A comparison of the effects of CIR‐ and CME‐induced geomagnetic activity on thermospheric densities and spacecraft orbits: Statistical studies

Chen, Guangming; Xu, Jiyao; Wang, Wenbin; Burns, A. G.

doi:10.1002/2014ja019831

Cited by 48 publications

(49 citation statements)

References 32 publications

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“…Above this value, we recognize larger scattering and some indication of saturation. The lower correlation between the AE index and the thermospheric densities is in agreement with previous findings [Akasofu et al, 1983;Baumjohann, 1986;Chen et al, 2014]. These authors revealed some limitations concerning the measured quantity (H field), the existence of longitudinal gaps and the small latitudinal range of the contributing observatories.…”

Section: Resultssupporting

confidence: 91%

Thermospheric and geomagnetic responses to interplanetary coronal mass ejections observed by ACE and GRACE: Statistical results

et al. 2015

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For the period July 2003 to August 2010, the interplanetary coronal mass ejection (ICME) catalogue maintained by Richardson and Cane lists 106 Earth‐directed events, which have been measured in situ by plasma and field instruments on board the ACE satellite. We present a statistical investigation of the Earth's thermospheric neutral density response by means of accelerometer measurements collected by the Gravity Recovery And Climate Experiment (GRACE) satellites, which are available for 104 ICMEs in the data set, and its relation to various geomagnetic indices and characteristic ICME parameters such as the impact speed ( vmax), southward magnetic field strength (Bz). The majority of ICMEs causes a distinct density enhancement in the thermosphere, with up to a factor of 8 compared to the preevent level. We find high correlations between ICME Bz and thermospheric density enhancements (≈0.9), while the correlation with the ICME impact speed is somewhat smaller (≈0.7). The geomagnetic indices revealing the highest correlations are Dst and SYM‐H(≈0.9); the lowest correlations are obtained for Kp and AE (≈0.7), which show a nonlinear relation with the thermospheric density enhancements. Separating the response for the shock‐sheath region and the magnetic structure of the ICME, we find that the Dst and SYM‐H reveal a tighter relation to the Bz minimum in the magnetic structure of the ICME, whereas the polar cap indices show higher correlations with the Bz minimum in the shock‐sheath region. Since the strength of the Bz component—either in the sheath or in the magnetic structure of the ICME—is highly correlated (≈0.9) with the neutral density enhancement, we discuss the possibility of satellite orbital decay estimates based on magnetic field measurements at L1, i.e., before the ICME hits the Earth magnetosphere. These results are expected to further stimulate progress in space weather understanding and applications regarding satellite operations.

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Section: Resultssupporting

confidence: 91%

Thermospheric and geomagnetic responses to interplanetary coronal mass ejections observed by ACE and GRACE: Statistical results

et al. 2015

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“…CIR‐ and CME‐driven storms can be classified based on the features of proton temperature, solar wind speed, magnetic field, and proton density (e.g., Richardson & Cane, ). CME‐driven storms can be identified by the stronger magnetic field, the enhanced solar wind speed, low proton temperature, and high ratio between the densities of alpha particles and protons (Chen et al, ; Gonzalez et al, ; Huttunen et al, ). Figure shows an example of a geomagnetic storm driven by CME during 15–20 March 2015.…”

Section: Methodsmentioning

confidence: 99%

“…On the other hand, the main features of CIR‐driven storms are an enhancement of proton temperature, an increase of solar wind speed, a compression of magnetic field, Bz component fluctuates throughout interval due to high‐speed streams, and proton density increases to unusually high values (e.g., Chen et al, ; Mavromichalaki et al, ; Xystouris et al, ).…”

Section: Methodsmentioning

confidence: 99%

Ionospheric Responses to CME‐ and CIR‐Driven Geomagnetic Storms Along 30°E–40°E Over the African Sector From 2001 to 2015

