SEISMIC SOLAR MODELS AND THE EMITTED SOLAR NEUTRINO FLUXES

Sylvaine TURCK-CHIEZE & Sébastien COUVIDAT

Last update: 21/08/2001



On this web page are available some files and tables useful to calculate

different solutions to the neutrino oscillations. They result from several papers dedicated to the solar neutrino puzzle:


  • Papers on solar modelling and the solar physical processes (partial list, see other references therein):

Turck-Chièze et al. ApJ,335 (1988), 415

Turck-Chièze & Lopes, ApJ, 408 (1993), 347

Turck-Chièze et al., Phys. Rep., 230 (2-4), (1993), 57-235

Dzitko et al., ApJ, 447, (1995), 428

Turck-Chièze et al., Sol. Phys., 175, (1997), 247

Brun, Turck-Chièze & Morel, ApJ, 506, (1998), 913

Brun, Turck-Chièze, Zahn, ApJ, 525, (1999), 1032

Turck-Chièze et al., Sol. Phys., 200, (2001), 323

Turck-Chièze et al., ApJ, 555, (2001), L69



  • Papers on helioseismic data:

Gabriel et al., Sol. Phys., 162, (1995), 61

Scherrer et al., Sol. Phys., 162, (1995), 129

Gabriel et al., Sol. Phys., 175, (1997), 207

Kosovichev et al., Sol. Phys., 170, (1997), 43

Thiery et al., A&A, 355, (2000), 743; Basu et al., ApJ, 535, (2000), 1078

Bertello et al., ApJ, 535, (2000), 1066

Bertello et al., ApJ, 537, (2000), L143

Garcia et al., Sol. Phys., 200, 361

Visit also the WEB sites of NASA, ESA and IAS.!



  • A solar seismic model we computed:

  1. This seismic model is derived from observations of the acoustic modes with SoHO.

  2. With the GOLF and MDI instruments onboard, we can measure most of the acoustic modes that reach the solar core. Observations of the year 2001 concern modes that are weakly influenced by the turbulent surface, and are thus better determined.

  3. With our seismic model we built a solar model compatible with the seismic observations, and we can then reject different astrophysical solutions to the solar neutrino puzzle that were proposed in the past. We also improve our knowledge of the solar core and reduce the error bars on the emitted neutrino predictions.

All the details of the model will be described in a paper in preparation (Couvidat, Turck-Chièze et Kosovichev) and are summarized in the ApJ letter

"Solar Neutrino Emission Deduced from a Seismic Model ", Turck-Chièze et al., 2001, ApJ, 555, L69

Here we give access to our seismic model with a great number of shells, and also to the electron number density that is needed for the neutrino oscillations (see the observables derived from the model).



Above is a plot that shows the relative differences between:

(a) the square of the sound speed and (b) the density inside the Sun derived from the GOLF/MDI frequencies and those of different Saclay solar models. The models are a reference model (continuous curve), the Btz model of Brun, Turck-Chièze, Zahn, 1999 (dashed curve), and our seismic model (curve with error bars). Superimposed on the density profile are two other models: a model with the reaction rate of (3He,4He) reduced by 10% (dot-dot-dot-dashed curve) and a model with the reaction rates of the CNO poly-cycle reduced by 70% (dot-dashed curve) compared with the seismic model.




Below we list the different neutrino fluxes and their present uncertainties. These error bars have been reduced compared to past results:






For a complete table of the neutrino emissions see the detailed table of the neutrino fluxes

We shall continue to work on solar modelling for two main reasons:

    • oWe need to improve the description of the outer layers. This may be useful for the determination of the neutrino oscillations parameters

    • oWe wish to progress on the description of the rotation and magnetic field in the convective zone, which may have some impact on the neutrino propagation inside the Sun….

For questions or comments, you can write to: turck@cea.fr, couvidat@stanford.edu

The background picture was provided by the EIT instrument aboard the SoHO satellite