Multiple coronal and heliospheric models have been recently upgraded at the Community Coordinated Modeling Center (CCMC), including the Wang-Sheeley-Arge (WSA)-Enlil model, MHD-Around-a-Sphere (MAS)-Enlil model, Space Weather Modeling Framework (SWMF), and heliospheric tomography using interplanetary scintillation data. To investigate the effects of photospheric magnetograms from different sources, different coronal models, and different model versions on the model performance, we run these models in 10 combinations. Choosing seven Carrington rotations in 2007 as the time window, we compare the modeling results with the Operating Mission as Nodes on the Internet data for near-Earth space environment during the late declining phase of solar cycle 23. Visual comparison is proved to be a necessary addition to the quantitative assessment of the models' capabilities in reproducing the time series and statistics of solar wind parameters. The MAS-Enlil model captures the time patterns of solar wind parameters better, while the WSA-Enlil model matches with the time series of normalized solar wind parameters better. Models generally overestimate slow wind temperature and underestimate fast wind temperature and magnetic field. Using improved algorithms, we have identified magnetic field sector boundaries (SBs) and slow-to-fast stream interaction regions (SIRs) as focused structures. The success rate of capturing them and the time offset vary largely with models. For this quiet period, the new version of MAS-Enlil model works best for SBs, while heliospheric tomography works best for SIRs. The new version of SWMF with more physics added needs more development. General strengths and weaknesses for each model are diagnosed to provide an unbiased reference to model developers and users. MotivationWe are motivated to validate the coronal and heliospheric models for the quasi-steady solar wind from the following three respects. First, a stream interaction region (SIR) forms when fast wind overtakes and interacts with the proceeding slow wind. It is in nature the same as the commonly known corotating interaction region [e.g., Smith and Wolfe, 1976;Gosling and Pizzo, 1999]. However, we use SIRs to emphasize that when the solar background changes within one Carrington rotation (CR), the resultant SIRs are short lived and do not corotate with the Sun to recur. In fact, Jian et al. [2006, 2011a] find 51% of SIRs near solar maximum and 10% at solar minimum do not recur at Earth. Large-amplitude Alfvén waves [Belcher and Davis, 1971] in SIRs and the following fast wind can drive a series of particle injections and affect the evolution of outer radiation belt (centered at about 4 R E ), as demonstrated in Miyoshi and Kataoka [2005]. Additionally, in geomagnetic storms, a large amount of energy is transferred from the solar wind into the magnetosphere and eventually dissipated in the thermosphere (about 90-600 km aboveground) and ionosphere (about 60-1000 km aboveground) by Joule heating and auroral precipitation [e.g., Gonzal...

Abstract. The ion dynamics in the distant Earth's magnetotail is studied in the case that a cross tail electric field E0 and reconnection-driven magnetic turbulence are present in the neutral sheet. The magnetic turbulence observed by the Geotail spacecraft is modeled numerically by a power law magnetic fluctuation spectrum. The magnetic fluctuations have the tearing mode parity with respect to the neutral sheet and are superimposed on a modified Harris sheet. A test particle simulation is performed for the ions, and the particle density, current density, bulk velocity, temperature, pressure, and heat flux are obtained for every point in the distant tail and as a function of the magnetic fluctuation level, 5B/Bo. It appears that the magnetic turbulence is very effective in maintaining the stationary structure of the current sheet and in changing the ion acceleration due to the electric field to thermal motion. Also, magnetic turbulence can inflate the current carrying region up to a thick current sheet, in contrast with the often assumed thin current sheet.