DIAGNOSTICS OF LOCAL MAGNETIC FIELDS IN SOLAR FLARES USING FeI 5383 AND MgI 5528 LINES

Main  purpose of  the  present work is  to estimate upper limit of the local magnetic field strength in solar flares  using spectral lines FeI  5383  and MgI  5528. These lines like FeI 5233  have  low  Landé  factors  (1.12 and 1.00,  respectively) and  relatively  large spectral width (0.2–0.3 Ǻ). On this account, even in a case of very strong fields (3-4 kG) they must show the simple picture of the Zeeman splitting, with parallel to each other the bisectors of profiles I+V and I – V.  In  actual  fact,  another picture was found  for  nine flares: bisectors  of  these  lines have maximums of splitting on certain distances from line center, what must not be in the homogeneous magnetic field. In particular, both lines have peak of bisector splitting on distance 150–170 mǺ  from  line center.  If we assume  the Zeeman nature of named peculiarities then necessary fields are11.2 kGfor FeI 5383 and 10.5-11.2 kGfor MgI 5528. Likely, this agreement of field values is a new argument to reality of such very strong magnetic fields in flares.  Main purpose of the present work is to estimate upper limit of the local magnetic field strength in solar flares using spectral lines FeI 5383 and MgI 5528. These lines like FeI 5233 have low Landé factors (1.12 and 1.00, respectively) and relatively large spectral width (0.2–0.3 Ǻ). On this account, even in a case of very strong fields (3-4 kG) they must show the simple picture of the Zeeman splitting, with parallel to each other the bisectors of profiles I+V and I – V. In actual fact, another picture was found for nine flares: bisectors of these lines have maximums of splitting on certain distances from line center, what must not be in the homogeneous magnetic field. In particular, both lines have peak of bisector splitting on distance 150–170 mǺ from line center. If we assume the Zeeman nature of named peculiarities then necessary fields are 11.2 kG for FeI 5383 and 10.5-11.2 kG for MgI 5528. Likely, this agreement of field values is a new argument to reality of such very strong magnetic fields in flares

PROGNOSES AND ANOMALY OF 24TH CYCLE OF SOLAR ACTIVITY

Development of solar activity in 24th cycle has specific peculiarity  – non-monotonous increasing of solar activity on grown phase which occurs for 1/3 number of all cycles. The modification of Waldmayer’s method was applied for forecasting 24th cycle which bases on a connection between maximum sunspot number and speed of increasing of activity on grown phase of cycle.  If we compare 24th cycle with previous similar cycles Nos. 1, 5, 6, 9, 12, 15 and 16, we can conclude that this cycle will be weak, with maximum sunspot number Wmax  (24)  =  73  ±  10  in 2014–2015, most  likely –  in  first half of 2014. Current cycle could be considered as anomaly by three criterions:  a) sharp slowdown in growth after the 30th of the month cycle, b) two-humped peak cycle with a significant predominance of the second peak height and c) the emergence of a giant sunspot with a diameter of about170 Mm. Development of solar activity in 24th cycle has specific peculiarity  – non-monotonous increasing of solar activity on grown phase which occurs for 1/3 number of all cycles. The modification of Waldmayer’s method was applied for forecasting 24th cycle which bases on a connection between maximum sunspot number and speed of increasing of activity on grown phase of cycle.  If we compare 24th cycle with previous similar cycles Nos. 1, 5, 6, 9, 12, 15 and 16, we can conclude that this cycle will be weak, with maximum sunspot number Wmax  (24)  =  73  ±  10  in 2014–2015, most  likely –  in  first half of 2014. Current cycle could be considered as anomaly by three criterions:  a) sharp slowdown in growth after the 30th of the month cycle, b) two-humped peak cycle with a significant predominance of the second peak height and c) the emergence of a giant sunspot with a diameter of about 170 Mm

ON THE POSSIBLE EXISTENCE OF SUPERSTRONG MAGNETIC FIELDS IN A LIMB SOLAR FLARE

We present the simultaneousobservations of the K Ca II 3933.7 Å, H δ 4101.7 Å andHe I 4471.5 Å lines in the limb solar flare of July 17,1981. For two moments of the flare we analyzed StokesI ± V and V profiles of these lines from observationsmade on the Echelle spectrograph of the horizontal solartelescope of the Astronomical Observatory of TarasShevchenko National University of Kiev. In the flashphase of the flare, all named lines had very wideemissions, with a wing length of 6–8 Å. An interestingfeature was observed in the violet wings of these lines,namely, narrow emission peaks with a width of only 0.25–0.35 Å. The Zeeman splitting of these emission peakscorrespond to magnetic field strength in range 1300-2900G at altitudes of 10–15 Mm above the level of thephotosphere. Magnetic fields of ‘kilogauss’ range (up to3200 G) were found for some locations also in post-peakphase of the flare. Likely, the true local magnetic fields inthe flare could be even larger, since the obtained resultsrepresent a longitudinal component of the magnetic fieldassuming that the filling factor equals unity. A newindication of the existence of superstrong magnetic fieldsfollows from a comparison of the kinetic temperatures andturbulent velocities found from the narrow emissioncomponent in the flash phase of the flare. Considering thisemission component to be optically thin, we found thatthere is an anti-correlation between temperature andturbulent velocity. Such a dependence seems unlikely and,possibly, the widths of the line profiles reflect, in our case,not turbulent velocities, but very strong magnetic fields.The corresponding estimates of the magnetic field by theK Ca II line lead to the value B = 8.3 kG, and by the He I4471.5 line - to the value B = 6.7 kG. Considering that theHe I line is clearly closer to the case of an optically thinlayer, the closeness of these estimates is very encouraging.Our results are apparently the first indications ofsuperstrong magnetic fields of 6-7 kG at an altitude ofabout 10 Mm in a solar flar

