Searching for the Signature of the Magnetic Fields at the Base of the Solar Convection Zone with Solar-Cycle Variations of p-Mode Travel Time

Details Searching for the Signature of the Magnetic Fields at the Base of the Solar Convection Zone with Solar-Cycle Variations of p-Mode Travel Time Searching for the Signature of the Magnetic Fields at the Base of the Solar Convection Zone with Solar-Cycle Variations of p-Mode Travel Time

2002-08-29

arxiv.org/abs/astro-ph/0208521v1

Astronomy and Astrophysics

Astrophysics

LaTeX (aastex-v5),14 pages,3 figures,submitted to ApJ Letters

Scientific paper

10.1086/344635

We study the solar-cycle variations of solar p-mode travel time for different wave packets to probe the magnetic fields at the base of the solar convection zone. We select the wave packets which return to the same spatial point after traveling around the Sun with integral number of bounces. The change in one-bounce travel time at solar maximum relative to minimum is approximately the same for all wave packets studied except a wave packet whose lower turning point is located at the base of the convection zone. This particular wave packet has an additional decrease in travel time at solar maximum relative to other wave packets. The magnitude of the additional decrease in travel time for this particular wave packet increases with solar activity. This additional decrease in travel time might be caused by the magnetic field perturbation and sound speed perturbation at the base of the convection zone. With the assumption that this additional decrease is caused only by the magnetic field perturbation at the base of the convection zone, the field strength is estimated to be about a 4-7x10^5 gauss at solar maximum if the filling factor is unity. We also discuss the problem of this interpretation.

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