Remote sensing of the proton aurora characteristics from IMAGE-FUV

Бисикало, Д. В.; Shematovich, V. I.; Gérard, Jean‐Claude; Meurant, M.; Mende, S. B.; Frey, H. U.

doi:10.5194/angeo-21-2165-2003

Cited by 9 publications

(7 citation statements)

References 36 publications

(46 reference statements)

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“…The proton flux so derived is also used to remove the proton contribution from the WIC and the SI13 images. This method was validated by comparisons with in situ measurements of the auroral particle energy flux obtained from the FAST [ Frey et al , 2001; Bisikalo et al , 2003], NOAA [ Hubert et al , 2002; Coumans et al , 2002; Meurant et al , 2003], and DMSP [ Bisikalo et al , 2003; Coumans et al , 2004] satellites.…”

Section: Discussionmentioning

confidence: 99%

Morphology and seasonal variations of global auroral proton precipitation observed by IMAGE‐FUV

et al. 2004

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[1] Observations with the FUV imagers on board the IMAGE satellite have been used to map the auroral electron and proton energy fluxes during the summer and winter solstices of 2000, in order to construct a statistical view of the global auroral proton precipitation. The distribution for electrons compare well both in morphology and in magnitude with those obtained previously with the Polar-UVI instruments and with an empirical auroral precipitation model based on DMSP data. The proton morphology also closely resembles the statistical ion oval derived from DMSP data, showing a ''C-shaped'' morphology with a minimum located in the morning sector. The precipitation proton auroral power is on the order of 2.2 GW for an average Kp value of 2, also in close agreement with the values of the DMSP empirical model. The FUV data also reveal the presence of seasonal effects in the proton precipitation. Specifically, the latitudinal width of the proton oval is larger in summer than in winter so that the globally precipitated proton power is 1.5 times higher in summer than in winter. The occurrence probability of intense proton auroras (with energy flux >0.5 mW m À2 ) is also shown to be nearly three times higher in summer than in winter. This seasonal effect in the proton precipitation contrasts with those observed for electrons, where intense electron events occur more often in winter than in summer. We discuss a mechanism that may account for these results based on the presence of field-aligned potential drops which accelerate auroral electrons downward in regions of upward directed field-aligned current, while suppressing the precipitating magnetospheric proton flux. The presence of such field-aligned potentials is dependent on the differing solar illumination in winter and summer.

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Section: Discussionmentioning

confidence: 99%

Morphology and seasonal variations of global auroral proton precipitation observed by IMAGE‐FUV

et al. 2004

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“…Combining the images of the proton and electron aurora allowed for a comparison of the brightness with expected values [ Hubert et al , 2001]. The in situ particle measurements provided enough high‐energy proton flux to completely account for the electron aurora signal without the need for additional electron precipitation [ Bisikalo et al , 2003].…”

Section: Localized Auroramentioning

confidence: 99%

Localized aurora beyond the auroral oval

Frey

2007

Reviews of Geophysics

109

113

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Aurora is the result of the interaction between precipitating energetic electrons and protons with the upper atmosphere. Viewed from space, it generally occurs in continuous and diffuse ovals of light around the geomagnetic poles. Additionally, there are localized regions of aurora that are unrelated to the ovals and exhibit different morphological, spatial, and temporal properties. Some of these localized aurorae are detached from the oval poleward or equatorward of it. Others are located within the oval and are brighter than the surrounding diffuse aurora. Many of them occur only during preferred solar wind conditions and orientations of the interplanetary magnetic field. This review describes the different localized aurorae and their particle sources in the plasma sheet, at the plasmapause, or at the magnetopause. Their origin is still not completely understood, and the study of aurorae can teach a great deal about their underlying physical processes of reconnection, electrostatic acceleration, or wave‐particle interactions.

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“…The halflength of the magnetic field line for L = 6.5 is %50,000 km. Supposing the pulsating auroras studied here are caused by protons with energies 10-30 keV [Galand et al, 2002;Bisikalo et al, 2003], we can evaluate their travel time as 35-20 s. For electrons, this time is considerably less.…”

Section: Discussionmentioning

confidence: 99%

Pc1–2 auroral pulsations

Roldugin

Pilgaev

2013

JGR Space Physics

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[1] By observations at Lovozero station (64.3 N, 114.3 E CGM coordinates), we have investigated two events of auroral pulsations of Pc1-2 type with periods in the range 2.5-7 s accompanied by similar geomagnetic pulsations. Luminous variations in different parts of the sky were found by photometric measurements of the frames of all-sky camera, which was operated at the rate of one frame per second. The pulsations under study are associated with the diffuse aurora. For the event with 7 s period, a phase relationship between auroral and magnetic pulsations is as follows: the luminosity bursts are coincident with positive half periods in the Z component and negative ones in the D component, while positive peaks in the H component lag behind the luminous peaks by about p/2. For the event with 2.5 s period, this relationship appears different. Within one of 10-min intervals, Pc2 pulsations observed in both magnetic field and aurora were superposed by regular Pc4 pulsations of 1-min period. For these, the luminosity bursts corresponded to negative half periods in the Z component. A connection between auroral and magnetic pulsations is discussed.

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Remote sensing of the proton aurora characteristics from IMAGE-FUV

Cited by 9 publications

References 36 publications

Morphology and seasonal variations of global auroral proton precipitation observed by IMAGE‐FUV

Morphology and seasonal variations of global auroral proton precipitation observed by IMAGE‐FUV

Localized aurora beyond the auroral oval

Pc1–2 auroral pulsations

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