scholarly journals Studying 630 nm atomic oxygen emission sources during strong magnetic storms in the night mid-latitude ionosphere

2019 ◽  
Vol 5 (2) ◽  
pp. 33-38
Author(s):  
Людмила Леонович ◽  
Lyudmila Leonovich ◽  
Анатолий Тащилин ◽  
Anatoliy Tashchilin ◽  
Сергей Лунюшкин ◽  
...  
Keyword(s):  
Magnetic Storm ◽  
Emission Intensity ◽  
Atomic Oxygen ◽  
Geomagnetic Storms ◽  
Energetic Electron ◽  
Magnetic Storms ◽  
Optical Measurements ◽  
Model Calculations ◽  
Good Agreement ◽  
Red Line

We analyze significant increases in 630 nm atomic oxygen night emissions during very strong geomagnetic storms, using optical measurements, theoretical modeling, and magnetogram inversion technique (MIT) data. It is shown that during strong magnetic storms when electron precipitation equatorial boundary at the night sector expands up to ~40°, the interaction of energetic electron flux with thermospheric components may cause extreme increases in the 630 nm emission intensity. Model calculations of the red line intensity show good agreement with observational data. Using the November 20, 2003 magnetic storm as an example, we have found that oxygen atom collisions with thermal Maxwell and superthermal electrons make a major contribution to the integral emission intensity. Thermospheric density variations during the magnetic storm significantly affect the red line generation.

scholarly journals Studying 630 nm atomic oxygen emission sources during strong magnetic storms in the night mid-latitude ionosphere

2019 ◽  
Vol 5 (2) ◽  
pp. 35-41
Author(s):  
Людмила Леонович ◽  
Lyudmila Leonovich ◽  
Анатолий Тащилин ◽  
Anatoliy Tashchilin ◽  
Сергей Лунюшкин ◽  
...  
Keyword(s):  
Magnetic Storm ◽  
Emission Intensity ◽  
Atomic Oxygen ◽  
Geomagnetic Storms ◽  
Energetic Electron ◽  
Magnetic Storms ◽  
Optical Measurements ◽  
Model Calculations ◽  
Good Agreement ◽  
Red Line

We analyze significant increases in 630 nm atomic oxygen night emissions during very strong geomagnetic storms, using optical measurements, theoretical modeling, and magnetogram inversion technique (MIT) data. It is shown that during strong magnetic storms when electron precipitation equatorial boundary at the night sector expands up to ~40°, the interaction of energetic electron flux with thermospheric components may cause extreme increases in the 630 nm emission intensity. Model calculations of the red line intensity show good agreement with observational data. Using the November 20, 2003 magnetic storm as an example, we have found that oxygen atom collisions with thermal Maxwell and superthermal electrons make a major contribution to the integral emission intensity. Thermospheric density variations during the magnetic storm significantly affect the red line generation.

The Energetic Electron Response to Magnetic Storms: HEO Satellite Observations

2004 ◽  
Author(s):  
J. F. Fennell ◽  
J. B. Blake ◽  
R. Friedel ◽  
S. Kanekal
Keyword(s):  
Energetic Electron ◽  
Magnetic Storms ◽  
Satellite Observations

scholarly journals Specific interplanetary conditions for CIR-, Sheath-, and ICME-induced geomagnetic storms obtained by double superposed epoch analysis

2010 ◽  
Vol 28 (12) ◽  
pp. 2177-2186 ◽  
Author(s):  
Yu. I. Yermolaev ◽  
N. S. Nikolaeva ◽  
I. G. Lodkina ◽  
M. Yu. Yermolaev
Keyword(s):  
Large Scale ◽  
Geomagnetic Storms ◽  
Magnetic Cloud ◽  
Magnetic Storms ◽  
Main Phase ◽  
Corotating Interaction Region ◽  
Superposed Epoch Analysis ◽  
Epoch Analysis ◽  
Archive Data ◽  
Scale Types

