Responses of the Thermosphere and Ionosphere System to Concurrent Solar Flares and Geomagnetic Storms. Issue 3 (28th February 2020)

• Record Type: Journal Article
• Authors: Qian, Liying; Wang, Wenbin; Burns, Alan G.; Chamberlin, Phillip C.; Solomon, Stanley C.
• Is Part Of: Journal of geophysical research. Volume 125:Issue 3(2020)
• Page Start: n/a
• Page End: n/a
• Publication Date: 2020-02-28
• Subjects: thermosphere -- ionosphere -- solar flare -- geomagnetic storm -- aurora oval -- traveling atmospheric disturbance; Magnetospheric physics -- Periodicals; Space environment -- Periodicals; Cosmic physics -- Periodicals; Planets -- Atmospheres -- Periodicals; Heliosphere (Astrophysics) -- Periodicals; Geophysics -- Periodicals; 523.01
• DOI: 10.1029/2019JA027431
• Languages: English
• ISSNs: 2169-9380

Abstract

Abstract: We conducted numerical simulations to examine dayside thermosphere and ionosphere responses to concurrent solar flares and a geomagnetic storm during 6–11 September 2017, as well as the interplay of flare and storm effects. We found that E ‐region electron density response to the flares was much smaller inside the auroral oval than it was outside the auroral oval due to an extra source of ionization by auroral particle precipitation. During quiet times in this period, flare enhanced ionization, which decreased daytime eastward electric fields, caused an initial weakening of the vertical E × B drifts. This weakening of the vertical E × B drifts was on the order of ~20% for an X8.2 flare in this period. During storm times, flare‐induced initial changes of the vertical plasma drifts varied between being positive and being negative, depending on latitudes, due to storm‐time disturbance dynamo effects. Storm effects also overall weakened flare effects on geopotential height, ionospheric F 2 peak height hmF 2, and ionospheric F 2 peak electron density NmF 2 . In addition, storm effects changed the latitudinal distributions of flare effects on hmF 2, NmF 2, vertical plasma drifts, and O/N 2 . On the other hand, no major X‐class flare occurred shortly before or during the storm. Model simulations indicate that the weaker C‐ and M‐class flares that occurred before and during the storm had a minor effect on the amplitude of the large‐scale traveling atmosphere disturbances generated by the storm. Key Points: Flare effects were smaller inside auroral oval than outside the oval due to an extra source of ionization by particle precipitation Storm effects changed the latitudinal distributions of flare effects on hmF2, NmF2, vertical plasma drifts, and O/N2 C‐ and M‐ class flares had a minor effect on how the upper atmosphere responded to storm