Auroral all-sky camera calibration

Sigernes, F.; Holmen, S. E.; Biles, Drummond; Björklund, Henrik; Chen, X.; Dyrland, M. E.; Lorentzen, D. A.; Baddeley, Lisa; Trondsen, T.; Brändström, Urban; Trøndsen, Espen; Lybekk, B.; Moen, J.; Chernouss, S. A.; Deehr, C. S.

doi:10.5194/gi-3-241-2014

Cited by 10 publications

(4 citation statements)

References 7 publications

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“…We present Wind IMF (Ogilvie et al, 1995) and solar wind plasma (Lin et al, 1995) observations with cadences of 0.092 and 6–12 s, respectively. Lastly, we present ASC observations with 3 s cadences from the Kjell Henricksen observatory in Longyearbyen, Svalbard, Norway (Sigernes et al, 2014, 2017).…”

Section: Observationsmentioning

confidence: 99%

Dayside Auroral Observation Resulting From a Rapid Localized Compression of the Earth's Magnetic Field

Briggs

Fasel

Silveira

et al. 2020

Geophysical Research Letters

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This paper presents observations of dayside auroral signatures resulting from a massive localized compression of the magnetopause, magnetosheath, and bow shock. On 10 December 2016, the Magnetospheric Multiscale Mission (MMS) spacecraft observed a compression of the entire magnetosheath and bow shock, which moved past the spacecraft in 1 min and 45 s. Shortly afterward, the resulting auroral signature was observed at the Kjell Henriksen Observatory located in Longyearbyen, Norway. The characteristics of this unique event have major ramifications for understanding dayside magnetospheric physics. Plain Language Summary The aurora borealis and australis are the visible signatures of interactions between the Earth's magnetic field and the solar wind. When the solar wind's magnetic field interacts with the Earth's magnetic field, there can be large fluctuations in its positioning and shape. This paper presents observations from satellites of a very large compression of the magnetic field, resulting in unique ionospheric signatures directly over an all-sky camera at Kjell Henricksen Observatory in Svalbard, Norway. One minute and 57 s after the compression at the magnetosphere, previously unstructured aurora began to intensify and organize, first propagating eastward and then brightening westward. The auroral arcs then began to spiral in a counterclockwise direction forming a spiral structure over the field of view. This defined shape only lasted for a few seconds before dispersing and moving poleward. The characteristics of this unique event have major ramifications for understanding dayside magnetospheric physics.

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Section: Observationsmentioning

confidence: 99%

Dayside Auroral Observation Resulting From a Rapid Localized Compression of the Earth's Magnetic Field

Briggs

Fasel

Silveira

et al. 2020

Geophysical Research Letters

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“…Among the means of direct ground-based observation of auroras, all-sky cameras due to their availability have become widespread [Lebedinsky, 1961;Sigernes et al, 2014]. However, the effectiveness of such observations strongly depends on environmental conditions (illumination of the sky, cloud cover, fog, etc.)…”

Section: Introductionmentioning

confidence: 99%

Local diagnostics of aurora presence based on intelligent analysis of geomagnetic data

Vorobev,

Soloviev,

Pilipenko

et al. 2023

Solar-Terrestrial Physics

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Despite the existing variety of approaches to monitoring space weather and geophysical parameters in the auroral oval region, the issue of effective prediction and diagnostics of auroras as a special state of the upper ionosphere at high latitudes remains virtually unresolved. In this paper, we explore the possibility of local diagnostics of auroras through mining of geomagnetic data from ground-based sources. We assess the significance of indicative variables and their statistical relationship. So, for example, the application of Bayesian inference to the data from the Lovozero geophysical station for 2012–2020 has shown that the dependence of a posteriori probability of observing auroras in the optical range on the state of geomagnetic parameters is logarithmic, and the degree of its significance is inversely proportional to the discrepancy between empirical data and approximating function. The accuracy of the approach to diagnostics of aurora presence based on the random forest method is at least 86 % when using several local predictors and ~80 % when using several global geomagnetic activity indices characterizing the geomagnetic field disturbance in the auroral zone. In conclusion, we discuss promising ways to improve the quality metrics of diagnostic models and their scope.

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“…The most frequent use of all-sky cameras is cloud cover detection (e.g. Tapakis and Charalambides, 2013, and references therein), but they have also been used for more complex purposes like solar irradiance forecasting (Alonso-Montesinos et al, 2015;Barbieri et al, 2017), to derive sky radiance and luminance measurements (Román et al, 2012;Tohsing et al, 2013), to retrieve aerosol properties (Cazorla et al, 2008;Román et al, 2017a), and to monitor aurora and airglow (Sigernes et al, 2014), among others. All-sky cameras are in general less accurate than well-calibrated photometers, but they are capable of obtaining a full map of the hemispherical sky radiance in a short time (a few seconds or less).…”

Section: Introductionmentioning

confidence: 99%

Relative sky radiance from multi-exposure all-sky camera images

et al. 2021

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Abstract. All-sky cameras are frequently used to detect cloud cover; however, this work explores the use of these instruments for the more complex purpose of extracting relative sky radiances. An all-sky camera (SONA202-NF model) with three colour filters narrower than usual for this kind of cameras is configured to capture raw images at seven exposure times. A detailed camera characterization of the black level, readout noise, hot pixels and linear response is carried out. A methodology is proposed to obtain a linear high dynamic range (HDR) image and its uncertainty, which represents the relative sky radiance (in arbitrary units) maps at three effective wavelengths. The relative sky radiances are extracted from these maps and normalized by dividing every radiance of one channel by the sum of all radiances at this channel. Then, the normalized radiances are compared with the sky radiance measured at different sky points by a sun and sky photometer belonging to the Aerosol Robotic Network (AERONET). The camera radiances correlate with photometer ones except for scattering angles below 10∘, which is probably due to some light reflections on the fisheye lens and camera dome. Camera and photometer wavelengths are not coincident; hence, camera radiances are also compared with sky radiances simulated by a radiative transfer model at the same camera effective wavelengths. This comparison reveals an uncertainty on the normalized camera radiances of about 3.3 %, 4.3 % and 5.3 % for 467, 536 and 605 nm, respectively, if specific quality criteria are applied.

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Auroral all-sky camera calibration

Cited by 10 publications

References 7 publications

Dayside Auroral Observation Resulting From a Rapid Localized Compression of the Earth's Magnetic Field

Dayside Auroral Observation Resulting From a Rapid Localized Compression of the Earth's Magnetic Field

Local diagnostics of aurora presence based on intelligent analysis of geomagnetic data

Relative sky radiance from multi-exposure all-sky camera images

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