2003
DOI: 10.5194/angeo-21-2165-2003
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Remote sensing of the proton aurora characteristics from IMAGE-FUV

Abstract: Abstract. The combination of simultaneous global images of the north polar region obtained with the IMAGE-FUV imaging system makes it possible to globally map the properties of the electron and proton auroral precipitation. The SI12 imager, which observes the Doppler-shifted Lyman-α emission, provides a global snapshot of the proton aurora every 2 min. These images may be combined with those from the Wide-band Imaging Camera (WIC), to remotely characterize the proton precipitation in proton-dominated auroral s… Show more

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Cited by 9 publications
(7 citation 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%
“…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%
“…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%
“…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%