Исследования Солнца. Публикации
Akimov
L.A., Beletsky S.A., Dyatel N.P. (1998)
The chromospheric D3 helium emission observed at the total
solar eclipse of July 31, 1981 // Astroph. And Sp.
Sc. -1998- V.252
The
digital images of 350 eclipse chromospheric spectra obtained with
a special automatic photometer have been used to construct the
image of the D3 HeI chromosphere over the range of 36°N - 42°S
in latitude. The chromospheric emission comes from two very irregular
layers with peaks of the intensities at the heights of 1100 -
1700 km for the layer with the dominant emission, and at the height
of around 300 km for the lower layer. The distribution of the
surface brightness averaged over all measured latitudes (36°N
- 42°S) versus height also reveals two peaks. The energy emitted
by the upper layer is determined to be 7 times larger than that
emitted by the lower one. The chromospheric D3 emission is well
correlated with the emission of the green corona (503.3 nm) at
low heights. The correlation disappears at heights more than 1500
km. The chromosphere above active regions and spots is lowered.
It is supposed that such behaviour is affected by large scale
magnetic fields of the Sun and by structural elements, such as
spicules and fibrils.
Akimov
L.A., Beletsky S.A., Dyatel N.P. (1998)
On the helium emission in the lower chromosphere. // UAA Information
bulletin, N12, 1998, p.34.
Akimov
L.A., Beletsky S.A., Dyatel N.P. (1999) The chromospheric
D3 helium emission observed at the total solar eclipse of July
31, 1981 // Astronomical and astrophysical transections.
-1999- V.18(1), p. 253-260.
The
digital images of 350 eclipse chromospheric spectra obtained with
a special automatic photometer have been used to construct the
image of the D3 HeI chromosphere over the range of 36°N - 42°S
in latitude. The chromospheric emission comes from two very irregular
layers with peaks of the intensities at the heights of 1100 -
1700 km for the layer with the dominant emission, and at the height
of around 300 km for the lower layer. The distribution of the
surface brightness averaged over all measured latitudes (36°N
- 42°S) versus height also reveals two peaks. The energy emitted
by the upper layer is determined to be 7 times larger than that
emitted by the lower one. The chromospheric D3 emission is well
correlated with the emission of the green corona (503.3 nm) at
low heights. The correlation disappears at heights more than 1500
km. The chromosphere above active regions and spots is lowered.
It is supposed that such behaviour is affected by large scale
magnetic fields of the Sun and by structural elements, such as
spicules and fibrils.
Акимов
Л.А., Белкина И.Л., Белецкий С.А., Дятел Н.П. (2000)
Хромосфера Солнца в линии D3 HeI по наблюдениям полных солнечных
затмений ч.1 Построение изображения хромосферы Солнца в спектральных
линиях // Кинематика и физика небесных тел, в печати.
Beletsky
S.A., Bushueva T.P.(1998)
DIGITIZED IMAGES FOR SOLAR ACTIVITY PATROL AT THE KHARKOV ST.
UNIVERSITY ASTRONOMICAL OBSERVATORY //
Izv. KRAO V. 94, Crimea 1998, p.190-192.
Белецкий
С.А., Бушуева Т.П. Использование цифровых изображений для
патрульных наблюдений солнечной активности в Астрономической обсерватории
Харьковского Университета // Известия КрАО т. 94, Крым
1998 с.190-192.
It
is described the digitized images usage for solar activity patrol.
The advantage of the CCD-observation as compared with the photographic
ones is shown by examples of the active processes research in
1993-1994.
Belkina
I.L, Beletsky S.A., Gretsky A.M., Korokhin V.V., Marchenko G.P.
(1994)
Solar
activity monitoring experience with CCD-photometer. (abstr.)
conf. Physics of Moon and planets.-1994.-p.18-21.
Белкина
И.Л., Белецкий С.А., Грецкий А.М., Корохин В.В., Марченко Г.П.
Опыт мониторинга солнечной активности при помощи ПЗС-фотометра
Физика Луны и планет. Тезисы конференции посвященной 100-летию
со дня рождения академика Н.П. Барабашова.-1994.-с.18-21.
Universal
photometer based on the cooled one-dimensional CCD followed by
computer was constructed at Kharkov St. University Astronomical
observatory. It was used to image the solar chromosphere at H
HI, K CaII lines and IR HeI 1083 nm line July - August 1993 observations.
The reasons leading to appearance such distorting effects as interference
and others in the monochromatic observations with CCD -photometer
are analysed. The observational method and data processing algorithms
are proposed. The images so obtained contain the photometric information
about the flares and high-speed processes in chromosphere.
Белкина
И.Л., Белецкий С.А., Грецкий А.М., Корохин В.В.,Марченко Г.П.
