of the Programs IHY-2007 and IYA-

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The astronomical researches in Uzbekistan
and activities in a frame

of the Programs IHY
-
2007 and IYA
-
2009 ”


Ibragimov I.A., Egamberdiev Sh.A.



The Astronomical
Institute,

Uzbekistan Academy of Science

UN/ESA/NASA/JAXA Workshop on

Basic Space Science and


the International Heliophysical Year
2007


21
-
25
September
2009
, Daejeon, Republic of Korea




Ulughbek

Astronomical

Institute

of

the

Uzbek

Academy

of

Sciences

is

the

oldest

scientific

institution

not

only

in

Uzbekistan

but

in

the

whole

Central

Asia

as

well
.




It

was

founded

in

Tashkent

in

1873

and

was

known

as

one

of

important

astrometry

center

in

the

world
.

Since

the

end

of

the

19
th

century

UzAI

was

involved

to

the

International

Latitude

Service
.


Fields of our activity are
:



Scientific:

helio
-

and astroseismology, planets and

asteroids, non
-
stationary stars, stars formations, stars

clusters’ dynamics in our galaxy, nuclei of active

galaxies, quasars and X
-
and gamma
-

radiation sources,

gravitational lenses and theoretical relativistic astrophysics.

Education
at the National University and at the affiliations

in the regions.

Popularization
of the astronomy

among scholars,

students and amateurs.

International

scientific cooperation.







Astronomical observations in Uzbekistan carry out at the Observatory located on
the mountain Maidanak (2700 m) with high quality atmospheric condition, one of
the best the world.



REPUBLIC OF UZBEKISTAN

Maidanak


Suffa

Satellite image of the Maidanak observatory

Night Time Seeing

Maidanak Observatory:

telescopes and instruments


6 telescopes: 1.5m, 1m, 4x60 cm


5 CCDs: SI 600 Series 4K,


SITe 2000x800,


2x FLI IMG 1K,


SBIG ST9
-
XE 0.5K



Direct imaging and photometry (in optic)
only, no IR, no Sp.


Zeiss
-
1000

ROBOT
-
TELESCOPE (EAST)

1
. Helioseismic and asteroseismic groups



Solar Cycle Variation of p
-
Mode Frequencies
generated by Perturbation in the Solar
Interior



Meridional flow circulation deep in the Solar
interior as seen by GONG+ time distance
analysis


Solar Cycle Variation of p
-
Mode Frequencies
Generated by Perturbation in the Solar Interior



p
-
modes with different
ω
/
l
penetrate to different solar depth (
ω
-
mode’s
frequency,

l
-

spherical degree of the mode)



Magnetic field in solar interior and at solar surface will change frequencies


of p
-
modes

Solar Cycle Variation of p
-
Mode Frequencies
Generated by Perturbation in the Solar Interior


Difference between high
-

and
low
-
phase velocity frequency
shifts are consistent for MDI
and GONG results (except for
1998)


Difference correlated with solar
activity cycle


Comparison of measured
signals and model study in
Chou & Serebryanskiy (2005)
suggests that temporal
variations of the frequency
change corresponds to a
perturbation of
δ
c/c≈2
-
6x10
-
5
at
r≈ 0.65
-
0.67

if the width of
the perturbed region is
0.05 R
.

Meridional flow circulation deep in the Solar
interior as seen by GONG+ time distance
analysis

Travel
-
time

difference

(Δτ)

in

the

meridional

plane

as

a

function

of

latitude,

for

different

depths

using

10
%

of

low
m

coefficients
.

The

five

ranges

of

separation

distances

correspond

to

different

lower

turning

points

(see

legend)
.

Lower

turning

points

for

these

five

ranges

are

0
.
96
,

0
.
90
,

0
.
79
,

0
.
71

and

0
.
64
R

respectively
.

First Results of Asteroseismic Observations at

Maidanak Observatory In Uzbekistan

We performed several campaigns of CCD
-
photometry observations in


2007
-
2009 to

evaluate the possible duration to be achieved and quality of

observations in

Maidanak observatory with existent facilities as well as to

figure

out what can be

done in near future with respect to some feasible

improvements in hardware and software (if necessary) to get higher

quality photometric data. For these

purpose we chose relatively bright

variable

stars (mainly of
δ
Sct type) with known periods and of pulsations.

2
. Investigation and analysis of solar corona, its small
features such as Coronal Bright Points (CBP)

in
Ultraviolet and X
-
ray images of the Sun

An automatic
procedure of
CBPs
identification
was
developed on
the base of
IDL software

Complete cycle
variation
s of CBPs number
(upper curve) vs. sunspot number (lower
curve)


An original automatic procedure of CBPs
identification and a complex of programs for
analysis of CBPs evolution was developed
using Interactive Data Language
-

IDL
.


CBP could be divided on two categories: dim
CBPs associated with quiet Sun and bright
-

active region CBPs
.


Number of

CBPs reached its maximum level (
the same as in
1996
-

previous period of
minimum of solar activity).


Results

3. The study of gravitational lenses and

the forming non
-
stationary galaxies

The aims:




Investigation

of

a

number

of

unique

and

priority

of

gravitationally

lensed

quasars

(GLQ)




Identifying

the

nature

of

the

early

stage

of

formation

of

galaxies

and

some

of

their

substructures
.

