Modeling the dynamics of the inner magnetosphere during strong geomagnetic storms

By N. Tsyganenko, M. Sitnov. 2005

1,080 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/e39468c008a773addb88eebc7e31ce064cc5d97c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. R. Thorne
2. Nigel P. Meredith
3. Wen Li
4. R. Horne
5. Y. Shprits
6. Binbin Ni
7. Jacob Bortnik
8. S. Glauert

In Molecular Biology

1. R. Thorne
2. Wen Li
3. R. Horne
4. Nigel P. Meredith
5. Y. Shprits
6. Jacob Bortnik
7. M. Sitnov
8. S. Glauert

Citations in the corpus

• MESSENGER Observations of Mercury's Magnetic Field Structure (2012, background): “Removing current system modules from Earth magnetospheric models is problematic because the different modules are not independent, in particular the tail and ring current systems [e.g., Tsyganenko and Sitnov, 2005].”
• Statistical properties of plasmaspheric hiss derived from Van Allen Probes data and their effects on radiation belt electron dynamics (2015, methodology): “PLASMASPHERIC HISS PROPERTIES AND EFFECT 3396 defined as the geocentric distance to the point with minimum magnetic field intensity using the TS04D magnetic field model [Tsyganenko and Sitnov, 2005] for the field line threading the satellite.”
• The Magnetic Field of Mercury (2010, methodology): “Earth-analog models place at least some of the cross-tail current below the surface of the planet (Korth et al. 2004; Tsyganenko and Sitnov 2005).”
• 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 =…”
• Dynamics of the Earth’s Particle Radiation Environment (2009, neutral): “Recently Desorgher et al. (2009) compared the different Tsyganenko models (Tsyganenko 1989, 1995, 1996; Tsyganenko and Sitnov 2005) and the Alexeev and Feldstein 2000 model (Alexeev et al. 1996; Alexeev and Feldstein 2001).”
• Modeling the propagation characteristics of chorus using CRRES suprathermal electron fluxes (2007, background): “…longer distance due to the lower cyclotron growth rate, which is made possible by the concomitant decrease in the Landau fluxes and resultant increase in lf (Figure 4), as well as decreased field-line inhomogeneity on the dayside [Tsyganenko and Sitnov, 2005] allowing more uniform wave propagation.”
• Radiation belt electron acceleration by chorus waves during the 17 March 2013 storm (2014, methodology): “Note that L* is calculated for 90° pitch angle particles using the TS05 model [Tsyganenko and Sitnov, 2005].”
• The occurrence and wave properties of H+‐, He+‐, and O+‐band EMIC waves observed by the Van Allen Probes (2015, methodology): “We used the 2004 Tsyganenko and Sitnov magnetic field model (TS04D) [Tsyganenko and Sitnov, 2005] to calculate the L values using real-time solar wind inputs.”
• Storm time evolution of the outer radiation belt: Transport and losses (2006, methodology): “[6] Recently, Ukhorskiy et al. [2006] developed a new technique for calculating the inductive electric field corresponding to time evolution of geomagnetic field models and implemented it for the Tsyganenko and Sitnov [2005] (TS05) magnetic field model.”
• Event‐specific chorus wave and electron seed population models in DREAM3D using the Van Allen Probes (2014, methodology): “The PSD is evaluated using the Tsyganenko 04 storm time model (TS04) [Tsyganenko and Sitnov, 2005].”
• Radiation Belt Environment model: Application to space weather nowcasting (2008, methodology): “In this work, we use the Tsyganenko 2004 model [ Tsyganenko and Sitnov, 2005 ] for the magnetic field and Weimer model [Weimer, 2001] for electric field.”
• Gradual diffusion and punctuated phase space density enhancements of highly relativistic electrons: Van Allen Probes observations (2014, methodology): “Figure 4a shows an example of PSD values for March 2013 calculated from REPT data, using the Tsyganenko (TS)04 magnetic field model [Tsyganenko and Sitnov, 2005], and plotted in L* [see Roederer, 1970] versus time.”
• Particle Dynamics in the Earth's Radiation Belts: Review of Current Research and Open Questions (2020, methodology): “A similar effort was made in Kang et al. (2015) who computed pitch angle diffusion coefficients but with the simpler parallel approximation of Summers (2005) and the Tsyganenko 04 (T04) magnetic field model (Tsyganenko & Sitnov, 2005).”
• Effect of EMIC waves on relativistic and ultrarelativistic electron populations: Ground‐based and Van Allen Probes observations (2014, methodology): “1378 differential electron flux in the 2.3, 4.5, and 5.6MeV energy channels as a function of L* (electron drift shell in the T04 magnetic field model [Tsyganenko and Sitnov, 2005]) between 9 October and 29 November 2012.”