A comparative analysis of the properties of the magnetic fields in leading and trailing sunspots

Zagainova, Yu. S.; Файнштейн, В. Г.; Rudenko, G. V.; Обридко, В. Н.

doi:10.1134/s1063772914120129

Cited by 3 publications

(8 citation statements)

References 13 publications

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“…For sunspots satisfying this condition, the aver age value was in leading sunspots, and ≈ 0.422. All of these values are smaller than the corresponding values obtained when the magnetic field was calculated in a potential approximation (Zagainova et al, 2014). Figure 3 shows that a positive correlation with a corre lation coefficient of 0.774 exists between the and values, for which As in (Zagainova et al, 2014), a weak negative cor relation between and on the one hand and between the maximal magnetic induction value ( ) and the umbra area (S) on the other hand was established based on SDO/HMI data.…”

Section: Comparison Of Magnetic Properties Of Leading and Trailing Sucontrasting

confidence: 69%

“…The present work continues the studies that were started in (Zagainova, 2011;Zagainova et al, 2014). The dependences of the contrast values in He II 304 above a C 304 umbra on the umbra area of leading and trailing sunspots at the cycle 24 growth phase and maximum were compared based on the solar observa tions in the SDO/AIA 304 Å channel (Lemen et al, 2012).…”

Section: Comparison Of the Properties Of Leading And Trailing Sunspotssupporting

confidence: 54%

“…Figure 1 from (Zagainova et al, 2014) illustrates magnetically con nected sunspot pairs and a single sunspot. It turned out that magnetically connected sunspots were character ized by a distinct regular umbra with a circular or ellip tical symmetry.…”

Section: Data and Methods Of Studiesmentioning

confidence: 99%

“…Using magnetic field cal culations in a potential approximation based on Bd technology (Rudenko, 2001) and SDO data for 2010-2013, Zagainova et al (2014) selected pairs of magnetically connected leading and trailing sunspots, the umbra of which are joined by magnetic field lines. It was found that the minimal angle between the field line and the normal to the solar surface (α min ) in a leading sunspot is smaller than in a trailing one iñ 81% of the cases.…”

Section: Comparison Of the Properties Of Leading And Trailing Sunspotsmentioning

confidence: 99%

“…These measurements have substan tially higher spatial resolution than the resolution pro vided by the magnetic field calculations in the solar atmosphere in a potential approximation, the data of which were used to perform a similar analysis of the field properties in leading and trailing sunspots in our previous work (Zagainova et al, 2014). We start analyzing magnetic field properties in an umbra with minimal values of the angle ( ) between the magnetic field direction and the normal to the solar surface at a point where the magnetic field was measured.…”

Section: Comparison Of Magnetic Properties Of Leading and Trailing Sumentioning

confidence: 99%

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Comparison of the properties of leading and trailing sunspots

2015

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The magnetic properties of leading and trailing sunspots were compared based on SDO/HMI and SDO/AIA data with a high spatial resolution for the growth phase and maximum of cycle 24. The properties of the solar atmosphere above sunspots are also discussed independently for both of these sunspot types. It was shown that the contrast in the He II 304 (C 304 ) line above the umbra of leading and single sunspots is on average smaller than such a contrast above the umbra of trailing sunspots and on average weakly depends on the umbra area for both C 304 sunspot types. It was established that the minimal angle between the field direc tion and the normal to the solar surface at the field measurement site is smaller in leading sunspots than in trailing ones (α min -ls < α min -fs ) in 84% of the considered magnetically connected "leading-trailing" sunspot pairs, and a positive correlation exists between angles α min -ls and α min -fs . It was found that the C 304 contrast increases with decreasing α min -ls, fs for leading and trailing sunspots, and the C 304 -ls /C 304 -fs ratio on average decreases with increasing α min -ls /α min -fs ratio. The dependences of the maximal and average magnetic induction values in an umbra on the umbra area were constructed for the first time and compared indepen dently for leading and trailing sunspots. It was concluded that the maximal and average magnetic field values do not vanish when the umbra area decreases to very small values. In all cases the magnetic field in leading and single sunspots is larger than in trailing ones.

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Section: Comparison Of Magnetic Properties Of Leading and Trailing Sucontrasting

confidence: 69%

Section: Comparison Of the Properties Of Leading And Trailing Sunspotssupporting

confidence: 54%

Section: Data and Methods Of Studiesmentioning

confidence: 99%

Section: Comparison Of the Properties Of Leading And Trailing Sunspotsmentioning

confidence: 99%

Section: Comparison Of Magnetic Properties Of Leading and Trailing Sumentioning

confidence: 99%

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