Contributions of imaging Echelle spectrographs to daytime optical aeronomy

Pallamraju, Duggirala; Chakrabarti, Supriya

doi:10.1016/j.jastp.2005.05.013

Cited by 12 publications

(5 citation statements)

References 63 publications

(76 reference statements)

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“…Thus, it is believed that the photoelectron flux variation due to solar flare through the PE impact mechanism is mainly responsible for the observed OI dayglow emission rate. This event is strikingly in contrast to the several optical daytime redline emission investigations wherein the small-scale variations have all been attributed to the variations in the electron densities (through the DR mechanism) [e.g., Sridharan et al, 1994;Pallamraju et al, 2001Pallamraju et al, , 2004Pallamraju et al, , 2010Chakrabarty et al, 2004;Pallamraju and Chakrabarti, 2006].…”

Section: Discussioncontrasting

confidence: 67%

Effect of an X‐Class solar flare on the OI 630 nm dayglow emissions

2010

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[1] We present a striking event that shows a prompt effect of an X-class solar flare (X6.2/3B) in the neutral optical dayglow emissions. This flare occurred on 13 December 2001 at 1424 UT and peaked at 1430 UT. The peak-to pre-flare X-ray intensity ratio as observed by GOES-10 was greater than 300 and the EUV flux observed by SEM/SOHO was greater by around 60%. As a response to this flare, the daytime redline (OI 630 nm) column integrated emission intensity measured from Carmen Alto (23.16°S, 70.66°W), in Chile, showed a prompt increase of around 50%. Our results show that this prompt enhancement in the thermospheric dayglow seems to be caused mainly due to an increase in photoelectrons due to a sudden increase in the solar EUV flux associated with this flare.

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Section: Discussioncontrasting

confidence: 67%

Effect of an X‐Class solar flare on the OI 630 nm dayglow emissions

2010

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“…The High Resolution Doppler Imager (HRDI) on the Upper Atmosphere Research Satellite [ Hays et al , 1993] had this capability and a ground‐based version could certainly detect this emission, if a burst occurred within its field of view. Daytime aurora has also been detected from the ground using an echelle grating instrument [ Pallamraju and Chakrabarti , 2006]. Alternatively, a simple device, even an imager, could be flown on a high‐altitude balloon.…”

Section: Discussionmentioning

confidence: 99%

Summer high‐latitude mesospheric observations of supersonic bursts and O(¹S) emission rate with the UARS WINDII instrument and the association with sprites, meteors, and lightning

Lee

Shepherd

2010

J. Geophys. Res.

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[1] Supersonic neutral velocities, called supersonic bursts, are observed in localized regions lasting for over 8 s of enhanced O( 1 S) emission rate for tangent altitudes of 73-80 km during summer daytime by the Wind Imaging Interferometer (WINDII) on board the UARS satellite; the occurrence rate is 40% (≥500 m s −1 ) for latitudes above 65°N. These bursts are proposed to be produced by accelerated electrons and ions in a strong electric field. Theory suggests that an electric field of 45 V m −1 is required to generate a typical supersonic velocity of 750 m s −1 forced by ion-neutral collisions at 82 km, the altitude at which polar mesospheric clouds occur. Coincidences in space and time between supersonic velocity profiles and space-based lightning detection observed at a wavelength of 777.4 nm were found in a limited number of cases in high-latitude summer, a region for which the lightning detection has the highest occurrence frequency (2-3.5%) and optical energy (1 J m −2 sr −1 mm −1 ) as a function of month and latitude. The electric field must have sufficient energy to generate atomic emission features, more than for sprites and comparable with tropospheric lightning. Support for the existence of supersonic bursts at high latitude is provided through the observation of "chirps" in infrasound emissions which frequently occur in the absence of tropospheric lightning.Citation: Lee, Y.-S., and G. G. Shepherd (2010), Summer high-latitude mesospheric observations of supersonic bursts and O( 1 S) emission rate with the UARS WINDII instrument and the association with sprites, meteors, and lightning, J. Geophys. Res., 115, A00E26,

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“…Their difference obtained in the wavelength region of interest yields information on the dayglow emission and scattering (Ring effect contributions). The details of measurement technique, removal of the Ring effect, and a review of results obtained by this technique have been reported earlier [ Pallamraju et al , 2000, 2002, 2004, 2010; Pallamraju and Chakrabarti , 2006].…”

Section: Data Descriptionmentioning

confidence: 99%

On deriving incident auroral particle fluxes in the daytime using combined ground-based optical and radar measurements

2011

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[1] Particle energies and fluxes have predominantly been measured from instruments onboard satellites. In this study, we use daytime ground-based oxygen redline emission measurements, along with the ionospheric electron density, and electron temperature profiles measured from the incoherent scatter radar, and a physics-based modeling approach to derive the energy and flux of particles incident over Boston during the storm of 30 October 2003. We find that the characteristic energy and the associated flux vary between 0.07-5.7 keV and 0.5-130 mW m −2 , respectively, during the intense magnetic disturbance that brought aurora to midlatitudes. Such an approach not only offers another method to estimate the incident particle energies and fluxes but also enhances our understanding on the channels of energy deposition in the upper atmospheric region, especially during magnetic disturbances, about which database is poor.Citation: Pallamraju, D., S. Chakrabarti, and S. C. Solomon (2011), On deriving incident auroral particle fluxes in the daytime using combined ground-based optical and radar measurements,

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Contributions of imaging Echelle spectrographs to daytime optical aeronomy

Cited by 12 publications

References 63 publications

Effect of an X‐Class solar flare on the OI 630 nm dayglow emissions

Effect of an X‐Class solar flare on the OI 630 nm dayglow emissions

Summer high‐latitude mesospheric observations of supersonic bursts and O(¹S) emission rate with the UARS WINDII instrument and the association with sprites, meteors, and lightning

On deriving incident auroral particle fluxes in the daytime using combined ground-based optical and radar measurements

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Contributions of imaging Echelle spectrographs to daytime optical aeronomy

Cited by 12 publications

References 63 publications

Effect of an X‐Class solar flare on the OI 630 nm dayglow emissions

Effect of an X‐Class solar flare on the OI 630 nm dayglow emissions

Summer high‐latitude mesospheric observations of supersonic bursts and O(1S) emission rate with the UARS WINDII instrument and the association with sprites, meteors, and lightning

On deriving incident auroral particle fluxes in the daytime using combined ground-based optical and radar measurements

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Summer high‐latitude mesospheric observations of supersonic bursts and O(¹S) emission rate with the UARS WINDII instrument and the association with sprites, meteors, and lightning