Specific features of ionospheric disturbances accompanying the 14–20 January 2022 magnetic storm

Мұқаба

Дәйексөз келтіру

Толық мәтін

Ашық рұқсат Ашық рұқсат
Рұқсат жабық Рұқсат берілді
Рұқсат жабық Рұқсат ақылы немесе тек жазылушылар үшін

Аннотация

We conducted the analysis of ionospheric disturbances that occurred during the moderate magnetic storm of 14–20 January 2022. The study is based on data of vertical and oblique ionospheric sounding obtained in the Northeastern region of Russia, and supplemented by observations at HF radars and magnetic observatories. It has been revealed that the amplitudes of positive and negative ionospheric disturbances accompanying this storm are comparable to those observed on other days of January during weak magnetic storms and disturbances. Specific features of the disturbances observed only during the storm in question are as follows: (1) a midnight–morning increase of the maximum observed frequency of one-hop mode of HF radio wave propagation on the paths Norilsk — Tory and Magadan — Tory on 14 January; (2) enhanced nighttime fluctuations in F2-layer critical frequency in Irkutsk and the maximum observed frequency of one-hop mode on the path Magadan — Tory on 15 January; (3) Morning–midday Es layers with limiting frequencies reaching 7 MHz that were observed in mid-latitudes at the end of the first and beginning of the second day of the storm recovery phase.

Толық мәтін

Рұқсат жабық

Авторлар туралы

V. Kurkin

Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of Sciences (ISTP SB RAS)

Хат алмасуға жауапты Автор.
Email: vikurkin@yandex.ru
Ресей, Irkutsk, 664033

N. Zolotukhina

Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of Sciences (ISTP SB RAS)

Email: zolot@iszf.irk.ru
Ресей, Irkutsk, 664033

S. Ponomarchuk

Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of Sciences (ISTP SB RAS)

Email: spon@iszf.irk.ru
Ресей, Irkutsk, 664033

A. Oinats

Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of Sciences (ISTP SB RAS)

Email: oinats@iszf.irk.ru
Ресей, Irkutsk, 664033

K. Ratovsky

Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of Sciences (ISTP SB RAS)

Email: ratovsky@iszf.irk.ru
Ресей, Irkutsk, 664033

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1. JATS XML
Жүктеу
2. Fig. 1. Variations in the speed of the Vsw solar wind (a); the Akasofu parameter ε (b); Dst- (c) and Kr- (d) indices in January 2022. Horizontal lines mark on panel (a) the Vsw value = 450 km/s, used to distinguish high—speed flows [Borovsky and Denton, 2010]; panel (c) shows Dst levels= -30 and -50 Nt, which are the upper thresholds for mild and moderate magnetic storms, respectively [Loewe and Prolss, 1997]; panel (d) shows Kp =5, which is used as the lower threshold for identifying magnetic storms. The symbols q and d with numbers indicate magnetically calm and magnetically disturbed days in accordance with their designations on [URL qd].

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3. Fig. 2. Map of the location of ionospheric sounding devices and magnetic observatories. The dots show ionospheric stations and magnetic observatories; dashed and solid lines represent radio paths and radar beams, respectively, and crosses represent the midpoints of radio paths.

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4. Fig. 3. Variations of the Dst index (a); MNH1F2 on the Norilsk–Tora (b) and Magadan–Tora (c) highways; foF2 and foEs in Irkutsk (d). The current/background values of MNH1F2 and foF2 are shown by black/gray lines, the values of foEs are squares.

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5. Fig. 4. The upper panel shows the variations of the Dst index; below - DMNH1F2 on the Norilsk—Tora, Magadan–Tora and foF2 routes over Irkutsk, the black arrows mark the elements of the ionospheric storm, presented in paragraphs 4.1, 4.2, 4.5 and 4.6 of Section 4 (see text).

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6. Fig. 5. From top to bottom on the left, the changes in the corrected geomagnetic latitude of the auroral oval (gray figure) and the bottom of the ISU at longitudes 105o and 120o E (lines), MNH1F2 on the Norilsk–Tora and Magadan–Tora routes are shown; on the right, the chart of the SME index and variations in the H—components of the geomagnetic field recorded by three observatories, located in the longitude sector in question. The dynamics of the ISU bottom is calculated using the model [Deminov and Shubin, 2018]. The boundaries of the oval are constructed according to the data provided on [URL Oval].

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7. Fig. 6. Map of auroral echo sources recorded by two HF radars at 22:15 UT on 01/14/2022. Dashed/solid lines show the position of the northern/southern border of the oval (plotted according to [URL Oval]).

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8. Fig. 7. Variations of the Dst index, the latitude of the ISU, and the short-period components of MNF1F2 on the Magadan–Toryand foF2 highway in Irkutsk at night.

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9. Fig. 8. The upper left shows the foEs values measured in Irkutsk during each day of January 2022; at the bottom is the time of registration of foEs greater than 3.1 MHz. Here 3.1 MHz is the upper quartile of the monthly range of foEs values, marked in the figure with a horizontal dotted line. On the right is an ionogram containing reflections from a sporadic diffuse layer. It was obtained in Tori using an LCHM ionosonde.

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10. Fig. 9. (a) — Values of positive ΔMH1F2 observed on the Magadan highway−Tori for each day of January 2022 (above), and the time of registration of those of them that lie above the upper quartiles of the monthly series of positive ΔMH1F2 (below); (b) is the same for negative ΔMH1F2 and those of them that lie below the lower quartiles of negative ΔMH1F2. Panels (c) and (d) show similar graphs constructed for positive and negative δfoF2. Horizontal dashed lines mark the upper quartiles for positive and lower quartiles for negative perturbations.

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11. Fig. 10. For positive (a–b) and negative (d–e) disturbances observed in Irkutsk in January 2022, changes in the absolute deviations of foF2 and hmF2 from their background values are shown.

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