Planetary magnetotails: Model based on ISEE-3 and voyager-2 evidence |
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| Institution: | 1. Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany;2. Physical Faculty, Moscow State University, 119992 GSP-2 Lengory, Moscow, Russia;3. Institute of Radio-engineering and Electronics, ulitza Mokhovaya, 11/7, 125009 Moscow, Russia;4. The All-Russian Research Institute for Optical and Physical Measurements (VNIIOFI), 119361 Moscow, Ozernaya, Russia;1. Department of Mechanical Science and Engineering, Graduate School of Engineering, Nagoya University, Japan;2. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Japan;1. Institute of Space Systems, German Aerospace Center, Robert-Hooke-Str. 7, 28359 Bremen, Germany;2. Institute of Planetary Research, German Aerospace Center, Rutherford str. 7, Berlin, Germany;1. UNESP-Grupo de Dinâmica Orbital e Planetologia, Guaratinguetá, SP 12516-410, Brazil;2. Instituto Nacional de Pesquisas Espaciais, Av. dos Astronautas 1758, São José dos Campos, SP 12227-010, Brazil;3. Departament de Matemàtica Aplicada I, ETSEIB-UPC, Avda. Diagonal 647, 08028 Barcelona, Spain;4. Departament de Matemàtica Aplicada i Anàlisi, UB, Gran Vía 585, 08007 Barcelona, Spain |
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| Abstract: | It is shown that one can understand the basic properties of the quiet distant Earth's / and Jupiter's magnetotails as seen in the ISEE-3 / and Voyager-2 data (at distances ∼ 200 RE / and ∼ 6 000 RJ correspondingly behind the planets) within a simple hydromagnetic model with a partially “open” boundary. The degree of openness required to explain the lobe densities (≳ 10−1 / ≳ 10−2 cm−3) is ∼ 10−1 in both cases. This gives the average lobe magnetic field intensities: 8–9 / 0–0.5 nT. The tail flaring rate decreases at ∼ 100 RE / ∼ 1 000 RJ, and for larger distances non-circular tails are obtained with the average diameters ∼ 60 RE / ∼ 600 RJ, in agreement with the data. The degree of flattening (east-west to north-south ratio) is 1.2–2.3 / 4–10 depending on the pressure anisotropy in the solar wind. The expected lengths of the magnetic tails of Mercury, Saturh, Uranus are: 10–50 RM, (1–7)×103 RS, (1–6) × 103 RU, in corresponding planetary radii. |
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