Playing with apparently brief (20 minute) time durations between the dynamic pressure measures, i implicitly assume that the alterations in the magnetopause reputation mainly originate from the changes on solar wind stress and you will distinctions of the dayside community-aimed Part 1 currents. Although the magnetotail current may have a slightly larger effect day, but in general they only intensifies the end result of your Area step one most recent. grams., certain estimations were made when you look at the Samso ); yet not, (1) the fresh noncoupled MHD design hence show was in fact presented over do perhaps not duplicate the brand new band latest and you will (2) the period of one’s band current intensification is normally even more than the step 3–cuatro time included in these types of simulations. We work of one’s combined designs below that is qualitatively just as the outcome of the newest noncoupled model, so this does not change our very own findings.
Ultimately, we should examine several runs to verify our results are design-independent. Desk step one collects the benefit legislation indices N in the (1) computed of six items from around three around the world MHD models. The first is new noncoupled SWMF model whoever abilities have been exhibited above. As well as the basic runs (Adaptation step one), i simulated about three other models of one’s an equivalent noncoupled model, one or two having increased ionospheric conductivity and one that have a good dipole tilt. Brand new height-included Pedersen conductivity is thought as equal to 5 S in all the items, except versions 2 and you can step three in which the fresh included conductivity was ten and you may 100 S respectively. Inside version cuatro, we simulated the latest magnetosphere having an excellent dipole tip 31° . Changes in N ranging from Systems 1 and you may dos and you can Versions step one and you will cuatro try brief, and you may ranging from Items 1 and step three try reasonable, however, only for the southward IMF. Keep in mind that the brand new ionospheric conductivity a hundred S may be very large and you can are going to be scarcely noticed in reality. I profile iraniansinglesconnection reveal it in order to show this new role from conductivity as the the 2 moments boost in conductivity in Type 2 transform N simply for the brand new acceleration raise having southward IMF.
An increase in the new magnetotail current also boost in the Area step 1 currents weakens brand new magnetospheric magnetized job and movements brand new dayside magnetopause earthward
Variation 5 stands for operates of your own SWMF model coupled with complete interior-magnetosphere ionosphere, and Adaptation 6 is the LFM-Combine design. Each type, we generate four runs with the northward/southward IMF and for the occurrence and acceleration develops since the said significantly more than (24 works overall). Keep in mind one Letter=six in the ideal theoretic instance whether your magnetopause position match pressure harmony involving the solar breeze dynamic tension and the Planet’s dipole community and you will N=six.6 regarding empirical Shue mais aussi al. ( 1998 ) design. In fact, all of the obtained N are ranging from both of these beliefs otherwise a bit faster. Four off six types expect Letter large otherwise comparable to seven from the operates on thickness increase to own southward IMF. Even if Version 5 predicts N smaller compared to seven, N is actually methodically high in this situation per model.
Meanwhile, Tsyganenko and you can Sibeck ( 1994 ) listed the cross-tail current plus in a shorter education brand new ring current as well as the location 1 currents influence the brand new magnetized career on the magnetospheric area of the magnetopause
In addition to the comparison of different models, we investigate the influence of grid resolution on our results. We have calculated two runs for the same southward IMF with density and velocity changes using the noncoupled SWMF model with the 1/16 RE grid spacing around the subsolar magnetopause. We obtain different power laws, N=6.712 and 6.132, in the density and velocity runs, respectively (instead of 7.80 and 6.69 for the same model with a low resolution). Moreover, the normalized (to the solar wind electric field) reconnection rates in the low-resolution runs are smaller than those in the high-resolution runs (but are about the same in the density and velocity runs for the same resolution). We also find some differences in the CPCP and the magnetic field magnitude at geosynchronous orbit. We note that the grid resolution influences the magnitude of maximal electric current density at the magnetopause and possibly may change the total magnetopause current, but this problem requires more careful studies and it stays outside of the scope of the paper.