(1995)
О возможносити применения диодной линейки на основе кремния
для наблюдений Солнца в линии НеI л=1,083мкм // Тез.док. конф.
Физические явления в твердых телах Харьков 1995, с. 106.
Belkina
I.L., Beletskiy S.A., Gretskij A.M., Marchenko G.P.
(1996)
CCD-observations of the Sun HeI 1083nm, Ha
and K Ca II lines// Kinematika i fizika nebesnyh tel., 1996,
v(t)12, N2,p(s)65-76.
Белкина
И.Л., Белецкий С.А., Грецкий А.М., Марченко Г.П.
ПЗС-наблюдения Солнца в линиях НеI 1083нм, Н-альфа, К СaII.
Кинематика и физика небесных тел.-1996.-т.12, No 2.-с.65-76.
The
digitized monochromatic images of the Sun in HeI 1083nm, Ha and
K CaII are obtained on the spectroheliograph with the CCD photometer
of the Kharkov University Astronomical Observatory. Optical characteristics
of the CCD receiver operating in the monochromatic regime are
studied from optical to the near IR spectral range. We present
the algorithms and software to remove the drawbacks inherent in
this class devices. The Ha
and
K CaII images obtained during 1993 July-Avgust and 1994 June-October
seasons (when chromospheric flares and other nonsteady processes
occurred) were used to determine heliographic positions and intensities
for the solar activity patrol program. The HeI
1083nm image sets were used to study line depth changes during
the development of two chromospheric subflares and accompanying
filaments. These flares were observed in absorption only. The
tangential velocity of propagation of the perturbation in one
of the filaments is evaluated.
Kurochka
L.N., Belkina I.L., Beletskiy S.A., Korokhin V.V., and
Marchenko G.P. (1997)
Observations
and Analysis of Emission from Solar Active Regions at the Edge
of Balmer Continuum. //Astronomicheskiy
Zhurnal., 1997, v(t)74, N3,p(s)460-465.
Курочка
Л.Н., Белкина И.Л., Белецкий С.А., Корохин В.В., Марченко Г.П.
Наблюдения
и анализ излучения активных областей на Солнце у границы бальмеровского
континуума.
Астрон. журнал. 1997. т.74. N 2. с.460-465.
The
first results of CCD observations of the Sun in Balmer and Pashen
continua and in the Balmer precontinuum are presented. The intensity
distribution in the Balmer precontinuum in a knot of the active
region NOAA/USAF 7890 provides information about inhomogeneities
in the electron density of the plasma along the sight line. The
value of conductiong monitoring observations of this kind is argued.
Kurochka
L.N. , Belkina I.L, Beletsky S.A., Korokhin V.V., Marchenko G.P.
(1999)
CCD- observations of the Sun in the Balmer and Pashen continue
// Astronomical and astrophysical transections. -1999- V.18(1),
p. 265-272.
The
first results of new kind observations in the Balmer and Pashen
series continua and Balmer precontinuum are presented. Such observations
will provide a valuable informations about Ne-irregulaties, processes
occuring in the a.r. and formation here of areas with the enhaced
plasma density.
Акимов
Л.А., Белецкий С.А., Белкина И.Л., Дятел Н.П. (2000) Вариации
интенсивности свечения солнечной хромосферы в линии D3 с циклом
солнечной активности по затменным наблюдениям // Астрономия
2000 года: Матер. конф., Одесса, 2000г.- Одесса, 2000.-С. 4.
Белкина
И.Л., Акимов Л.А., Белецкий С.А., Корохин В.В., Марченко Г.П.
(2000) Экваториальные
корональные дыры по наблюдениям в крыльях линии HeI 1083 нм //
Кинем. и физ. неб. тел.-2000.-Т.16, № 4. -С.316-323.
Belkina I.L., Akimov
L.A., Beletsky S.A., Korokhin V.V., Marchenko G.P. EQUATORIAL
CORONAL HOLES FROM THE OBSERVATIONS AT HeI l 1083 НМ WINGS
// Kinematika i Fizika Nebeshykh Tel.-2000.- V. 16, No
4.-P. 316-323.
The
average intensities of areas in the blue and red wings of HeI
1083nm line for equatorial coronal holes (CH) and unipolar quit
regions are determined from solar CCD images which have been taken
at ±0.05nm from the line centre in 1995 and 1999. These data were
used for the evaluation of average doppler line shift, which is
caused by the presence presence of outflows from CH (Dlh) and
unipolar quit regions (Dlq). The value Dlh = -0.0032нм (sm=0.0002)
was received for 105 CH areas; the value Dlq=-0.0012A (sm=0.0002)
was received for 41 unipolar quit regions. This result is indicative
the significant difference beetween CH and quit regions in the
size of average stream velocity of outflow. It means that the
solar wind from CH starts to accelerate from the middle chromosphere.