SBS1520

Q2237


Einstein Cross


UM673=Q0142

Q
0957

H
14
13

SBS0909

Light curves of GLQ with taking into account time delay and

microlensing events

Deconvolution of RXJ
1131
-
123

Deconvolution of


HS0435
-
1223

Results


Performing

of

multi
-
colour

photometric

observations

of

double

and

quadruple

GLQ

-

Q
2237
+
030
,

H
1413
+
117
,

B
1422
+
237
,

UM
673
,

SBS
1520
+
530
,

PG
1115
+
080
,

etc
.


Analysis

of

the

light

curves

-

calculation

of

the

time

delay,

the

identification

of

microlensing,

the

study

of

the

nature

of

the

radiation

source

and

the

galaxy
-
lens



Construction

of

the

anisotropic

multiparametric

models

of

the

forming

non
-
stationary

galaxies
.


Research

and

analysis

of

gravitational

instability

of

these

models,

the

definition

of

relations

between

physical

parameters

that

lead

to

the

formation

of

various

large
-
scale

structures
.


4
. Asteroids: MBA, NEA, young family

Currently gathered observations on the families:

(
2005
-
2008
,
more then

150
asteroids
,
NAO Japan)



Karin
-

832
,
1998
sq
81
,
10783
,
28271
,
33143
,
79213



Lannini

-
1929
cz,
2000
oh
45
,
2000
oz
7
,
2000
ro
76
,
2001
xg
241
,
2003
af
89
,
2001
pu
35
,
4652
,
81550
, etc.



Veritas
-

1902
jp,
1964
tn
2
,
1975
sb
1
,
1976
us,
1982
an,
1997
ro
7
,
1998
rp
80
,
1998
ry
63
,
1999
xf
8
,
2000
ck
92
,
2000
dm
102
,
2000
ef
148
,
2000
fk
2
, etc.



Datura
-

1270



Koronis
-

10267
,
10534
,
10954
,
11241
,
15195
,
1570
,
16326
,
1762
,
1774
,
1848
,
1894
,
1913
,
1955
,
2051
,
2209
,
2338
,
2574
,
3032
, etc.



Themis
-

1027
,
1259
,
16300
,
1669
,
1729
,
17291
,
18214
,
2009
,
222
,
2297
,
2361
,
2718
,
3008
,
3174
,
3183
,
3358
,
4366
, etc.



Theoretical astrophysics


1
. Research of the group is mainly devoted to the general
-
relativistic electrodynamics of continuous media such as
superconductor, conductor, plasma etc and its application for
theoretical explanation and analysis of electromagnetic and
astrophysical processes in external gravitational fields.



2
. Experimental tests of general relativity, general relativistic
electromagnetic effects and fields for pulsars and magnetized
rotating and oscillating neutron stars are also in our scientific
interests.


3
. The group is also studying solutions of field equations,
particle motion and electromagnetic fields and waves around
compact gravitating objects.




We also focus on space weather applications:



1
. R
adio transparency, its variation and correlation
with meteoparameters and active processes on the
Sun and
in
heliosphere

(
at the plateau Suffa)


2
. Ionosphere investigation is carry out with the
VLF
-
receiver supplied by the Stanford University
under IHY
-
2007
. This equipment provides
monitoring of the ionosphere over the territory of
Tashkent on the permanent basis.

Radio observatory at the plateau Suffa

70 m radiotelescope in mm range

AWESOME

A
tmospheric

W
eather

E
lectromagnetic

S
ystem for

O
bservation

M
odeling and

E
ducation

Tashkent VLF receiver (May, 2008)


The receiver consists of GPS antenna, VLF antenna,
the block of the preliminary amplifier, the block of the
linear receiver.



Research of acting signals allows to make the
qualitative physical analysis of the electromagnetic
phenomena in bottom D
-

a layer of an ionosphere
and in prospect will allows to define ionospheric
precursors of the seismic phenomena.



First results were discussed at the International
Workshop “Advancing VLF Science through the
Global AWESOME Network” in Tunis, Tunisia,


30.05


01.06
,
2009
.


Suffa

Maidanak

Parkent

Kitab

Affiliations astronomy centers

under leadership of the Astronomical Institute

Educational
-
Scientific Observatory is also operating at
the Samarkand State University
-

in the Motherland of
the great astronomer Ulughbek
.

Parkent (
1100
m) Solar furnace

In the frame of the IYA
-
2009 Program:





The International Conference “Mirzo Ulughbek and his
contribution to the development of the

World Science
"
was organized

in

Samarkand,

9
-
11
June, 2009.



The Museum of astronomic instruments of the 18
-
19th
century with unique instruments and appliances have been
created in the Astronomical Institute this year.



The training astronomical Seminar for university
lecturers and students Uzbekistan was organized by UzAI
in April 2009.



Every week we organize open lectures and excursions
for scholars, students and amateurs in the Astronomical
Institute.

Ulughbek Observatory in Samarkand


Museum of the Astronomical Institute

Telescopes of the
18
th Century

Our International Links



Astronomical Institute of Moscow University (Russia)


Astrophysical Institute of Potsdam (Germany)


Van Vlec Observatory of Wesleyan University (USA)


Harvard
-
Smithsonian Center for Astrophysics (USA)


Stanford University (USA)


Grenoble Observatory of J. Fourier University (France)


University de Nice (France)


National Astronomical Observatory (Japan)


Astronomical Institute of Amsterdam University (Holland)


Astrophysical Laboratory of National Tsing Hua University
(Taiwan)


Astronomical Consortium of Korean Universities (Korea)


Coming together is the beginning. Keeping together is progress.

Working together is success. Henry Ford



We are open for new scientific cooperation

and collaborations



Thank you