Matamba

Habarulema

2018

Space Weather

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In this paper, we present the responses of the ionospheric total electron content (TEC) to coronal mass ejection (CME)‐ and corotating interaction region (CIR)‐driven storms using stations that lie within 30°E–40°E geographic longitude in middle, low, and equatorial latitudes over the African sector. CIR‐driven storms are generally weak (−50 nT < Dst < −25 nT) to moderate (−100 nT < Dst < −50 nT) in intensity, while CME‐driven storms are often associated with the intense (Dst < −100 nT) geomagnetic storms. CIR‐driven storms have long recovery phase as compared to CME‐driven storms. CME‐ and CIR‐driven storms were classified based on the features of proton temperature, magnetic field, solar wind speed, and proton density. The storm periods analyzed occurred during the period 2001–2015, which covers part of solar cycles 23 and 24. Disturbance storm time (Dst) ≤ −30 nT and Kp ≥ 3 indices were used simultaneously to identify the storm periods considered. The total number of CME‐ and CIR‐driven storms identified was 148 and 167, respectively. However, due to lack of TEC data, the number of CME‐ and CIR‐driven storms considered for the middle‐latitude, low‐latitude, and equatorial latitude stations are different for different regions. TEC data used in this study was derived from the Global Navigation Satellite System observations. The statistical analysis of ionospheric storm effects were compared over middle, low, and equatorial latitudes in the African sector for the first time. Negative ionospheric storm effects occurred only during CME‐driven storms over midlatitude stations and were more prevalent in summer. For the low and equatorial latitudes, negative ionospheric storm effects were observed during both CME‐ and CIR‐driven storms. Our analysis has shown that positive ionospheric storm effects were more prevalent over middle, low, and equatorial latitudes during both CME‐ and CIR‐driven storms. A significant number of cases where the electron density changes remained within the background variability during storm conditions were observed over the low‐latitude stations compared to other latitude regions.

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“…These recurrent geomagnetic activities can perturb the ionosphere and thermosphere on a global scale as a result of energy and momentum deposition [ Lei et al ., ; Thayer et al ., ; Wang et al ., ; Burns et al ., ; Solomon et al ., ; Verkhoglyadova et al ., ]. As CIR and high‐speed stream‐induced geomagnetic activity can last for a long period of time (up to 27 days) due to the continuous Alfvén fluctuations within the high‐speed stream proper [ Tsurutani and Gonzalez , ; Tsurutani et al ., , ], the resulting total thermospheric density and satellite orbit perturbations can be larger than those produced by major geomagnetic storms associated with coronal mass ejections, [ Chen et al ., , ].…”

Section: Introductionmentioning

confidence: 99%

Multiday thermospheric density oscillations associated with variations in solar radiation and geomagnetic activity

Wang

Zhang

et al. 2015

JGR Space Physics

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Thermospheric densities observed by Challenging Minisatellite Payload and Gravity Recovery and Climate Experiment satellites during 2002-2010 and the globally averaged thermospheric densities from 1967 to 2007 have been used to investigate latitudinal, longitudinal, and height dependences of the multiday oscillations of thermospheric densities. The data show that the main multiday oscillations in thermospheric densities are 27, 13.5, 9, and 7 day oscillations. The high-correlation coefficients between the density oscillations and the F 10.7 or Ap index indicate that these oscillations are externally driven. The 27 day density oscillation, being the strongest, is induced by variations in solar radiation, as well as recurrent geomagnetic activity that is the result of corotating interaction regions (CIRs) and high-speed solar wind streams of coronal hole origin. Density oscillations at periods of 13.5, 9, and 7 days at solar minimum and during the declining phase are stronger than those at solar maximum. These oscillations are mainly associated with recurrent geomagnetic activity due to coronal hole high-speed streams and CIRs. The multiday, periodic oscillations of thermospheric density exhibit strong latitudinal and longitudinal variations in the geomagnetic coordinate and oscillate synchronously at different heights. Oscillations with zonal wave number 0 oscillate globally, whereas those with nonzero wave numbers are strong at high geomagnetic latitudes, and hemispherically asymmetric. They are stronger in the Southern Hemisphere. The spectral distributions of thermospheric densities at different heights have almost the same latitude and longitude structures, but the spectral magnitudes increase with height.

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A comparison of the effects of CIR‐ and CME‐induced geomagnetic activity on thermospheric densities and spacecraft orbits: Statistical studies

Cited by 48 publications

References 32 publications

Thermospheric and geomagnetic responses to interplanetary coronal mass ejections observed by ACE and GRACE: Statistical results

Thermospheric and geomagnetic responses to interplanetary coronal mass ejections observed by ACE and GRACE: Statistical results

Ionospheric Responses to CME‐ and CIR‐Driven Geomagnetic Storms Along 30°E–40°E Over the African Sector From 2001 to 2015

Multiday thermospheric density oscillations associated with variations in solar radiation and geomagnetic activity

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