Abstract. A comparison of specific interplanetary conditions for 798 magnetic storms with Dst <−50 nT during 1976–2000 was made on the basis of the OMNI archive data. We categorized various large-scale types of solar wind as interplanetary drivers of storms: corotating interaction region (CIR), Sheath, interplanetary CME (ICME) including both magnetic cloud (MC) and Ejecta, separately MC and Ejecta, and "Indeterminate" type. The data processing was carried out by the method of double superposed epoch analysis which uses two reference times (onset of storm and minimum of Dst index) and makes a re-scaling of the main phase of the storm in a such way that all storms have equal durations of the main phase in the new time reference frame. This method reproduced some well-known results and allowed us to obtain some new results. Specifically, obtained results demonstrate that (1) in accordance with "output/input" criteria the highest efficiency in generation of magnetic storms is observed for Sheath and the lowest one for MC, and (2) there are significant differences in the properties of MC and Ejecta and in their efficiencies.

Measurements of the viscometric functions for a fluid in steady shear flows

1971 ◽  
Vol 270 (1208) ◽  
pp. 507-556 ◽  
Keyword(s):  
Normal Stress ◽  
Couette Flow ◽  
Direct Method ◽  
Normal Stress Difference ◽  
Optical Measurements ◽  
Measuring Error ◽  
Stress Difference ◽  
Concentric Cylinders ◽  
Plate Apparatus ◽  
Good Agreement

This paper describes a series of experiments in which the three material functions of steady viscometric flows were measured for a given polyisobutene solution. A number of instruments and measuring techniques were used in order to check the experimental method. The shear stress was determined from the torque transmitted by the fluid in a cone-and-plate apparatus and in Couette flow between concentric cylinders. The results obtained from these measurements were in good agreement with each other. The primary normal-stress difference was determined from the normal force acting on the plate of a cone-and-plate apparatus, and from stress-optical measurements on Couette flow between concentric cylinders. These results are in good agreement with each other. Detailed measurements of the distribution f Permanent address: Fluid Mechanics Research Institute, University of Essex, Colchester, Essex. of the normal stress acting on the plate of the cone-and-plate apparatus were made for three cone angles and for two boundary configurations at the rim of the apparatus: from these results a combination of the primary and the secondary normal-stress differences was deduced, thereby making possible the computation of the secondary normal-stress difference. When the normal stress acting on a rigid surface is measured by means of a hole leading to a pressure transducer the results are in error by an amount roughly proportional to the primary normal-stress difference of the fluid (cf. Kaye, Lodge & Vale 1968). In the present experiments this error was determined from measurements of the distribution of the normal stress acting on the plates of a plate-and-plate apparatus, together with the assumption that the error is a function only of the shear rate at the position o the hole in the undisturbed viscometric flow. The values of the measuring error thus obtained are in goo agreement with measurements made in Gouette flow between concentric cylinders. The secondary normal-stress difference, P2, was measured in a number of different ways. From the results it is suggested that the methods of Jackson & Kaye and of Marsh & Pearson may be imprecise and, in particular, may yield incorrect values for P2- A new, direct, method of estimating P2, suggested by Higashitani & Pritchard (1971) and outlined in appendix A, may provide a more convenient means of determining P2.

Plasmaspheric response to the geomagnetic storm period March 20–23, 1990, observed by the ACTIVNY (MAGION-2) satellite

1992 ◽  
Vol 70 (7) ◽  
pp. 569-574 ◽  
Author(s):  
M. Förster ◽  
N. Jakowski ◽  
A. Best ◽  
J. Smilauer
Keyword(s):  
Magnetic Storm ◽  
Electron Density ◽  
Geomagnetic Storm ◽  
Joule Heating ◽  
Growth Phase ◽  
Langmuir Probe ◽  
Atomic Oxygen ◽  
Scale Height ◽  
Ionospheric Response ◽  
Increased Pressure

