The 17 GHz active region number
We report the statistics of the number of active regions (NAR) observed at 17 GHz with the Nobeyama Radioheliograph between 1992, near the maximum of cycle 22, and 2013, which also includes the maximum of cycle 24, and we compare with other activity indexes. We find that NAR minima are shorter than...
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todo:paper_0004637X_v790_n2_p_Selhorst2023-10-03T14:02:35Z The 17 GHz active region number Selhorst, C.L. Costa, J.E.R. Giménez De Castro, C.G. Valio, A. Pacini, A.A. Shibasaki, K. Sun: activity Sun: magnetic fields Sun: radio radiation We report the statistics of the number of active regions (NAR) observed at 17 GHz with the Nobeyama Radioheliograph between 1992, near the maximum of cycle 22, and 2013, which also includes the maximum of cycle 24, and we compare with other activity indexes. We find that NAR minima are shorter than those of the sunspot number (SSN) and radio flux at 10.7 cm (F10.7). This shorter NAR minima could reflect the presence of active regions generated by faint magnetic fields or spotless regions, which were a considerable fraction of the counted active regions. The ratio between the solar radio indexes F10.7/NAR shows a similar reduction during the two minima analyzed, which contrasts with the increase of the ratio of both radio indexes in relation to the SSN during the minimum of cycle 23-24. These results indicate that the radio indexes are more sensitive to weaker magnetic fields than those necessary to form sunspots, of the order of 1500 G. The analysis of the monthly averages of the active region brightness temperatures shows that its long-term variation mimics the solar cycle; however, due to the gyro-resonance emission, a great number of intense spikes are observed in the maximum temperature study. The decrease in the number of these spikes is also evident during the current cycle 24, a consequence of the sunspot magnetic field weakening in the last few years. © 2014. The American Astronomical Society. All rights reserved.. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_0004637X_v790_n2_p_Selhorst |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Sun: activity Sun: magnetic fields Sun: radio radiation |
| spellingShingle |
Sun: activity Sun: magnetic fields Sun: radio radiation Selhorst, C.L. Costa, J.E.R. Giménez De Castro, C.G. Valio, A. Pacini, A.A. Shibasaki, K. The 17 GHz active region number |
| topic_facet |
Sun: activity Sun: magnetic fields Sun: radio radiation |
| description |
We report the statistics of the number of active regions (NAR) observed at 17 GHz with the Nobeyama Radioheliograph between 1992, near the maximum of cycle 22, and 2013, which also includes the maximum of cycle 24, and we compare with other activity indexes. We find that NAR minima are shorter than those of the sunspot number (SSN) and radio flux at 10.7 cm (F10.7). This shorter NAR minima could reflect the presence of active regions generated by faint magnetic fields or spotless regions, which were a considerable fraction of the counted active regions. The ratio between the solar radio indexes F10.7/NAR shows a similar reduction during the two minima analyzed, which contrasts with the increase of the ratio of both radio indexes in relation to the SSN during the minimum of cycle 23-24. These results indicate that the radio indexes are more sensitive to weaker magnetic fields than those necessary to form sunspots, of the order of 1500 G. The analysis of the monthly averages of the active region brightness temperatures shows that its long-term variation mimics the solar cycle; however, due to the gyro-resonance emission, a great number of intense spikes are observed in the maximum temperature study. The decrease in the number of these spikes is also evident during the current cycle 24, a consequence of the sunspot magnetic field weakening in the last few years. © 2014. The American Astronomical Society. All rights reserved.. |
| format |
JOUR |
| author |
Selhorst, C.L. Costa, J.E.R. Giménez De Castro, C.G. Valio, A. Pacini, A.A. Shibasaki, K. |
| author_facet |
Selhorst, C.L. Costa, J.E.R. Giménez De Castro, C.G. Valio, A. Pacini, A.A. Shibasaki, K. |
| author_sort |
Selhorst, C.L. |
| title |
The 17 GHz active region number |
| title_short |
The 17 GHz active region number |
| title_full |
The 17 GHz active region number |
| title_fullStr |
The 17 GHz active region number |
| title_full_unstemmed |
The 17 GHz active region number |
| title_sort |
17 ghz active region number |
| url |
http://hdl.handle.net/20.500.12110/paper_0004637X_v790_n2_p_Selhorst |
| work_keys_str_mv |
AT selhorstcl the17ghzactiveregionnumber AT costajer the17ghzactiveregionnumber AT gimenezdecastrocg the17ghzactiveregionnumber AT valioa the17ghzactiveregionnumber AT paciniaa the17ghzactiveregionnumber AT shibasakik the17ghzactiveregionnumber AT selhorstcl 17ghzactiveregionnumber AT costajer 17ghzactiveregionnumber AT gimenezdecastrocg 17ghzactiveregionnumber AT valioa 17ghzactiveregionnumber AT paciniaa 17ghzactiveregionnumber AT shibasakik 17ghzactiveregionnumber |
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