Variations of auroral hydrogen emission near substorm onset

Borovkov, L. P.; Kozelov, B. V.; Yevlashin, L. S.; Chernouss, S. A.

doi:10.5194/angeo-23-1623-2005

Cited by 7 publications

(9 citation statements)

References 42 publications

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“…The blue-shifted wing of the Doppler profile was found to vary with magnetic local time (MLT), with narrower spectra and smaller mean Doppler shifts found on the dayside than the nightside. Its interpretation as proportional to the line of sight-integrated H + /H energy spectrum supports the notion that lower energy proton precipitation can be found near the dayside cusp [e.g., Derblom, 1975;, and higher energy proton precipitation is found in the evening and on the nightside [e.g., Borovkov et al, 2005]. Figure 10 illustrates the variation of the Doppler profile in H between the night-and dayside.…”

Section: Proton Aurorasupporting

confidence: 61%

Absolute calibration of optical devices with a small field of view

Sigernes¹,

Holmes²,

Dyrland³

et al. 2007

J. Opt. Technol.

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I would like to give thanks to those who I have learned a tremendous amount over the last years: my advisors Professor Dag Lorentzen and Professor Fred Sigernes. I feel very privileged to be able to refine my experimental techniques and learn the finer points of dayside aurora from both of them. From my first arctic lesson with Fred, to my first polar bear encounter with Dag, my education on Svalbard has been quite diverse. I also feel quite honoured to be a part of the team of scientists, both from The University Centre in Svalbard (UNIS) and our collaborating international institutions, that worked at the close of historic Nordlysstasjonen (The Auroral Station) in Adventdalen and the opening of the Kjell Henriksen Observatory (KHO). Special thanks also go to my mentors and collaborators Dr. Boris Kozelov, Professor Charles Deehr, and Dr. Magnar Gullikstad Johnsen who have helped me tremendously. Thanks also to Mr. Matteo Ottaviani, who played a major role in the deployment of the Black spectrometer to Ny-Ålesund, which provided essential data. I would also like to acknowledge Professor Jøran Moen for being my advisor at the University of Oslo. Thanks also to Espen Trondsen for helping me in lots of different ways. I would like to recognize and the life and work of the late Nikita Shumilov, my predecessor. I was fortunate to briefly collaborate with Nikita while living in London, but never had the privilege of meeting him in person. Extra special thanks must go to my fellow station/observatory co-manager, Dr. Margit Dyrland. She was a great partner in managing the old station and the new observatory. Each of us probably could have managed it alone, but together our differing skills complemented each other quite well! I would like to acknowledge and say thanks for the opportunities given to me by both

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Section: Proton Aurorasupporting

confidence: 61%

Absolute calibration of optical devices with a small field of view

Sigernes¹,

Holmes²,

Dyrland³

et al. 2007

J. Opt. Technol.

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“…Typical values for auroral blue‐line emission during pulsating aurora are of the order of a few hundred R to kR [ Royrvik and Davis , ]. This is much less than during the active phases of substorms, when the intensity may exceed 10 kR at 427.8 nm [ Borovkov et al , ]. CNA values typically exceed 0.5 dB during energetic particle precipitation and may occasionally reach values as high as 10 dB.…”

Section: Resultsmentioning

confidence: 99%

Observation of pulsating aurora signatures in cosmic noise absorption data

Grandin

Kero

Partamies

et al. 2017

Geophysical Research Letters

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This study investigates the contribution of energetic (E > 30 keV) particle precipitation during a pulsating aurora event over Kilpisjärvi (L = 6.2) on 26 February 2014. It is based on the comparison of auroral blue‐line emission (427.8 nm) data from an all‐sky camera and cosmic noise absorption (CNA) data obtained from a multibeam experiment of the Kilpisjärvi Atmospheric Imaging Receiver Array (KAIRA) riometer. The data sets are compared for three KAIRA beams close to magnetic zenith. Results show a clear correlation between the measured CNA and the auroral blue‐line emission during the event, for each beam. In addition, individual pulsations are observed for the first time in the cosmic noise absorption data measured by KAIRA and are found to be close‐to‐identical to the optical pulsations. This suggests that the modulation of electron precipitation during pulsating aurora takes place in a consistent way over a broad range of energies.

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“…Because of scattered sunlight approaching local noon, the H β profiles obtained were superimposed on a background containing significant Fraunhofer absorption near the H β rest wavelength. Although methods currently exist to account for this twilight component of the background (Robertson et al, 2006;Borovkov et al, 2005), the profiles were not chosen for analysis. We investigate here the effects of the angular redistributions on the overall shape of the spectral lines.…”

Section: Esr and Optical Observationsmentioning

confidence: 99%

TRANS4: a new coupled electron/proton transport code – comparison to observations above Svalbard using ESR, DMSP and optical measurements

Simon¹,

Lilensten²,

Moen

et al. 2007

Ann. Geophys.

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Abstract. We present for the first time a numerical kinetic/fluid code for the ionosphere coupling proton and electron effects. It solves the fluid transport equations up to the eighth moment, and the kinetic equations for suprathermal particles. Its new feature is that for the latter, both electrons and protons are taken into account, while the preceding codes (TRANSCAR) only considered electrons. Thus it is now possible to compute in a single run the electron and ion densities due to proton precipitation. This code is successfully applied to a multi-instrumental data set recorded on 22 January 2004. We make use of measurements from the following set of instruments: the Defence Meteorological Satellite Program (DMSP) F-13 measures the precipitating particle fluxes, the EISCAT Svalbard Radar (ESR) measures the ionospheric parameters, the thermospheric oxygen lines are measured by an all-sky camera and the H α line is given by an Ebert-Fastie spectrometer located at Ny-Ålesund. We show that the code computes the H α spectral line profile with an excellent agreement with observations, providing some complementary information on the physical state of the atmosphere. We also show the relative effects of protons and electrons as to the electron densities. Computed electron densities are finally compared to the direct ESR measurements.

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Variations of auroral hydrogen emission near substorm onset

Cited by 7 publications

References 42 publications

Absolute calibration of optical devices with a small field of view

Absolute calibration of optical devices with a small field of view

Observation of pulsating aurora signatures in cosmic noise absorption data

TRANS4: a new coupled electron/proton transport code – comparison to observations above Svalbard using ESR, DMSP and optical measurements

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