A model of the near magnetosphere with a dawn-dusk asymmetry 2. Parameterization and fitting to observations: A NEW MAGNETOSPHERE MAGNETIC FIELD MODEL, 2

By N. Tsyganenko. 2002

478 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/0773b33e63e89fc9358cd3870ada97cffaaff78d

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Citations in the corpus

A statistical study of EMIC waves observed by Cluster: 1. Wave properties (2014, methodology): “EMIC WAVE PROPERTIES 5578 magnetic field model with real-time solar wind input from the OMNI data set [Tsyganenko, 2002a, 2002b].”
First Results from the THEMIS Mission (2008, methodology): “The left portion of the image shows standard mapping using the Tsyganenko 2001 (Tsyganenko 2002a, 2002b) model, by varying the level of geomagnetic activity (Dst, AE) to determine the range of the footpoint locations and hence get an estimate of the mapping uncertainty.”
Precipitation of radiation belt electrons by EMIC waves, observed from ground and space (2008, methodology): “The magnetic field intensity was calculated using an empirical model [Tsyganenko, 2002a, 2002b].”
Modeling the dynamics of the inner magnetosphere during strong geomagnetic storms (2005, result): “TSK03, as in an earlier work [ Tsyganenko, 2002a, 2002b ] (hereinafter referred to as T02a and T02b), attempted to empirically model the delayed reaction of the magnetosphere to changing solar wind and IMF conditions.”
Magnetospheric configurations from a high-resolution data-based magnetic field model (2007, methodology): “[5] In the recent models [ Tsyganenko, 1995, 1996, 2002a, 2002b; Tsyganenko et al., 2003; Tsyganenko and Sitnov, 2005, referred henceforth as T96, T02a, b, TSK03, and TS05, respectively] the tail field was represented by a linear combination of two or three partial fields, or ‘‘modules’’ BT,i (i = ”
A model of the near magnetosphere with a dawn-dusk asymmetry 1. Mathematical structure (2002, background): “In particular, because of an oversimplified approximation for the ring current, the model field in the inner magnetosphere was found generally overstretched [Tsyganenko, 2001; Ganushkina et al., 2001], especially during strongly disturbed conditions.”
Storm‐time distortion of the inner magnetosphere: How severe can it get? (2003, result): “The first attempt to overcome that limitation was made in a recent work [Tsyganenko, 2002a, 2002b; hereinafter referred to as T02a, b], where the strengths of the tail, Birkeland, and partial ring currents at any given time included terms with the factors G 1 and G 2 , defined as integrals of…”
Simultaneous Cluster and IMAGE observations of cusp reconnection and auroral proton spot for northward IMF (2003, methodology): “The mapping is done using the Tsyganenko (T-89, T-96 and T-01) models [Tsyganenko, 2002, and references therein].”