Physics
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh53b1505b&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #SH53B-1505
Physics
2104 Cosmic Rays, 2134 Interplanetary Magnetic Fields
Scientific paper
A linear relationship between the observed 26-day recurrent cosmic-ray intensity variations and the global latitudinal gradient was first reported by Zhang (1997, ApJ, 488), who made extensive use of Ulysses data. This relationship is seen for all species considered and at all latitudes covered by the spacecraft. Burger and Hitge (2004, ApJL, 617) used a three-dimensional steady-state numerical modulation model and showed that a Fisk-type (Fisk 1996, JGR, 101) heliospheric magnetic field (HMF) can in principle explain these observations, at least at high latitudes. In this progress report we use a refinement of the Fisk-Parker hybrid HMF model of Burger and Hitge (2004) by Kruger (2006, MSc dissertation, NWU University) (see also Kruger, Burger and Hitge 2005, AGU Fall meeting abstracts SH23B-0341) to study these 26-day recurrent variations in more detail with the same modulation code. In Kruger's model the HMF is Parker-like at the highest latitudes, becomes Fisk- like at intermediate latitudes, and becomes Parker-like again in the region swept out by the wavy current sheet. By using an almost continuous range of latitudinal gradients for both solar magnetic polarity cycles and for both protons and electrons - in contrast to the limited number of values used by Burger and Hitge (2004) - the structure of the graphs of amplitude of the recurrent cosmic-ray intensity variations as function of global latitudinal gradient can be studied in detail. This was performed in a 100 AU model heliosphere for solar minimum conditions with the tilt angle of the heliospheric current sheet at 10 degrees. In all cases drift effects are included. We find that these curves for amplitude vs. latitudinal gradient are similar for protons and for electrons. By switching the sign of the modeled amplitudes when the latitudinal gradient becomes negative, the existence of a single relationship between the two quantities can be studied for the whole range of modeled latitudinal gradients. This study shows that a single second-order fit gives better results than a first-order fit for the whole range of latitudinal gradients (and consequently for both species and both solar magnetic polarities) and that there is a difference in the amplitudes for high- and for low rigidities, even if the latitudinal gradient is the same. This difference is a minimum at latitudes where the Fisk-type field is expected to dominate. In the ecliptic at 1 AU, we find that at high rigidity, the amplitude of the recurrent variations is larger for protons during A > 0 polarity epochs than for A < 0 epochs. This is in agreement with observational results of Richardson, Cane and Wibberenz (1999, JGR, 104). For the case of a Parker field, the modeled amplitudes have about the same magnitude for both polarity epochs. Note that what we discus here are preliminary results, and while they clearly suggest the existence of a Fisk-type HMF, the role of the diffusion tensor (and the associated turbulence quantities) has yet to be determined.
Burger R. A.
Engelbrecht E. E.
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