SIMULTANEOUS MAGNETIC FIELD MEASUREMENTS IN SUNSPOTS USING SPECTRAL LINES WITH DIFFERENT LANDE FACTORS

We present magnetic field measurements in several sunspots observed in June-July 2015 on Horizontal Solar Telescope ATsU-5 of Main Astronomical Observatory of National Academy of Sciences of Ukraine. The Zeeman splittings were measured using I ± V profiles of about ten spectral lines of Mn I, Fe I and Ni I including three lines with negative Lande factors, namely Fe I 5434.527 Å, Fe I 6094.419 Å and Fe I 4995.411 Å ( geff = – 0.014, – 0.218, and – 0.25, respectively). Our main conclusions are the following: a) as rule, spectral lines with largest Lande factors give the strongest measured magnetic fields Bobs in sunspot umbra that can be interpreted as a result of blending the Zeeman π- and σ-components in case of non-longitudinal magnetic field. b) in some places of sunspots, Bobs differs also for lines with close Lande factors, e.g. by Fe I 5432.950 and Ni I 5435.871 (geff = 0.67 and 0.5, respectively). c) lines Fe I 6094.419 Å and Fe I 4995.411 Å with geff < 0 have in sunspots signs of splitting which corresponds to geff > 0. The possible causes of named effects are discussed in short form

SIMULTANEOUS MAGNETIC FIELD MEASUREMENTS IN SUNSPOTS USING SPECTRAL LINES WITH DIFFERENT LANDE FACTORS

We present magnetic field measurements in several sunspots observed in June-July 2015 on Horizontal Solar Telescope ATsU-5 of Main Astronomical Observatory of National Academy of Sciences of Ukraine. The Zeeman splittings were measured using I ± V profiles of about ten spectral lines of Mn I, Fe I and Ni I including three lines with negative Lande factors, namely Fe I 5434.527 Å, Fe I 6094.419 Å and Fe I 4995.411 Å ( geff = – 0.014, – 0.218, and – 0.25, respectively). Our main conclusions are the following: a) as rule, spectral lines with largest Lande factors give the strongest measured magnetic fields Bobs in sunspot umbra that can be interpreted as a result of blending the Zeeman π- and σ-components in case of non-longitudinal magnetic field. b) in some places of sunspots, Bobs differs also for lines with close Lande factors, e.g. by Fe I 5432.950 and Ni I 5435.871 (geff = 0.67 and 0.5, respectively). c) lines Fe I 6094.419 Å and Fe I 4995.411 Å with geff < 0 have in sunspots signs of splitting which corresponds to geff > 0. The possible causes of named effects are discussed in short form

ANOMALOUS WIDENING OF 5434.5 LINE IN SUNSPOTS: SUPER-STRONG MAGNETIC FIELDS?

We present results of spectralobservations of two sunspots in six metal lines near Fe I5434.5 Å, which have effective Lande factors g eff from –0.014 to 2.14. The observations were made on July 8 andAugust 25, 2015, with the ATsU-5 telescope of GAO NASof Ukraine using a circular polarization analyzer andspectra registration with the SBIG ST-8300 CCD camera.The following line parameters are compared: observedsplitting of I ± V profiles, the width and depth of the StokesI profiles. Significant differences of the measured magneticfield strengths B eff were found in separate places of thespots and by lines with different g eff values. The Fe I 5434.5Ǻ line (g eff = –0.014) shows measurable splitting in somelocations of the sunspots, which corresponds to themagnetic field B obs ≈ 20 kG. Comparison of the widths anddepths of the line profiles revealed several special places inthe sunspots, where the Fe I 5434.5 Ǻ line was expandedadditionally by ≈ 15–35%, whereas other lines with largerLande factors did not have such a feature. One of thereasons for this expansion could be a sharp and localincrease of turbulent velocities, but no active processes suchas solar flares or significant Doppler flows were observed atthese locations. A semi-empirical model constructed for thefirst sunspot by FeI 5434.5 line using inverse code withTikhonov`s stabilizers shows an anomalous feature – themaximum of microturbulent velocities in the upperphotosphere and the temperature minimum zone instead ofthe usual small increase of microturbulence at these heights.This may be the effect of very strong magnetic fields ofmixed polarity or unresolved turbulent structures. As to firstcase, the estimated value of the magnetic field in suchlocations of sunspots is ~10 5 G, which requires additionalcareful verification

Analysis of the structure - anticancer activity relationship in a set of Schiff bases of macrocyclic 2,6-bis(2- and 4-formylaryloxymethyl)pyridines.

Quantitative estimation of the structure - anticancer activity relationship in a series of macrocyclic Schiff bases of 2,6-bis(formylaryloxymethyl)pyridines was carried out by the topological approach. Correlation equations describing the relationship between the anticancer activity and structural parameters of the molecules studied and descriptors characterizing their structure were obtained on the basis of in vitro screening data. The influence of structure of the investigated substances as reflected by the parameters studied on the anticancer activity, was established