Fig. 1


General overview of Run 2. Panel A: magnetosonic Mach number = 2 and cometopause surfaces (orange and red, respectively) and the electron fluid-velocity streamlines, overlaid with the simulation grid displaying the grid refinements. On the X =−1000 km plane, the magnetic field magnitude is displayed in blue. Panel B: magnetic field lines connected to the comet-Sun line, viewed along the direction of the convective electric field. Features of the environment listed in the main text are annotated in the panels. Panel C: values of the magnetic field magnitude B and solar wind H+ bulk values (number density , bulk velocity and thermal velocity vth) relative to upstream values, along the X-axis from X =−1000 to X = 9000 km. Simulation cometopause (red), bow shock standoff (blue) distances, and the extent of the diamagnetic cavity boundary observations(green) of Rosetta up to July 2015 (Goetz et al. 2016) are shown by the shaded areas for reference. Four regions of the environment are numbered in the panels. 1: gradual mass-loading and some draping (panels A–C), 2: a sharp shock-like structure (A–C), 3: magnetic field pile-up approaching the nucleus (B and C), and 4: draping of the magnetic field lines around the inner coma (B).

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.