Modification of midlatitude ionospheric parameters in the F2 layer by persistent high‐speed solar wind streams

Denton, M. H.; Ulich, Thomas; Turunen, Esa

doi:10.1029/2008sw000443

Cited by 43 publications

(64 citation statements)

References 58 publications

(65 reference statements)

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“…The response of the rTEC shown here and its relation to the 27‐day variations produced by the solar ionizing flux, clearly requires further investigation over the time scales of a few days Denton et al [2009]…”

Section: Discussionmentioning

confidence: 96%

Response of low‐latitude ionosphere to medium‐term changes of solar and geomagnetic activity

Kutiev¹,

Otsuka²,

Pancheva³

et al. 2012

J. Geophys. Res.

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[1] The paper presents the medium-term quasi periodic ($9-27 day) response of middle and low-latitude ionosphere to solar [F10.7) and geomagnetic (Kp-index) forcing. The ionospheric response is examined by wavelet analysis of the relative deviations of TEC over Japan for the period of time 2000-2008. It is found that the $27-day rTEC oscillations correlate well with the same oscillations of the solar index F10.7 particularly in the solar maximum and its early declining phase (2001)(2002)(2003)(2004)(2005). During the declining phase of solar activity (for example, year of 2005) the Kp-index variability exhibits additionally strong oscillations with periods 13.5-and 9-days. Similar oscillations are found in rTEC as well but they do not follow the geomagnetic forcing as faithfully as those associated with F10.7. During solar minimum the quasi periodic rTEC variability is shaped mainly by the recurrent geomagnetic activity. An attempt is made to investigate the latitudinal dependence of the $9-27-day rTEC response over Japan as well as the phase relationship between the forcing and response.

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Section: Discussionmentioning

confidence: 96%

Response of low‐latitude ionosphere to medium‐term changes of solar and geomagnetic activity

Kutiev¹,

Otsuka²,

Pancheva³

et al. 2012

J. Geophys. Res.

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“…To assess the general behavior of the trapped and precipitating energetic electrons during HSS‐driven storms, we conducted a superposed epoch analysis of 42 HSS storms that occurred between 2003 and 2005. The storms were selected by examining the solar wind velocities and seeking intervals of east‐west flow deflection followed by sustained elevated solar wind speed, and correspond to the subset of the 124 HSS storms used successfully in the studies of the magnetospheric response to HSSs [ Borovsky and Denton , 2008, 2009a, 2009b; Denton and Borovsky , 2008, 2009; Denton et al , 2009, 2010] which occurred after the launch of NOAA‐15 in 1998. The zero epoch for each storm was taken to be the time of storm convection onset.…”

Section: Superposed Epoch Analysismentioning

confidence: 99%

Energetic electron precipitation during high-speed solar wind stream driven storms

et al. 2011

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[1] Electron precipitation from the Earth's inner magnetosphere transmits solar variability to the Earth's upper atmosphere and may affect surface level climate. Here we conduct a superposed epoch analysis of energetic electrons observed by the NOAA POES spacecraft during 42 high-speed solar wind stream (HSS) driven geomagnetic storms to determine the temporal evolution and global distribution of the precipitating flux. The flux of trapped and precipitating E > 30 keV electrons increases immediately following storm onset and remains elevated during the passage of the HSS. In contrast, the trapped and precipitating relativistic electrons (E > 1 MeV) drop out following storm onset and subsequently increase during the recovery phase to levels which eventually exceed the prestorm levels. There is no evidence for enhanced precipitation of relativistic electrons during the MeV flux drop out, suggesting that flux drop outs during the main phase of HSS-driven storms are not due to precipitation to the atmosphere. On average, the flux of precipitating E > 30 keV electrons is enhanced by a factor of ∼10 during the passage of the high-speed stream at all geographic longitudes. In contrast, the precipitating relativistic electron count rate is observed to peak in the region poleward of the South Atlantic Anomaly. During the passage of the high-speed stream, the flux of precipitating E > 30 keV electrons peaks in the region from 2100 to 1200 magnetic local time at low L (4 < L < 7) and in the prenoon sector at high L (7 < L < 9), suggesting that chorus waves are responsible for the precipitation of E > 30 keV electrons in both regions.

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“…Thayer et al (2008) have shown that the thermospheric mass density response is global and varies coherently with the recurrent geomagnetic activity, although the response is slightly larger at high latitudes. Modifications of the midlatitude F region during persistent HSSs have been studied by Denton et al (2009). By using superposed epoch analysis, these authors studied changes in F-region parameters before and after the onset of magnetospheric convection, the latter represented by sudden increases of Kp-index above 4.…”

Section: Medium-and Long-term Ionospheric Response To the Changes In mentioning

confidence: 99%

Solar activity impact on the Earth’s upper atmosphere

Kutiev

Tsagouri

Perrone

et al. 2013

J. Space Weather Space Clim.

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The paper describes results of the studies devoted to the solar activity impact on the Earth's upper atmosphere and ionosphere, conducted within the frame of COST ES0803 Action. Aim: The aim of the paper is to represent results coming from different research groups in a unified form, aligning their specific topics into the general context of the subject. Methods: The methods used in the paper are based on data-driven analysis. Specific databases are used for spectrum analysis, empirical modeling, electron density profile reconstruction, and forecasting techniques. Results: Results are grouped in three sections: Medium-and long-term ionospheric response to the changes in solar and geomagnetic activity, storm-time ionospheric response to the solar and geomagnetic forcing, and modeling and forecasting techniques. Section 1 contains five subsections with results on 27-day response of low-latitude ionosphere to solar extreme-ultraviolet (EUV) radiation, response to the recurrent geomagnetic storms, long-term trends in the upper atmosphere, latitudinal dependence of total electron content on EUV changes, and statistical analysis of ionospheric behavior during prolonged period of solar activity. Section 2 contains a study of ionospheric variations induced by recurrent CIR-driven storm, a case-study of polar cap absorption due to an intense CME, and a statistical study of geographic distribution of so-called E-layer dominated ionosphere. Section 3 comprises empirical models for describing and forecasting TEC, the F-layer critical frequency foF2, and the height of maximum plasma density. A study evaluates the usefulness of effective sunspot number in specifying the ionosphere state. An original method is presented, which retrieves the basic thermospheric parameters from ionospheric sounding data.

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Modification of midlatitude ionospheric parameters in the F2 layer by persistent high‐speed solar wind streams

Cited by 43 publications

References 58 publications

Response of low‐latitude ionosphere to medium‐term changes of solar and geomagnetic activity

Response of low‐latitude ionosphere to medium‐term changes of solar and geomagnetic activity

Energetic electron precipitation during high-speed solar wind stream driven storms

Solar activity impact on the Earth’s upper atmosphere

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