| タイトル | Latitudinal Dependence of the Radial IMF Component - Interplanetary Imprint |
| 本文（外部サイト） | http://hdl.handle.net/2060/19970021679 |
| 著者（英） | Suess, S. T.; Nerney, S.; Smith, E. J.; Phillips, J.; Goldstein, B. E. |
| 著者所属（英） | NASA Marshall Space Flight Center |
| 発行日 | 1996-06-14 |
| 言語 | eng |
| 内容記述 | Ulysses measurements have confirmed that there is no significant gradient with respect to heliomagnetic latitude in the radial component, B(sub r,), of the interplanetary magnetic field. There are two processes responsible for this observation. In the corona, the plasma beta is much less than 1, except directly above streamers, so both longitudinal and latitudinal (meridional) gradients in field strength will relax, due to the transverse magnetic pressure gradient force, as the solar wind carries magnetic flux away from the Sun. This happens so quickly that the field is essentially uniform by 5 solar radius. Beyond 10 solar radius, beta is greater than 1 and it is possible for a meridional thermal pressure gradient to redistribute magnetic flux - an effect apparently absent in Ulysses and earlier ICE and Interplanetary Magnetic Physics (IMP) data. We discuss this second effect here, showing that its absence is mainly due to the perpendicular part of the anisotropic thermal pressure gradient in the interplanetary medium being too small to drive significant meridional transport between the Sun and approx. 4 AU. This is done using a linear analytic estimate of meridional transport. The first effect was discussed in an earlier paper. |
| NASA分類 | Lunar and Planetary Exploration |
| レポートNO | 97N22577
NASA-CR-204716
NAS 1.26:204716 |
| 権利 | No Copyright |
| URI | https://repository.exst.jaxa.jp/dspace/handle/a-is/101467 |
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