The
Physics of Sun and Star Spots
Proceedings
IAU Symposium No. 273, 2010
D.P.
Choudhary & K.G. Strassmeier, eds.
_c International Astronomical Union
2011
doi:10.1017/S1743921311015699
Are
the umbral dots, penumbral grains, and
G
band bright points formed by the same
type
of magnetic flux tubes?
Isroil Sattarov
Tashkent
State Pedagogical University, 103 Yusif Kxos Kxojib str.,Tashkent 100070,
Uzbekistan
email:
isattar@astrin.uz
Abstract.
Today’s Solar
Physics comes across of different type of fine structures in solar atmosphere
including
umbral dots and penumbral grains in sunspots, and G-band bright points in
quiet
Sun. In this report, we present evidence that umbral dots, penumbral grains,
and, possibly,
G
band bright points are related to a common type of features in solar atmosphere
magnetic
flux
tubes.
Keywords.
Umbral dots,
penumbral grains, sunspots, G-band bright points
1. Introduction
Stratospheric
balloon-borne observations of sunspots in USA under leadership of M.
Schwarzchild
in 1959 (Danielson 1964), and balloon experiments in USSR under leadership
of
V. Krat (Krat et
al. 1972) excited
great interest and put forward many problems
in
physics of sunspot fine structure. The mechanism of emergence of so-called
umbral
dots,
their relation with penumbral filaments are examples of questions raised by
these
observations.
These earlier stratospheric observations had turned out to be insufficient
for
study the dots evolution, which require long-term observations; and the author
was
among
the first observers, who begun studying the sunspots’ fine structure using
groundbased
telescopes.
Today’s Solar Physics comes across different types of fine structures in
solar
atmosphere. In this report we present evidence to support that umbral dots,
penumbral
grains,
and, possibly, G-band bright points are related to the same type of features
magnetic
flux tubes in solar atmosphere.
2. The
telescope and observations
Horizontal
solar telescope ATSU-5 used by us is one of the serial instruments (D=44
cm,
F=1700 cm, where D is diameter of main mirror, and F is its focal length)
developed
by
Russian optician V.N. Ponamarev 55 years ago. Ten years later, the majority of
Soviet
Union
observatories were equipped with such telescopes. In 1964, ATSU-5 telescope was
mounted
in Tashkent Astronomical Observatory in the city of Tashkent. The territory of
Uzbekistan
is very sunny. In Tashkent, the average sunshine time is near 2900 hours per a
year
with a consistently very good seeing from June 20 to the beginning of October.
The
very
good seeing takes place during windless and hot weather, frequently for several
days
before
a cyclone. White light observations of sunspots, discussed in this article,
were
carried
out in Cassegrain focus (diameter of solar disk is 60 cm) using high-speed 35
mm
photographic camera (exposure time 0.01 sec). Bursts of images were taken
during
the
periods of best seeing, based on visual control by the observer (the author of
this
article). Spectral observations were
conducted in Newton (prime) focus of the telescope
IAU273: Umbral dots, penumbral grains, and
G band bright points
Figure
1. Two prints (a
0650 UT, b 0828 UT) of umbra of the unipolar sunspot observed 8 August
1981
at the ATSU-5 in Tashkent. Vertical touch on Fig. 1b shows position of
spectrograph’s
slit at receiving spectrum presented on
Fig. 3.
Figure
2. Drawing of
penumbral grains and umbral dots (short filigree) of the large sunspot
exhibiting
counter-clockwise rotation for 14(a), 15(b) and 16(c) September 1977.
using
ASP-20 horizontal spectrograph with linear dispersion of 0.6 ˚A / mm at optical
wavelength.
The spectra were recorded using photographic plates and film with exposure
time
of 1-3 seconds. The observations were used to study the magnetic field, fine
structure
and
evolution penumbral filaments and umbral dots.
3. The results
of sunspots fine structure studies
It
was found that in most studied cases the umbral dots persist for more than 30
minute:
43 % of dots persist more than 60 minutes and 10% - more than 90 minutes.
In
their evolution, bright dots increase the brightness reaching the maximum
during a
relativity
short time, and after that, gradually become weaker and expand. Finally, the
dots
break up and disappear (Sattarov 1981a). Most of bright dots are observed at
the
disk
center side of penumbra umbra boundary (as in right side of umbra on Fig. 1 b).
In
September 1977, a rotation of an unipolar sunspot with two umbrae (small
northern
and
large southern umbra) was observed. During 13-16 September the spot rotated
by
700 around its northern small umbra in counter-clockwise direction. The
rotation
affected
the orientation of penumbral filaments (grains) and umbral fine structure,
twisting
them
in clockwise direction. In the course of rotation, the main (large) umbra was
deformed;
its east boundary was “attacked” by brushes of penumbral grains, which appear
as
“peninsula” intruding into the umbra. The dots in front of “peninsula” were
transformed
into the bright penumbral grains. On the west boundary of main umbra,
the
opposite affect took place, i.e. the penumbral west boundary joined the umbra
and
the
bright penumbral grains turned into the umbral dots (Sattarov 1981b). It
appears
that
the magnetic flux tube that forms the large unipolar sunspot rotates, indeed.