Langmuir probe data obtained during the storm period March 20–23, 1990, on board the MAGION-2 subsatellite of the ACTIVNY experiment are analyzed to study the plasmaspheric and ionospheric response to a magnetic storm. The data indicate a well-pronounced equatorward edge of the electron density trough in the afternoon (18:15 LT) at about 800 km height that moves towards lower latitudes during the course of the storm. It is interesting to note that the electron density inside the plasmasphere is increased by more than 20% in the morning shortly after sunrise (07:30 LT). This is due to enhanced O+ densities in the lower plasmasphere during the growth phase of the geomagnetic storm as measured by the ion mass spectrometer NAM-5 onboard the main satellite. It is suggested that the source for the increased density is thermospheric Joule heating at auroral latitudes with a commensurate increase in thermospheric pressure. This increased pressure causes the local thermosphere to expand both upward and equatorward. The increased atomic-oxygen scale height coupled with equatorward motion of fhermospheric perturbations results in an increased O density and resulting O+ density within the lower plasmasphere. The observations indicate a storm-induced compression of the plasmasphere that favourizes an enhanced outflow of plasma into the ionosphere leading to an increased nighttime F2-layer ionization and a depletion of the plasmasphere during the following hours.

scholarly journals A great space weather event in February 1730

2018 ◽  
Vol 616 ◽  
pp. A177 ◽  
Author(s):  
Hisashi Hayakawa ◽  
Yusuke Ebihara ◽  
José M. Vaquero ◽  
Kentaro Hattori ◽  
Víctor M. S. Carrasco ◽  
...  
Keyword(s):  
Solar Activity ◽  
East Asia ◽  
Magnetic Storm ◽  
East Asian ◽  
Active Phase ◽  
Magnetic Storms ◽  
Historical Records ◽  
Maximum Phase ◽  
Weather Event ◽  
Space Weather Event

Aims. Historical records provide evidence of extreme magnetic storms with equatorward auroral extensions before the epoch of systematic magnetic observations. One significant magnetic storm occurred on February 15, 1730. We scale this magnetic storm with auroral extension and contextualise it based on contemporary solar activity. Methods. We examined historical records in East Asia and computed the magnetic latitude (MLAT) of observational sites to scale magnetic storms. We also compared them with auroral records in Southern Europe. We examined contemporary sunspot observations to reconstruct detailed solar activity between 1729 and 1731. Results. We show 29 auroral records in East Asian historical documents and 37 sunspot observations. Conclusions. These records show that the auroral displays were visible at least down to 25.8° MLAT throughout East Asia. In comparison with contemporary European records, we show that the boundary of the auroral display closest to the equator surpassed 45.1° MLAT and possibly came down to 31.5° MLAT in its maximum phase, with considerable brightness. Contemporary sunspot records show an active phase in the first half of 1730 during the declining phase of the solar cycle. This magnetic storm was at least as intense as the magnetic storm in 1989, but less intense than the Carrington event.

scholarly journals RELATIONSHIP OF THE ASY-H INDEX WITH INTERPLANETARY MEDIUM PARAMETERS AND AURORAL ACTIVITY IN MAGNETIC STORM MAIN PHASES DURING CIR AND ICME EVENTS

2020 ◽  
Vol 6 (1) ◽  
pp. 43-50
Author(s):  
Roman Boroev ◽  
Mikhail Vasiliev
Keyword(s):  
Magnetic Storm ◽  
Interplanetary Medium ◽  
Magnetic Storms ◽  
Main Phase ◽  
Storm Main Phase ◽  
H Index ◽  
Auroral Activity ◽  
Different Types ◽  
Relationship Of ◽  
The Relationship

In this study, we examine the relationship of the ASY-H index characterizing the partial ring current intensity with interplanetary medium parameters and auroral activity during the main phase of magnetic storms, induced by the solar wind (SW) of different types. Over the period 1979–2017, 107 magnetic storms driven by CIR and ICME (MC + Ejecta) events have been selected. We consider magnetic storms with Dstmin≤ – 50 nT. The average ASY-H index (ASYaver) during the magnetic storm main phase is shown to increase with increasing SW electric field and southward IMF Bz regardless of SW type. There is no relationship between ASYaver and SW velocity. For the CIR and ICME events, the average AE (AEaver) and Kp (Kp aver) indices have been found to correlate with ASYaver. The highest correlation coefficient between AEaver and ASYaver (r = 0.74) is observed for the magnetic storms generated by CIR events. A closer relationship between Kp aver and ASYaver (r = 0.64) is observed for the magnetic storms induced by ICME events. The ASYaver variations correlate with Dstmin. The relationship between ASYaver and the rate of storm development is weak.

scholarly journals Extremely intense (SML ≤–2500 nT) substorms: isolated events that are externally triggered?

