expression for the radial mode excitation rate derivedExpand
Stochastic excitation of nonradial modes II. Are solar asymptotic gravity modes detectable
Detection of solar gravity modes remains a major challenge to our understanding of the innerparts of the Sun. Their frequencies would enable the derivation of constraints on the core physicalExpand
Observational Searches for Solar g-modes: Some Theoretical Considerations
We argue that the solar g-modes are unlikely to have caused the discrete peaks in the power spectrum of the solar wind flux observed by Thomson et al. (1995). The lower limit to the energy ofExpand
Theoretical Prediction of an Observed Solar g-Mode
This Letter considers the weak but persistent radial velocity variations measured by the Global Oscillations at Low Frequencies instrument on the Solar and Heliospheric Observatory satellite at 75.55Expand
Solar seismology. II - The stochastic excitation of the solar p-modes by turbulent convection
We test the hypothesis that the solar rho-modes are stabilized by damping due to turbulent viscosity in the convective zone. Starting from the assumption that the modes are stable, we calculateExpand
Solar seismology. I - The stability of the solar p-modes
We investigate the stability of the radial p-modes of the Sun by computing nonadiabatic eigen-values and e1genfunctions for a solar envelope model which extends from an inner radius r ≈ 0.3 R_☉ outExpand
In the early days of helioseismology, around 1975, independent detections of an oscillation with a period of 160 min in solar spectral line-shift data caused very substantial interest: it wasExpand