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The quest for the solar g modes |
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| Authors: | T Appourchaux K Belkacem A-M Broomhall W J Chaplin D O Gough G Houdek J Provost F Baudin P Boumier Y Elsworth R A García B N Andersen W Finsterle C Fröhlich A Gabriel G Grec A Jiménez A Kosovichev T Sekii T Toutain S Turck-Chièze |
| Institution: | 1. Institut d’Astrophysique Spatiale, UMR8617, Batiment 121, 91405, Orsay Cedex, France 2. Institut d’Astrophysique et Géophysique, Université de Liège, Allée du 6 Ao?t 17, 4000, Liège, Belgium 3. School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK 4. Department of Applied Mathematics and Theoretical Physics, Institute of Astronomy, University of Cambridge, Cambridge, CB30HA, UK 5. Institute of Astronomy, University of Vienna, Türkenschanzstra?e 17, 1180, Vienna, Austria 6. Institute of Astronomy, University of Cambridge, Cambridge, CB30HA, UK 7. Université de Nice Sophia-Antipolis, CNRS, Laboratoire Cassiopée, Observatoire de la C?te d’Azur, BP 4229, 06304, Nice Cedex 4, France 8. Laboratoire AIM, CEA/DSM—CNRS, Université Paris Diderot, IRFU/ SAp, Centre de Saclay, 91191, Gif-sur-Yvette, France 9. Norwegian Space Centre, 0212, Oslo, Norway 10. Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center, 7260, Davos Dorf, Switzerland 11. Instituto de Astrofisica de Canarias, 38205, La Laguna, Tenerife, Spain 12. W.W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA, 94305, USA 13. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan 14. Center for Information Technology, University of Oslo, P. O. Box 1059, Blindern, 0316, Oslo, Norway |
| Abstract: | 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 conditions in the core. Owing to the existence of the convection zone, the g modes have very low amplitudes at photospheric levels, which makes the modes extremely hard to detect. In this article, we review the current state of play regarding attempts to detect g modes. We review the theory of g modes, including theoretical estimation of the g-mode frequencies, amplitudes and damping rates. Then we go on to discuss the techniques that have been used to try to detect g modes. We review results in the literature, and finish by looking to the future, and the potential advances that can be made—from both data and data-analysis perspectives—to give unambiguous detections of individual g modes. The review ends by concluding that, at the time of writing, there is indeed a consensus amongst the authors that there is currently no undisputed detection of solar g modes. |
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