2015 ◽  
Vol 33 (5) ◽  
pp. 519-524 ◽  
Author(s):  
B. T. Tsurutani ◽  
R. Hajra ◽  
E. Echer ◽  
J. W. Gjerloev
Keyword(s):  
Solar Wind ◽  
Magnetic Fields ◽  
Magnetic Storm ◽  
Solar Wind Plasma ◽  
Magnetic Storms ◽  
Input Energy ◽  
Stored Energy ◽  
Ionospheric Currents ◽  
Interplanetary Magnetic Fields ◽  
Very High

Abstract. We examine particularly intense substorms (SML &amp;leq;–2500 nT), hereafter called "supersubstorms" or SSS events, to identify their nature and their magnetic storm dependences. It is found that these intense substorms are typically isolated events and are only loosely related to magnetic storms. SSS events can occur during super (Dst &amp;leq;–250 nT) and intense (−100 nT &amp;geq; Dst >–250) magnetic storms. SSS events can also occur during nonstorm (Dst &amp;geq;–50 nT) intervals. SSSs are important because the strongest ionospheric currents will flow during these events, potentially causing power outages on Earth. Several SSS examples are shown. SSS events appear to be externally triggered by small regions of very high density (~30 to 50 cm−3) solar wind plasma parcels (PPs) impinging upon the magnetosphere. Precursor southward interplanetary magnetic fields are detected prior to the PPs hitting the magnetosphere. Our hypothesis is that these southward fields input energy into the magnetosphere/magnetotail and the PPs trigger the release of the stored energy.

scholarly journals The Red Line of Atomic Oxygen in the Day Airglow

1964 ◽  
Vol 21 (5) ◽  
pp. 463-474 ◽  
Author(s):  
A. Dalgarno ◽  
James C. G. Walker
Keyword(s):  
Atomic Oxygen ◽  
Red Line

scholarly journals A Search for an Excited Kp=0+ Rotational Band in 24Mg

1976 ◽  
Vol 29 (3) ◽  
pp. 139 ◽  
Author(s):  
D Branford ◽  
LE Carlson ◽  
FCP Huang ◽  
N Gardner ◽  
TR Ophel ◽  
...  
Keyword(s):  
Shell Model ◽  
Quadrupole Moment ◽  
Rotational Band ◽  
Doppler Shift ◽  
Transition Rates ◽  
Model Calculations ◽  
Doppler Shift Attenuation ◽  
Doppler Shift Attenuation Method ◽  
Absolute Transition ◽  
Good Agreement

A search is described for an excited Kn = 0+ rotational band based on the 6� 44 MeV level of 24Mg. Mean nuclear lifetimes have been measured by the Doppler shift attenuation method using the 12C('60,a)24Mg reaction and the results are 't'm = 66�29, 28�7 and 13�3 fs for levels at 6'44, 8�65 and 10� 58 MeV respectively. The absolute transition rates found for the y decays from the 6�44 and 8�65 MeV levels are in good agreement with the results of shell model calculations if it is assumed that these levels are the 0+ and 2 + members respectively of the excited Kn = 0+ rotational band. Based on this assumption, a result Qoo = 0�48 �0�08b is obtained for the intraband quadrupole moment. From a study of the 23Na(p, y) reaction, it is established that the J = 4 levels at 12� 63 and 13�05 MeV do not decay by enhanced E2 transitions to the 8� 65 MeV level. This suggests that neither of these levels is the 4 + member of the excited Kn = 0+ rotational band. An assignment of J" = 4+ is made to one member of the doublet at 10�58 MeV.

Sign in / Sign up

Export Citation Format

Share Document