Sentence examples for magnetic onset from inspiring English sources

The imager at RANK detected a brightening near the southern horizon at the time of magnetic onset (5 33 UT) and rapidly poleward moving auroras, approaching the northern horizon at approximately 6 UT, and subsequently retreating equatorward to be followed by auroral activity.

Taking into account the permanently high level of auroral activity and inconsistency of aurora behavior and magnetic onsets during sawtooth substorms, the conclusion is made that auroral ionosphere conductivity is typically high and ensures an extremely high intensity of field-aligned currents in R1 FAC system.

Because Pi2 disturbances often precede the magnetic dipolarization onset in the plasma sheet as well as the substorm auroral expansion onset in the ionosphere, we investigate the correlation between the Pi2 disturbances in the near-Earth plasma sheet and the corresponding substorm wave-like arcs in the ionosphere around the substorm onset time.

The relative error of the magnetic disturbance onset time (δTT=7.4%) is less than 10% for 50% of all the events and less than 20% for 70% of all the events.

The relationships between the magnetic disturbance onsets, aurora dynamics and particles injections at the geostationary orbit have been analyzed in detail for 25 sawtooth substorms.

The distinguishing feature of the aurora in case of saw-tooth substorms is permanently high level of auroral activity irrespective of the magnetic disturbance onsets and the double oval structure of the aurora display.

In many substorm events, Pi2 disturbances appear prior to the magnetic field dipolarization onset in the plasma sheet and Pi1 disturbances are commonly observed at or after the substorm onset (e.g., Takahashi et al. 1987, Roux et al. 1991; Cheng and Lui 1998; Shiokawa et al. 2005).

The azimuthal propagation speed of the substorm expansion at geosynchronous orbit (L = 6.6 RE) was derived from the time difference between the magnetic field dipolarization onset observed by the GOES 8 and 9 satellites and the auroral breakup observed by the Polar ultraviolet imager (Liou et al. 2002).

Given that accretion times are on the order of 10 Myr (Brasser 2013), the scaling places the inner core's (and thus its magnetic field's) onset time before accretion's end and requires inner core growth during accretion and during growth of the core itself.

They found that dynamically important magnetic fields delay the onset of fragmentation by an order of magnitude compared to the case where no magnetic field is present.

Also the onset of magnetic variations trailed the onset of the flows by 20 s for D and by 1 min 25 s for E. These facts indicate that the actual time difference between equatorial flow and field onsets and the auroral onset depends on the location of the spacecraft and our ability to define precise onset times.