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Study of the Lightning Activity Over Poland for Different Solar Activity

Jan Błęcki

Jan Błęcki

Space Research Centre, Polish Academy of SciencesWarsaw, Poland
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Błęcki, Jan
, 
Rafał Iwański

Rafał Iwański

Satellite Remote Sensing Department, Institute of Meteorology and Water Management – National Research InstituteCracow, Poland
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Iwański, Rafał
, 
Roman Wronowski

Roman Wronowski

Space Research Centre, Polish Academy of SciencesWarsaw, Poland
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Wronowski, Roman
 and 
Paweł Jujeczko

Paweł Jujeczko

Space Research Centre, Polish Academy of SciencesWarsaw, Poland
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Jujeczko, Paweł
  
Dec 29, 2022
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Published Online: Dec 29, 2022
Page range: 194 - 209
Received: Aug 22, 2022
Accepted: Nov 16, 2022
DOI: https://doi.org/10.2478/arsa-2022-0010
Keywords
© 2022 Jan Błęcki et al., published by Sciendo
This work is licensed under the Creative Commons Attribution 4.0 International License.

Figure 1.

The 23rd–24th solar cycle. The red line shows an averaged sunspot number. The red vertical arrows indicate the time interval of DEMETER operation, 06.29.2004 is the day of launch, 12.09.2010 is the day of switch off of the satellite’s payload (based on Alvestad, 2012).
The 23rd–24th solar cycle. The red line shows an averaged sunspot number. The red vertical arrows indicate the time interval of DEMETER operation, 06.29.2004 is the day of launch, 12.09.2010 is the day of switch off of the satellite’s payload (based on Alvestad, 2012).

Figure 2.

The satellite measurements of the solar activity are represented by a number of CMEs (a), sunspot number (b), and a number of strong flares (c) (McIntosh et al., 2015)
The satellite measurements of the solar activity are represented by a number of CMEs (a), sunspot number (b), and a number of strong flares (c) (McIntosh et al., 2015)

Figure 3.

The total annual amount of lightning discharges in three basic types. As expected, the domination of IC discharges is clear. The visible maximum relates to the year 2007, which was not especially standing out in terms of solar activity.
The total annual amount of lightning discharges in three basic types. As expected, the domination of IC discharges is clear. The visible maximum relates to the year 2007, which was not especially standing out in terms of solar activity.

Figure 4.

Monthly thunderstorm activity for the period of DEMETER operation. The color of lines indicates different types of discharge.
Monthly thunderstorm activity for the period of DEMETER operation. The color of lines indicates different types of discharge.

Figure 5a.

The registrations of the waveform of the electric field in the frequency range ELF (upper panel) and spectrogram of it (lower panel), and in VLF (third panel) and spectrogram of it (lower panel). The bottom panel shows the spectrogram of high-frequency variations of the electric field. The figure presents measurements during thunderstorms on July 23, 2009 when there was a minimum of solar activity.
The registrations of the waveform of the electric field in the frequency range ELF (upper panel) and spectrogram of it (lower panel), and in VLF (third panel) and spectrogram of it (lower panel). The bottom panel shows the spectrogram of high-frequency variations of the electric field. The figure presents measurements during thunderstorms on July 23, 2009 when there was a minimum of solar activity.

Figure 5b.

The same as for Figure 5a, but for the year 2006 when CMEs occurred
The same as for Figure 5a, but for the year 2006 when CMEs occurred

Figure 6a.

The same as in Figure 5a, but for a thunderstorm in 2005 when the sunspot number was highest for the time of DEMETER operation.
The same as in Figure 5a, but for a thunderstorm in 2005 when the sunspot number was highest for the time of DEMETER operation.

Figure 6b.

The same as in Figure 5a, but for a thunderstorm in 2005 when the sunspot number was highest for the time of DEMETER operation (another example).
The same as in Figure 5a, but for a thunderstorm in 2005 when the sunspot number was highest for the time of DEMETER operation (another example).

Figure 7a.

The same as in Figure 5a, but for the year of very low sunspot number, 2010
The same as in Figure 5a, but for the year of very low sunspot number, 2010

Figure 7b.

The same as in Figure 5a, but for the year of a moderate sunspot number, 2006
The same as in Figure 5a, but for the year of a moderate sunspot number, 2006

Figure 8.

