GPS ionospheric TEC measurement during the 23rd November 2003 total solar eclipse at Scott Base Antarctica

Rashid, Zainol Abidin Abdul; Momani, Mohammad; Sulaiman, Sallehudin; Ali, Mohd Alaudin Mohd; Yatim, Baharudin; Fraser, G. J.; Sato, Natsuo

doi:10.1016/j.jastp.2006.03.006

Cited by 28 publications

(8 citation statements)

References 15 publications

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“…The TEC values were corrected from the receiver and satellite biases by using the AIUB Data Center of Bern University in Switzerland (AIUB, 2000). The equivalent absolute vertical TEC, Percentage deviation of the GPS TEC and the rate of change of TEC (ROT) have been calculated using standered methods (Rashid et al, 2006;Momani et al, 2008;2010;Abdullah et al, 2009).…”

Section: Methodsmentioning

confidence: 99%

GPS Ionospheric Total Electron Content and Scintillation Measurements during the October 2003 Magnetic Storm

Momani¹

2011

American Journal of Engineering and Applied Sciences

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Problem Statement: Ionospheric scintillations, cause significant effects on satellite signals for communication and navigation in equatorial region and polar regions mainly during sever magnetic storms periods. This phenomenon is not fully understood due to few studies performed. The study investigates variability of Total Electron Content (TEC) and ionospheric scintillation during October 2003 magnetic storm over Antarctica using ground based GPS technique. Approach: The TEC/scintillation measuring system at Scott Base station, consists of Trimble TS5700 24-channel (a high-precision dual-frequency GPS receiver), a Trimble Zephyr Geodetic antenna and a notebook computer for data logging. The absolute GPS TEC was calculated from differential phase advance GPS observables (1-L2). The GPS signal-to-noise ratios (C/No) and 1/L2 carrier frequencies were employed to determine the scintillation index S 4 every 60 s, amplitude scintillation (in dB-Hz) and phase scintillation. Results: The GPS measurements during storm periods at Scott Base show pronounced phase and amplitude scintillation activities, sudden increase in TEC followed by trough-like figure depletions. The maximum value of phase scintillation during the main phase of third episode was 8.3 times the value during Sudden Storm Commencement (SSC) period. Measured amplitude scintillation and S4 index on both 1 and L2 signals are >15dB-Hz and >0.4dB-Hz respectively. Conclusion/Recommendation: The timing and intensity of TEC and scintillation measurements during the storm event were are in a good agreement with WDC measurements. For this particular event, the duration of enhanced periods were approximately 12 h while periods of TEC depletions were more than 30 h. This value implies better understanding of the polar ionospheric response to magnetic storm and eases efforts for better space weather prediction in this region.

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Section: Methodsmentioning

confidence: 99%

GPS Ionospheric Total Electron Content and Scintillation Measurements during the October 2003 Magnetic Storm

Momani¹

2011

American Journal of Engineering and Applied Sciences

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“…The geomagnetic storm may corrupt and cause a problem in detecting the ionospheric response to the solar eclipse [ Afraimovich et al , 2002]. The mixed storm‐eclipse‐TIDs solar eclipses events were also reported by several researchers [ Abdul Rashid et al , 2006; Musatenko et al , 2003; Arendt , 1971; Chimonas and Hines , 1971; Flaherty et al , 1970; N. Sato et al, Conjugate ionospheric disturbances affected by the 23 November 2003 solar eclipse, paper presented at XXVIII Open Science Conference, Scientific Committee on Antarctic Research, Bremen, Germany, 2004]. Most of these measurements were made for the 23 November 2003 total solar eclipse over Antarctica and the 7 March 1970 total solar eclipse over Mexico and the southern United States.…”

Section: Introductionmentioning

confidence: 98%

“…Nowadays, the availability of GPS satellite signals gives a good opportunity for studying the temporal and spatial variations of the ionosphere. The GPS TEC measurements become widely used method by many researchers for studying the ionospheric variations caused by the solar eclipse [ Abdul Rashid et al , 2006; Korenkov et al , 2003; Baran et al , 2003; Afraimovich et al , 2002; Bamford , 2001; Liu et al , 1999; N. Jakowski et al, Total electron content studies of the solar eclipse on 11 August 1999, paper presented at International Beacon Satellite Symposium BSS‐2001, Chestnut Hill, Mass., 2001]. The employment of dual‐frequency GPS data for studying the ionospheric response to solar eclipses has obvious advantages due to global and regional coverage capability.…”

Section: Introductionmentioning

confidence: 99%

Ionospheric and geomagnetic response to the total solar eclipse on 1 August 2008 over Northern Hemisphere

