## 摘要

We present a comparison of the electron density and temperature behaviour in the ionosphere and plasmasphere measured by the Millstone Hill incoherent-scatter radar and the instruments on board of the EXOS-D satellite with numerical model calculations from a time-dependent mathematical model of the Earth's ionosphere and plasmasphere during the geomagnetically quiet and storm period on 20-30 January, 1993. We have evaluated the value of the additional heating rate that should be added to the normal photoelectron heating in the electron energy equation in the daytime plasmasphere region above 5000 km along the magnetic field line to explain the high electron temperature measured by the instruments on board of the EXOS-D satellite within the Millstone Hill magnetic field flux tube in the Northern Hemisphere. The additional heating brings the measured and modelled electron temperatures into agreement in the plasmasphere and into very large disagreement in the ionosphere if the classical electron heat flux along magnetic field line is used in the model. A new approach, based on a new effective electron thermal conductivity coefficient along the magnetic field line, is presented to model the electron temperature in the ionosphere and plasmasphere. This new approach leads to a heat flux which is less than that given by the classical Spitzer-Harm theory. The evaluated additional heating of electrons in the plasmasphere and the decrease of the thermal conductivity in the topside ionosphere and the greater part of the plasmasphere found for the first time here allow the model to accurately reproduce the electron temperatures observed by the instruments on board the EXOS-D satellite in the plasmasphere and the Millstone Hill incoherent-scatter radar in the ionosphere. The effects of the daytime additional plasmaspheric heating of electrons on the electron temperature and density are small at the F-region altitudes if the modified electron heat flux is used. The deviations from the Boltzmann distribution for the first five vibrational levels of N_{2}(ν) and O_{2}(ν) were calculated. The present study suggests that these deviations are not significant at the first vibrational levels of N_{2} and O_{2} and the second level of O_{2}, and the calculated distributions of N_{2}(ν) and O_{2}(ν) are highly non-Boltzmann at vibrational levels v > 2. The resulting effect of N_{2}(ν > 0) and O_{2}(ν > 0) on NmF2 is the decrease of the calculated daytime NmF2 up to a factor of 1.5. The modelled electron temperature is very sensitive to the electron density, and this decrease in electron density results in the increase of the calculated daytime electron temperature up to about 580 K at the F2 peak altitude giving closer agreement between the measured and modelled electron temperatures. Both the daytime and night-time densities are not reproduced by the model without N_{2}(ν > 0) and O_{2}(ν > 0), and inclusion of vibrationally excited N_{2} and O_{2} brings the model and data into better agreement.

原文 | English |
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頁（從 - 到） | 1257-1272 |

頁數 | 16 |

期刊 | Annales Geophysicae |

卷 | 18 |

發行號 | 10 |

DOIs | |

出版狀態 | Published - 2000 十月 |

## All Science Journal Classification (ASJC) codes

- 天文和天體物理學
- 地質學
- 大氣科學
- 地球與行星科學（雜項）
- 空間與行星科學