Magnetosheath for almost-aligned solar wind magnetic field and flow vectors: Wind observations across the dawnside magnetosheath at x = -12 Re

• Autores: Farrugia, C. J.; Erkaev, N. V.; Torbert, R.; Biernat, H. K.; Gratton, Fausto Tulio Livio; Szabo, A.; Kucharek, H.; Matsui, H.; Lin, R. P.; Ogilvie, K.; Lepping, R. P.; Smith, C. W.
• Año de publicación: 2010
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: MAGNETOSPHERE; KELVIN-HELMHOLTZ; WAVES; INSTABILITIES
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

While there are many approximations describing the flow of the solar wind past the magnetosphere in the magnetosheath, the case of perfectly aligned (parallel or anti-parallel) interplanetary magnetic field (IMF) and solar wind flow vectors can be treated exactly in a magnetohydrodynamic (MHD) approach. In this work we examine a case of nearly-opposed (to within 15) interplanetary field and flow vectors, which occurred on October 24-25, 2001 during passage of the last interplanetary coronal mass ejection in an ejecta merger. Interplanetary data are from the ACE spacecraft. Simultaneously Wind was crossing the near-Earth (X ∼ -13 Re) geomagnetic tail and subsequently made an approximately 5-hour-long magnetosheath crossing close to the ecliptic plane (Z = -0.7 Re). Geomagnetic activity was returning steadily to quiet, "ground" conditions. We first compare the predictions of the Spreiter and Rizzi theory with the Wind magnetosheath observations and find fair agreement, in particular as regards the proportionality of the magnetic field strength and the product of the plasma density and bulk speed. We then carry out a small-perturbation analysis of the Spreiter and Rizzi solution to account for the small IMF components perpendicular to the flow vector. The resulting expression is compared to the time series of the observations and satisfactory agreement is obtained. We also present and discuss observations in the dawnside boundary layer of pulsed, high-speed (v ∼ 600 km/s) flows exceeding the solar wind flow speeds. We examine various generating mechanisms and suggest that the most likely cause is a wave of frequency 3.2 mHz excited at the inner edge of the boundary layer by the Kelvin-Helmholtz instability. Copyright 2010 by the American Geophysical Union.
Fil: Farrugia, C. J.. University Of New Hampshire Durham; Reino Unido
Fil: Erkaev, N. V.. Institute Of Computational Modelling Of The Siberian Branch Of The Ras; Rusia
Fil: Torbert, R.. University Of New Hampshire Durham; Reino Unido
Fil: Biernat, H. K.. Osterreichische Akademie Der Wissenschaften; Austria. Karl-franzens-universitat Graz; Austria
Fil: Gratton, Fausto Tulio Livio. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física del Plasma. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física del Plasma; Argentina
Fil: Szabo, A.. Nasa Goddard Space Flight Center; Estados Unidos
Fil: Kucharek, H.. University Of New Hampshire Durham; Reino Unido
Fil: Matsui, H.. University Of New Hampshire Durham; Reino Unido
Fil: Lin, R. P.. Space Sciences Laboratory At Uc Berkeley; Reino Unido
Fil: Ogilvie, K.. Nasa Goddard Space Flight Center; Estados Unidos
Fil: Lepping, R. P.. Nasa Goddard Space Flight Center; Estados Unidos
Fil: Smith, C. W.. University Of New Hampshire Durham; Reino Unido