Chromosphere Activity Relation with Solar Dynamo Magnetic Activity Cycle
In this article, we analyzed the abnormal thickness of the chromosphere above the coronal holes (CH) at the poles of the Sun for 13 years (2010-2022), on the 15th of every month, by using AIA/SDO telescope data. We used the light emitted from helium-2 (He II) at a wavelength of 304 {AA} at about 50,...
Saved in:
| Main Authors: | , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
Damghan university
2022-10-01
|
| Series: | Iranian Journal of Astronomy and Astrophysics |
| Subjects: | |
| Online Access: | https://ijaa.du.ac.ir/article_317_b45fc0aa13a9791ca06264a696c2fa4a.pdf |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1841545113682051072 |
|---|---|
| author | Ehsan Tavabi Mina Rajabi Sima Zeighami |
| author_facet | Ehsan Tavabi Mina Rajabi Sima Zeighami |
| author_sort | Ehsan Tavabi |
| collection | DOAJ |
| description | In this article, we analyzed the abnormal thickness of the chromosphere above the coronal holes (CH) at the poles of the Sun for 13 years (2010-2022), on the 15th of every month, by using AIA/SDO telescope data. We used the light emitted from helium-2 (He II) at a wavelength of 304 {AA} at about 50,000 K to investigate the solar holes in its north and south poles. This light is emitted from the chromosphere and the transition region. According to the values of the graphs obtained by the MATLAB program and the comparison between solar cycles during the 2010-2022 years, it was seen that the Full width of the intensity curves at half maximum (FWHM) in the poles, and as a result the magnetic activity of the sun and especially the activity of coronal cavities as the main source of the solar dipole magnetic field before cycle 25 is significantly greater than this thickness before cycle 24. According to the relationship between the number of sunspots and the solar activity in the coronal holes at the solar poles with a time delay of 2 to 5 years, we expect the maximum increasing in the number of sunspots around the year 2025. As a result,in terms of the number of sunspots, the height of the solar cycle 25 probably is higher than the cycle 24, which was a low sunspot number cycle. We also concluded that the thickness of the Chromosphere has an inverse relationship with solar dynamo magnetic activity cycle. |
| format | Article |
| id | doaj-art-446e6a5ef51443878e813bb43840da37 |
| institution | Kabale University |
| issn | 2322-4924 2383-403X |
| language | English |
| publishDate | 2022-10-01 |
| publisher | Damghan university |
| record_format | Article |
| series | Iranian Journal of Astronomy and Astrophysics |
| spelling | doaj-art-446e6a5ef51443878e813bb43840da372025-01-12T10:09:48ZengDamghan universityIranian Journal of Astronomy and Astrophysics2322-49242383-403X2022-10-01929710710.22128/ijaa.2022.636.1135317Chromosphere Activity Relation with Solar Dynamo Magnetic Activity CycleEhsan Tavabi0Mina Rajabi1Sima Zeighami2Physics Department, Payame Noor University (PNU), 19395-3697-Tehran, I. R. of IranPhysics Department, Payame Noor University (PNU), 19395-3697-Tehran, I. R. of IranDepartment of Physics, Tabriz Branch, Islamic Azad University, Tabriz, IranIn this article, we analyzed the abnormal thickness of the chromosphere above the coronal holes (CH) at the poles of the Sun for 13 years (2010-2022), on the 15th of every month, by using AIA/SDO telescope data. We used the light emitted from helium-2 (He II) at a wavelength of 304 {AA} at about 50,000 K to investigate the solar holes in its north and south poles. This light is emitted from the chromosphere and the transition region. According to the values of the graphs obtained by the MATLAB program and the comparison between solar cycles during the 2010-2022 years, it was seen that the Full width of the intensity curves at half maximum (FWHM) in the poles, and as a result the magnetic activity of the sun and especially the activity of coronal cavities as the main source of the solar dipole magnetic field before cycle 25 is significantly greater than this thickness before cycle 24. According to the relationship between the number of sunspots and the solar activity in the coronal holes at the solar poles with a time delay of 2 to 5 years, we expect the maximum increasing in the number of sunspots around the year 2025. As a result,in terms of the number of sunspots, the height of the solar cycle 25 probably is higher than the cycle 24, which was a low sunspot number cycle. We also concluded that the thickness of the Chromosphere has an inverse relationship with solar dynamo magnetic activity cycle.https://ijaa.du.ac.ir/article_317_b45fc0aa13a9791ca06264a696c2fa4a.pdfsolar cycle 24 and 25coronal activitiessunspotschromosphere thickness |
| spellingShingle | Ehsan Tavabi Mina Rajabi Sima Zeighami Chromosphere Activity Relation with Solar Dynamo Magnetic Activity Cycle Iranian Journal of Astronomy and Astrophysics solar cycle 24 and 25 coronal activities sunspots chromosphere thickness |
| title | Chromosphere Activity Relation with Solar Dynamo Magnetic Activity Cycle |
| title_full | Chromosphere Activity Relation with Solar Dynamo Magnetic Activity Cycle |
| title_fullStr | Chromosphere Activity Relation with Solar Dynamo Magnetic Activity Cycle |
| title_full_unstemmed | Chromosphere Activity Relation with Solar Dynamo Magnetic Activity Cycle |
| title_short | Chromosphere Activity Relation with Solar Dynamo Magnetic Activity Cycle |
| title_sort | chromosphere activity relation with solar dynamo magnetic activity cycle |
| topic | solar cycle 24 and 25 coronal activities sunspots chromosphere thickness |
| url | https://ijaa.du.ac.ir/article_317_b45fc0aa13a9791ca06264a696c2fa4a.pdf |
| work_keys_str_mv | AT ehsantavabi chromosphereactivityrelationwithsolardynamomagneticactivitycycle AT minarajabi chromosphereactivityrelationwithsolardynamomagneticactivitycycle AT simazeighami chromosphereactivityrelationwithsolardynamomagneticactivitycycle |