Midlatitude auroras in the south of Eastern Siberia during strong geomagnetic storms on October 29?31, 2003 and November 20?21, 2003

Михалев, А. В.; Beletsky, Aleksandr; Kostyleva, N. V.; Chernigovskaya, M.A.

doi:10.1007/s10604-005-0006-8

Cited by 20 publications

(7 citation statements)

References 6 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Great auroras have “high visual brightness with a progression to exceptionally low latitudes” [ Jones , 1992]. An examination of the catalog of great aurora events of Jones [1992], supplemented by Yevlashin [2000], Pallamraju and Chakrabarti [2005], and Mikhalev et al [2004], finds that the great aurora chiefly occur during solar maximum. A display of the solar cycle dependence of great aurora is shown in Figure 14, where the sunspot number is plotted as a function of time and the reported occurrences of great aurora are indicated by the circles.…”

Section: Differencesmentioning

confidence: 99%

Differences between CME‐driven storms and CIR‐driven storms

2006

View full text Add to dashboard Cite

[1] Twenty one differences between CME-driven geomagnetic storms and CIR-driven geomagnetic storms are tabulated. (CME-driven includes driving by CME sheaths, by magnetic clouds, and by ejecta; CIR-driven includes driving by the associated recurring high-speed streams.) These differences involve the bow shock, the magnetosheath, the radiation belts, the ring current, the aurora, the Earth's plasma sheet, magnetospheric convection, ULF pulsations, spacecraft charging in the magnetosphere, and the saturation of the polar cap potential. CME-driven storms are brief, have denser plasma sheets, have strong ring currents and Dst, have solar energetic particle events, and can produce great auroras and dangerous geomagnetically induced currents; CIR-driven storms are of longer duration, have hotter plasmas and stronger spacecraft charging, and produce high fluxes of relativistic electrons. Further, the magnetosphere is more likely to be preconditioned with dense plasmas prior to CIR-driven storms than it is prior to CME-driven storms. CME-driven storms pose more of a problem for Earth-based electrical systems; CIR-driven storms pose more of a problem for space-based assets.Citation: Borovsky, J. E., and M. H. Denton (2006), Differences between CME-driven storms and CIR-driven storms,

show abstract

Section: Differencesmentioning

confidence: 99%

Differences between CME‐driven storms and CIR‐driven storms

2006

View full text Add to dashboard Cite

show abstract

“…The description of the analyzed events from the ground-based and satellite geomagnetic and optical observations is presented in a number of papers [Huttunen et al, 2002;Mishin et al, 2010;Mikhalev et al, 2004;Ebihara et al, 2005;Hairston et al, 2005;Hori et al, 2006;Mishin et al, 2007;Solovyev et al, 2008;Karavaev et al, 2009;Valladares et al, 2015;Mishin et al, 2016;Mishin, Karavaev, 2017;Mishin et al, 2018].…”

Section: Databasementioning

confidence: 99%

“…When studying the main objects of space weather and of geodynamics -magnetospheric substorms and storms -one observes geomagnetic pulsations of various types, as well as auroras with the intensity exceeding 100 kR. These events are accompanied by an increase in electric fields and currents in the ionosphere of the auroral zone that, during superstorms (sometimes observed strongest storms), can spread to the mid latitudes [Troitskaya, Gul'elmi, 1967;Pudovkin et al, 1976;Tinsley et al, 1986;Brunelli, 1988;Rassoul et al, 1993;Kangas et al, 1998;Mikhalev et al, 2004;Zverev et al, 2012;Leonovich et al, 2013;Li, Wang, 2018]. During the 2003 Nov 20 storm (one of the strongest), from the mid-latitude geophysical observatories located near Irkutsk (CGM: 47.3° Ф, 177° Λ) in the post-midnight MLT sector, there recorded shortperiod Pi1B/Pi1С pulsations, and disturbances of optical emissions in the 557.7 nm and 630.0 nm atomic oxygen [OI] lines, as well as in 391.4 nm ionized nitrogen molecular band, with record-breaking intensity values [Mishin et al, 2018].…”

Section: Introductionmentioning

confidence: 99%

Dynamics for geomagnetic pulsations, field-aligned currents, and airglow at mid-latitudes within substorm activations during superstorms

Клибанова

Мишин

Михалёв

et al. 2019

Geodin. tektonofiz.

Self Cite

View full text Add to dashboard Cite

Within substorm activations during two superstorms (2000 and 2003) from the observations at midlatitude geomagnetic observatories, we study short-period irregular geomagnetic pulsations and airglow in the 557.7 nm and 630.0 nm atomic oxygen emission lines, and in the 391.4 nm ionized nitrogen molecular band. Through the genuine magnetogram inversion technique, from the 1-minute data of the ground-based magnetometer global network, we investigate the distribution dynamics for field-aligned currents (FACs) in the ionosphere. The relation is shown between pulsation bursts and airglow disturbances in the post-midnight sector to precipitations of energetic electrons (~keV) and increase in the R2 upward FACs.

show abstract

“…Yet 557.7 and 630.0 nm emissions of atomic oxygen [OI] being the brightest discrete lines both in polar aurorae and in airglow occur respectively in different color channels G and R and are situated in regions with maximum spectral sensitivity of these channels. At middle latitudes, intensities of these emissions during some geophysical phenomena, such as geomagnetic storms ([OI] 630 nm emission) and sudden winter stratospheric warmings ([OI] 557.7 nm emission) can increase by an order of magnitude or more [Mikhalev et al, 2001;Mikhalev et al, 2004]. This allows us to consider the possibility of quantitatively associating the increase in signals in the G and R channels with the increase in intensities of the discrete emissions at 557.7 and 630.0 nm for the above geophysical phenomena.…”

Section: Distribution Of Gns Components Over R G B Channels Of the mentioning

confidence: 99%

Night airglow in RGB mode

Михалев¹,

Подлесный²,

Podlesny³

et al. 2016

Solar-Terrestrial Physics

View full text Add to dashboard Cite

To study dynamics of the upper atmosphere, we consider results of the night sky photometry, using a color CCD camera and taking into account the night airglow and features of its spectral composition. We use night airglow observations for 2010–2015, which have been obtained at the ISTP SB RAS Geophysical Observatory (52° N, 103° E) by the camera with KODAK KAI-11002 CCD sensor. We estimate average brightness of the night sky in R, G, B channels of the color camera for eastern Siberia with typical values ranging from ~0.008 to 0.01 erg·cm–2·s–1. Besides, we determine seasonal variations in the night sky luminosities in R, G, B channels of the color camera. In these channels, luminosities decrease in spring, increase in autumn, and have a pronounced summer maximum, which can be explained by scattered light and is associated with the location of the Geophysical Observatory. We consider geophysical phenomena with their optical effects in R, G, B channels of the color camera. For some geophysical phenomena (geomagnetic storms, sudden stratospheric warmings), we demonstrate the possibility of quantitative relationship between enhanced signals in R and G channels and increases in intensities of discrete 557.7 and 630 nm emissions, which are predominant in the airglow spectrum.

show abstract

Midlatitude auroras in the south of Eastern Siberia during strong geomagnetic storms on October 29?31, 2003 and November 20?21, 2003

Cited by 20 publications

References 6 publications

Differences between CME‐driven storms and CIR‐driven storms

Differences between CME‐driven storms and CIR‐driven storms

Dynamics for geomagnetic pulsations, field-aligned currents, and airglow at mid-latitudes within substorm activations during superstorms

Night airglow in RGB mode

Contact Info

Product

Resources

About