The
rotation
may be caused by interaction of the magnetic tube forming unipolar sunspot
and
the magnetic tubes of new sunspot group developed near the southern boundary
of
the penumbra of unipolar sunspot. The magnetic field of sunspot had southern
(S)
polarity,
and the sunspot of leading (N) polarity of this new group had developed near
it
later (Sattarov 1981b). Between the white light observations we took
spectrograms of
sunspots by scanning their umbrae in
selected (narrow or wide) spectral bands. In the
Sattarov
Figure
3. A part of the
central section (noted in Fig. 1b by vertical stroke) spectrum with the
line
Fe I 6302.5 of the umbra printed on Fig. 1.
spectrograms
we have identified individual bright points or their clusters. It was found
that
the magnetic field in umbral dots (or clusters of them) is more longitudinal
than
the
field strength in the darkest regions of umbra. The field strength in umbral
dots is
about
20% lower than the field strength in the darkest regions of umbra (Sattarov
1982,
Litvinov
& Sattarov 1989).
As
one can see on Fig. 3 spatial resolution of spectral observations is lower than
the
resolution
of the white light images (compare Fig. 1 with Fig. 3). It is the result of
blurring
effect,
which is larger near the boundary of umbra. In our estimate, the contribution
of
scatter
light in brightness of sunspot is not significant. Fig. 3 shows the spectral
line Fe I
6302.5
with telluric lines of both sides. On Fig. 3, one can see the simple doublet
Zeeman
splitting
(middle white band on Fig. 3) on bright dot’s cluster (Fig. 1b). If the scatted
light
was strong, we would see strong central component, which is not present on the
middle
white band. The observations of clusters of dots do not show measurable Doppler
displacement.
This implies that if there were plasma flows in dots the velocity of these
flows
should not exceed 100 m/s (Litvinov & Sattarov 1989).
4. Discussion
and conclusions
Bright
dots were observed near the disk side of penumbra-umbra boundary in the
“intrusion”
of
penumbral material into the umbra. Rotation of the sunspot had transformed
umbral
dots into penumbral grains and penumbral grains into umbral dots. Umbral dots
are
associated with vertical magnetic tubes and, it seems, the rotation deflected
umbral
dots
flux tubes from its vertical direction to more horizontal orientation prior to
formation
of
penumbral peninsula in umbra. Magnetic field in penumbral grain flux tubes have
more
horizontal direction and sunspot rotation had deflected penumbral flux tubes on
the
opposite (limb) side of the umbra from its horizontal direction to more
vertical position.
Umbral
dots and penumbral grains are the very small structural elements of solar
atmosphere.
The movie of a newly developing sunspot (Fig. 4 presents one of images of
this
movie) shows how the penumbral grains are formed. They develop in intergranular
spaces
from low contrast small photosphere features (it seems, from photosphere bright
points),
but not from granules themselves. Plasma flow velocities in umbral dots are
as
small as in intergranular spaces in the photosphere(Litvinov & Sattarov
1989, Lites
et
al. 1991). The
umbral dots live longer than the photospheric granules, and it seems
they
may have a different mechanism of flaring up than granulation As it appears
from
our
study, the granules cannot transform to the penumbral grains (as was suggested
by
some
models of sunspot penumbra). The granules show plasma flows of sufficiently
larger
velocity
directed vertically upward, whereas the dots have not show such strong plasma
flows.
Intergranular lanes exhibit bright points - a very small structural element of
solar
atmosphere. A sunspot movie (Nemirooff
& Bonnel 2000) shows how the formation of
IAU273: Umbral dots, penumbral grains, and
G band bright points
Figure
4. Small new sunspot
observed at 8 August 1981 in ATSU-5 in Tashkent.
grains
and photosphere bright points takes place near outside boundary of penumbra;
both
features go away: the grains move to umbra, while the bright points move to the
surrounding
photosphere. The grains and the bright points have opposite magnetic polarity.
On
sunspot images of low resolution the grains present inner and the photosphere
bright
points outer rings of Secchi. Therefore, we propose that the umbral dots,
penumbral
grains,
and photosphere bright points are associated with the feature - magnetic flux
tubes
- which float to the solar surface in outside parts of sunspot penumbra.
Acknowledgments
The
presentation of this paper in the IAU Symposium 273 was possible due to partial
support
from the National Science Foundation grant numbers ATM 0548260, AST
0968672
and NASA - Living With a Star grant number 09-LWSTRT09-0039.
References
Danielson,
R. E. 1964, Astrophys.
J. 139, 45
Krat,
V. A., Karpinsky, V. N., & Pravdjuk, L. M. 1972, Solar Phys. 26, 305
Sattarov,
I. 1981a, Morphology
and Cyclicity of Solar Activity, 122
Sattarov,
I. 1981b, Morphology
and Cyclicity of Solar Activity, 107
Sattarov,
I. 1982, Sun and
Planetary System, 96,
129
Sattarov,
I. 1980, Soviet
Astron. 24, 352
Litvinov,
O.V., & Sattarov, I. 1989,Magnetic Fields and Corona, (Moscow, Nauka), 210
Lites,
B. W., Bida, T. A., Johannesson, A., & Scharmer, G. B. 1991, Astrophys. J. 373, 683
Nemirooff, R.& Bonnel, J. 2000,
Astronomy Picture Of the Day, 23/02/2000.
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