Correlation between solar activity represented by sunspot number (SSN upper panel) and cosmic rays’(CR) flux measured in four stations (MCMD = McMurdo, NEWK = Newark, SOPO = South Pole, THUL = Thule) (Ross and Chaplin, 2019)
Correlation between solar activity represented by sunspot number (SSN upper panel) and cosmic rays’(CR) flux measured in four stations (MCMD = McMurdo, NEWK = Newark, SOPO = South Pole, THUL = Thule) (Ross and Chaplin, 2019)

Figure 1.

The 23rd–24th solar cycle. The red line shows an averaged sunspot number. The red vertical arrows indicate the time interval of DEMETER operation, 06.29.2004 is the day of launch, 12.09.2010 is the day of switch off of the satellite’s payload (based on Alvestad, 2012).
The 23rd–24th solar cycle. The red line shows an averaged sunspot number. The red vertical arrows indicate the time interval of DEMETER operation, 06.29.2004 is the day of launch, 12.09.2010 is the day of switch off of the satellite’s payload (based on Alvestad, 2012).

Figure 2.

The satellite measurements of the solar activity are represented by a number of CMEs (a), sunspot number (b), and a number of strong flares (c) (McIntosh et al., 2015)
The satellite measurements of the solar activity are represented by a number of CMEs (a), sunspot number (b), and a number of strong flares (c) (McIntosh et al., 2015)

Figure 3.

The total annual amount of lightning discharges in three basic types. As expected, the domination of IC discharges is clear. The visible maximum relates to the year 2007, which was not especially standing out in terms of solar activity.
The total annual amount of lightning discharges in three basic types. As expected, the domination of IC discharges is clear. The visible maximum relates to the year 2007, which was not especially standing out in terms of solar activity.

Figure 4.

Monthly thunderstorm activity for the period of DEMETER operation. The color of lines indicates different types of discharge.
Monthly thunderstorm activity for the period of DEMETER operation. The color of lines indicates different types of discharge.

Figure 5a.

The registrations of the waveform of the electric field in the frequency range ELF (upper panel) and spectrogram of it (lower panel), and in VLF (third panel) and spectrogram of it (lower panel). The bottom panel shows the spectrogram of high-frequency variations of the electric field. The figure presents measurements during thunderstorms on July 23, 2009 when there was a minimum of solar activity.
The registrations of the waveform of the electric field in the frequency range ELF (upper panel) and spectrogram of it (lower panel), and in VLF (third panel) and spectrogram of it (lower panel). The bottom panel shows the spectrogram of high-frequency variations of the electric field. The figure presents measurements during thunderstorms on July 23, 2009 when there was a minimum of solar activity.

Figure 5b.

The same as for Figure 5a, but for the year 2006 when CMEs occurred
The same as for Figure 5a, but for the year 2006 when CMEs occurred

Figure 6a.

The same as in Figure 5a, but for a thunderstorm in 2005 when the sunspot number was highest for the time of DEMETER operation.
The same as in Figure 5a, but for a thunderstorm in 2005 when the sunspot number was highest for the time of DEMETER operation.

Figure 6b.

The same as in Figure 5a, but for a thunderstorm in 2005 when the sunspot number was highest for the time of DEMETER operation (another example).
The same as in Figure 5a, but for a thunderstorm in 2005 when the sunspot number was highest for the time of DEMETER operation (another example).

Figure 7a.

The same as in Figure 5a, but for the year of very low sunspot number, 2010
The same as in Figure 5a, but for the year of very low sunspot number, 2010

Figure 7b.

The same as in Figure 5a, but for the year of a moderate sunspot number, 2006
The same as in Figure 5a, but for the year of a moderate sunspot number, 2006

Figure 8.

Correlation between solar activity represented by sunspot number (SSN upper panel) and cosmic rays’(CR) flux measured in four stations (MCMD = McMurdo, NEWK = Newark, SOPO = South Pole, THUL = Thule) (Ross and Chaplin, 2019)
Correlation between solar activity represented by sunspot number (SSN upper panel) and cosmic rays’(CR) flux measured in four stations (MCMD = McMurdo, NEWK = Newark, SOPO = South Pole, THUL = Thule) (Ross and Chaplin, 2019)
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