2010

Self Cite

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[1] The ionospheric and geomagnetic response to the total eclipse of the Sun on 1 August 2008 over Northern Hemisphere has been examined using 14 GPS, three ISR radar, and three magnetometer ground-based stations. Three different approaches were employed to examine the TEC depletion occurrence at the GPS stations: determination of the TEC depletion parameters during the solar eclipse with respect the quiet day TEC variations, comparison of the total TEC (STEC) during the solar eclipse period with respect to quiet day TEC measurements for the same period of time, and determination of the average daily TEC obtained from eight GPS stations and compares the values with the average quiet day TEC at these stations. The GPS observations indicate obvious TEC depression occurrence at all stations with the values was varying between 11% and 40%. The observations show that TEC depression at most GPS stations started on the neck of the first contact of the eclipse followed by deeper negative deviation while the area of optical disk obscured getting larger. Periods of TEC depletion were also observed before the first contact time of solar eclipse and after the fourth contact of solar eclipse due to earlier and later obscuration of the solar corona before and after the eclipse observation time. The incoherent scatter radar observations at Svalbard, Tromso, and Sondrestrom also show clear depletion occurrence in electron density, electron temperature, ion velocity, and plasma cutoff frequency during the solar eclipse passage at these stations. Radar measurements show obvious difference in the ionospheric response between the E and F layers of ionosphere and between ion and electron temperature in the F layer. The geomagnetic field response to the solar eclipse at CBB, RESO, and NUR stations was examined by using two different techniques, first by comparing the daily variations of geomagnetic field during the eclipse period with the variations on the day before and day after the eclipse, and second by determination the D magnetic field with respect to the average quiet geomagnetic field. The results show obvious decrease in the total field, X and Z components of geomagnetic field and obvious increase in the Y component at both CBB and RESO stations. The depletion in X, Z, and total field was in the range between 15 and 28 nT while the increase in the Y component was 18-22 nT.

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“…Consequently, some eclipse effects on the ionosphere come with a delay, which can be quite substantial in some circumstances (Hoque et al, 2016;Stankov et al, 2017). In addition to the direct impact locally, that is, along the path of obscuration, a solar eclipse can induce far reaching wave-like phenomena traveling away from the path (Abidin Abdul Rashid et al, 2006;Afraimovich et al, 2000;Altadill et al, 2001;Mošna et al, 2018;Verhulst & Stankov, 2018). Considering the complex response of the ionosphere, it is of particular importance that an accurate calculation of key characteristics of solar eclipses-such as timing, locations, and levels of obscuration-is carried out, and preferably provided in advance.…”

Section: Introductionmentioning

confidence: 99%

Height Dependency of Solar Eclipse Effects: The Ionospheric Perspective

Verhulst

Stankov

2020

JGR Space Physics

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A reliable interpretation of solar eclipse effects on the geospace environment, and on the ionosphere in particular, necessitates a careful consideration of the so‐called eclipse geometry. A solar eclipse is a relatively rare astronomical phenomenon, which geometry is rather complex, specific for each event, and fast changing in time. The standard, most popular way to look at the eclipse geometry is via the two‐dimensional representation (map) of the solar obscuration on the Earth's surface, in which the path of eclipse totality is drawn together with isolines of the gradually‐decreasing eclipse magnitude farther away from this path. Such “surface maps” are widely used to readily explain some of the solar eclipse effects including, for example, the well‐known decrease in total ionization (due to the substantial decrease in solar irradiation), usually presented by the popular and easy to understand ionospheric characteristic of total electron content (TEC). However, many other effects, especially those taking place at higher altitudes, cannot be explained in this fashion. Instead, a more detailed description of the umbra (and penumbra), would be required. This paper addresses the issue of eclipse geometry effects on various ionospheric observations carried out during the total solar eclipse of 21 August 2017. In particular, GPS‐based TEC measurements were analyzed and eclipse effects on the ionosphere are interpreted with respect to the actual eclipse geometry at ionospheric heights. Whenever possible, a comparison was made with results from other eclipse events.

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GPS ionospheric TEC measurement during the 23rd November 2003 total solar eclipse at Scott Base Antarctica

Cited by 28 publications

References 15 publications

GPS Ionospheric Total Electron Content and Scintillation Measurements during the October 2003 Magnetic Storm

GPS Ionospheric Total Electron Content and Scintillation Measurements during the October 2003 Magnetic Storm

Ionospheric and geomagnetic response to the total solar eclipse on 1 August 2008 over Northern Hemisphere

Height Dependency of Solar Eclipse Effects: The Ionospheric Perspective

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