Effects of the Strong Ionospheric Storm of August 26, 2018: Results of Multipath Radiophysical Monitoring

The technique of using instantaneous maps for ionospheric storm studies is further developed. Integral parameters are introduced characterizing the main features of each map. These parameters are the net volumes of ?f0F2, ?M(3000)F2and their gradients. The magnetic storm 1-2 March, 1982 was considered and it was found that before the storm commencement and in recovery phase the Net Gradient (NG) is directed steadily to the East, while in the main phase it turns southward. NG shows where the changes of the F-layer come from. The net volume of ?f0F2 (NF) correlates well with Dst and AE indices.

Download Full-text

EFEK CME HALO PENUH PADA IONOSFER LINTANG RENDAH DARI DATA GPS BAKO DI CIBINONG [EFFECT OF FULL HALO CME ON LOW LATITUDE IONOSPHERE FROM BAKO GPS DATA IN CIBINONG]

Jurnal Sains Dirgantara ◽

10.30536/j.jsd.2017.v15.a2735 ◽

2018 ◽

Vol 15 (1) ◽

pp. 51

Author(s):

Fakhrizal Muttaqien ◽

Buldan Muslim

Keyword(s):

Total Electron Content ◽

Geomagnetic Storm ◽

Geomagnetic Disturbance ◽

Main Phase ◽

Gps Data ◽

Electron Content ◽

Ionospheric Storm ◽

Total Electron ◽

Dst Index ◽

Software Analysis

A full halo coronal mass ejections (CMEs) are most energetic solar events that eject huge amount of mass and magnetic fields into heliosphere with 360o angular angle. The full halo CME effect on the ionosphere can be determined from the ionospheric total electron content (TEC) derived from GPS data. GPS data from BAKO station in Cibinong, satellite orbital data (brcd files) and intrumental bias data (DCB files) have been used to obtain TEC using GOPI software. Analysis of the full halo CME data, Dst index, and TEC during October 2003 and February 2014 showed that the full halo CME could cause ionospheric disturbances called ionospheric storms. Magnitude and time delay of the ionospheric storms depended on the full halo CME speed. For the high-speed full halo CME, the negative ionospheric storm generally occured during recovery phase of the geomagnetic storm. When the initial phase of geomagnetic disturbance with increasing Dst index more than +30 nT, the ionospheric storm occured during main phase of geomagnetic disturbance although the main phase of geomagnetic disturbance did not reach geomagnetic storm condition. ABSTRAKCoronal mass ejection (CME) halo penuh merupakan peristiwa matahari berenergi tinggi, yang menyemburkan massa dan medan magnet ke heliosfer dengan sudut angular sebesar 360º. Efek CME halo penuh pada ionosfer dapat diketahui dari Total Electron Content (TEC). Data GPS BAKO di Cibinong, data orbit satelit (file brcd) dan data bias instrumental (file DCB) dapat digunakan untuk penentuan TEC menggunakan software GOPI. Analisis data CME halo penuh, indeks Dst, dan TEC selama bulan Oktober 2003 dan Februari 2014 menunjukkan bahwa CME halo penuh dapat menimbulkan gangguan ionosfer yang disebut badai ionosfer. Besar dan selang waktu badai ionosfer setelah terjadinya CME, tergantung pada kelajuan CME halo penuh. Untuk CME halo penuh berkelajuan tinggi, badai ionosfer negatif umumnya terjadi pada fase pemulihan badai geomagnet. Jika fase awal gangguan geomagnet diawali dengan peningkatan indeks Dst melebihi +30 nT, maka badai ionosfer dapat terjadi pada fase utama gangguan geomagnet walau gangguan geomagnet setelah fase awal tidak mencapai kondisi badai geomagnet.

Download Full-text

Positive and negative GPS-TEC ionospheric storm effects during the extreme space weather event of March 2015 over the Brazilian sector

Journal of Geophysical Research Space Physics ◽

10.1002/2015ja022214 ◽

2016 ◽

Vol 121 (6) ◽

pp. 5613-5625 ◽

Cited By ~ 38

Author(s):

P. R. Fagundes ◽

F. A. Cardoso ◽

B. G. Fejer ◽

K. Venkatesh ◽

B. A. G. Ribeiro ◽

...

Keyword(s):

Space Weather ◽

Ionospheric Storm ◽

Weather Event ◽

Storm Effects ◽

Gps Tec ◽

Space Weather Event

Download Full-text

Derivation of a planetary ionospheric storm index

Annales Geophysicae ◽

10.5194/angeo-26-2645-2008 ◽

2008 ◽

Vol 26 (9) ◽

pp. 2645-2648 ◽

Cited By ~ 49

Author(s):

T. L. Gulyaeva ◽

I. Stanislawska

Keyword(s):

Solar Cycle ◽

Extreme Values ◽

Grid Point ◽

Radiant Energy ◽

Electron Content ◽

Vertical Total Electron Content ◽

Ionospheric Storm ◽

Total Electron ◽

Grid Points ◽

Storm Index

Abstract. The planetary ionospheric storm index, Wp, is deduced from the numerical global ionospheric GPS-IONEX maps of the vertical total electron content, TEC, for more than half a solar cycle, 1999–2008. The TEC values are extracted from the 600 grid points of the map at latitudes 60° N to 60° S with a step of 5° and longitudes 0° to 345° E with a step of 15° providing the data for 00:00 to 23:00 h of local time. The local effects of the solar radiant energy are filtered out by normalizing of the TEC in terms of the solar zenith angle χ at a particular time and the local noon value χ0. The degree of perturbation, DTEC, is computed as log of TEC relative to quiet reference median for 27 days prior to the day of observation. The W-index map is generated by segmentation of DTEC with the relevant thresholds specified earlier for foF2 so that 1 or −1 stands for the quiet state, 2 or −2 for the moderate disturbance, 3 or −3 for the moderate ionospheric storm, and 4 or −4 for intense ionospheric storm at each grid point of the map. The planetary ionospheric storm Wp index is obtained from the W-index map as a latitudinal average of the distance between maximum positive and minimum negative W-index weighted by the latitude/longitude extent of the extreme values on the map. The threshold Wp exceeding 4.0 index units and the peak value Wpmax≥6.0 specify the duration and the power of the planetary ionosphere-plasmasphere storm. It is shown that the occurrence of the Wp storms is growing with the phase of the solar cycle being twice as much as the number of the magnetospheric storms with Dst≤−100 nT and Ap≥100 nT.

Download Full-text