Taking into account the existense of the fine structure elemets
in CH with radial outflow speed of 8km/s, we found that these
elements are covering about 10% of the whole CH area. Tendency
of |Dlh | increasing at a period near maximum of solar activity
is noted.
Белецкий С.А.
(2000) Результаты
исследований солнечной хромосферы в линиях гелия D3 и 1083 нм.
- дис. канд.физ.-мат. наук: 01.03.03 (рукопись).- Харьков, 2000.-157с.
Beletsky S. A.
Results of solar chromosphere recearch in D3 and 1083 nm
lines.- Manuscript. Thesis for a candidates degree by specialty
01.03.03 - Heliophysics and Physics of Solar System. Kharkov,
2000.-p.157.
The
dissertation is devoted to the study of the solar chromosphere
from the spectroheliograms recorded in HeI 1083 nm line and from
the slitless cinematographic observations of solar eclipses in
D3 helium line. For the first time the chromospheric D3 surface
brightness distribution along the whole observed part of the solar
limb is received from the results of two eclipse observations.
The maximum of the chromosphere brightness distribution near the
limb was for the first time discovered to be located at the heights
less than 500 km for a considerable part of the solar limb. From
the study of the 1083 nm spectroheliograms the solar wind from
the coronal holes was shown to accelerate from the middle chromosphere.
The results of observations of 3 flares have shown that a relation
between the flare regions in the chromosphere and the "hidden"
activity centres located in the corona can be found from the 1083
nm line observations.
Key words: Sun, chromosphere, coronal holes, eclipse, helium,
concentration.
Акимов Л.А., Белкина
И.Л., Белецкий С.А., Дятел Н.П. (2002)
Структура и эмиссия солнечной хромосферы в линии D3 HeI по наблюдениям
полных солнечных затмений.//
Кинем. и физ. неб. тел.-2002.-Т.18, № xx. -С.xxx-xxx.
Akimov L.A., Belkina
I.L., Beletsky S.A., Dyatel N.P. The structure and the
emission of the solar chromosphere at the helium D3 line from
the total solar eclipses. // Kinematika i Fizika Nebeshykh
Tel.-2002.- V. 18, No xx.-P. xxx-xxx.
Maps
of the chromospheric emission at the helium D3 line as functions
of heliographic latitude and height obtained from cinematographic
observations of the total solar eclipses 1972 July 10 and 1981
July 31 are presented. It is discovered that the helium emission
is observed in separate features with the characteristic size
of the supergranule of 20000-30000km along the limb mainly. The
features with the maximum concentration near the height of 1400km
are extended to 3000-4000km. These are present at the base of
the chromosphere also, therefore the surface brightness height
distributions are reveal two peaks at the heights about 1400 and
250km.
The energy emitted by the chromosphere over the height range of
the lower maximum is about 5% and 10% of the total energy emitted
by the chromosphere at the D3 line for the eclipses of 1972 and
1981 respectively.
It is found that the integral brightness of the quiet chromosphere
for the eclipse of 1981 was twice the 1972 eclipse one. It is
connected with the sunspot cycle different phases for the every
eclipse.
For the inhomogeneous chromosphere it is shown the helium emission
at the height range of the temperature minimum can be explained
by the penetration of the coronal radiation with l< 6 nm to
these heights.
Белкина И.Л., Акимов Л.А., Белецкий С.А. (2002)
Активные процессы на Солнце по наблюдениям в линии НеI 1083 нм
// Тез. конф. "Активные процессы в Солнце и звездах",
СПб, 1-6 июля 2002 года.
Корохин
В.В., Белецкий С.А., Белкина И.Л., Великодский Ю.И., Марченко
Г.П. (2002)
Применение ПЗС-матрицы для спектрогелиографических
наблюдений // Тез. крымской конф."Солнечная активность
и параметры ее прогноза" 3 - 8 июня 2002 г. Научный, Крым,
Украина.
Акимов
Л.А., Белкина И.Л., Бушуева Т.П. (2002) Вспышечные
индексы солнечной активности в рентгеновском и оптическом диапазоне
в 22 и 23 циклах // Тез. крымской конф."Солнечная активность
и параметры ее прогноза" 3 - 8 июня 2002 г. Научный, Крым,
Украина.
Александров
Ю.В., Белкина И.Л., Грецкий А.М. (2002) О
возможном влиянии некоторых геофизических и гелиофизических факторов
на возникновение аварий при глубоком газовом бурении // Тез.
крымской конф."Солнечная активность и параметры ее прогноза"
3-8 июня 2002 г. Научный, Крым, Украина.
2002/06/08