The astronomical researches in Uzbekistan The astronomical researches in Uzbekistan and activities in a frame and activities in a frame

of the Programs IHY-2007 and IYA-2009 ”of the Programs IHY-2007 and IYA-2009 ”

Ibragimov I.A., Egamberdiev Sh.A.Ibragimov I.A., Egamberdiev Sh.A.

The Astronomical The Astronomical Institute, Institute, Uzbekistan Academy of ScienceUzbekistan Academy of Science

UN/ESA/NASA/JAXA Workshop on UN/ESA/NASA/JAXA Workshop on Basic Space Science andBasic Space Science and

the International Heliophysical Year 2007 the International Heliophysical Year 2007 21-25 September 2009, Daejeon, Republic of Korea21-25 September 2009, Daejeon, Republic of Korea

Ulughbek Astronomical Institute of the Ulughbek Astronomical Institute of the Uzbek Academy of Sciences is the oldest Uzbek Academy of Sciences is the oldest scientific institution not only in scientific institution not only in Uzbekistan but in the whole Central Asia Uzbekistan but in the whole Central Asia as well. as well.

It was founded in Tashkent in 1873 and It was founded in Tashkent in 1873 and was known as one of important was known as one of important astrometry center in the world. Since the astrometry center in the world. Since the end of the 19end of the 19thth century UzAI was involved century UzAI was involved to the International Latitude Service. to the International Latitude Service.

Fields of our activity areFields of our activity are::

Scientific:Scientific: helio- and astroseismology, planets and helio- and astroseismology, planets andasteroids, non-stationary stars, stars formations, stars asteroids, non-stationary stars, stars formations, stars clusters’ dynamics in our galaxy, nuclei of active clusters’ dynamics in our galaxy, nuclei of active galaxies, quasars and X-and gamma- radiation sources, galaxies, quasars and X-and gamma- radiation sources, gravitational lenses and theoretical relativistic astrophysics. gravitational lenses and theoretical relativistic astrophysics. Education Education at the National University and at the affiliationsat the National University and at the affiliationsin the regions.in the regions.Popularization Popularization of the astronomyof the astronomy among scholars, among scholars, students and amateurs. students and amateurs. InternationalInternational scientific cooperation. scientific cooperation.

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

the best the world.the best the world.

REPUBLIC OF UZBEKISTAN

Maidanak

Suffa

Satellite image of the Maidanak observatorySatellite image of the Maidanak observatory

Night Time Seeing

Maidanak Observatory:Maidanak Observatory:telescopes and instrumentstelescopes and instruments

6 telescopes: 1.5m, 1m, 4x60 cm6 telescopes: 1.5m, 1m, 4x60 cm

5 CCDs: SI 600 Series 4K, 5 CCDs: SI 600 Series 4K,

SITe 2000x800, SITe 2000x800,

2x FLI IMG 1K,2x FLI IMG 1K,

SBIG ST9-XE 0.5KSBIG ST9-XE 0.5K

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

Zeiss-1000Zeiss-1000

ROBOT-TELESCOPE (EAST)ROBOT-TELESCOPE (EAST)

1. Helioseismic and asteroseismic groups1. Helioseismic and asteroseismic groups

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

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

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

p-modes with different p-modes with different ωω//l l penetrate to different solar depth (penetrate to different solar depth (ωω-mode’s -mode’s frequency, frequency, l- l- spherical degree of the mode) spherical degree of the mode) Magnetic field in solar interior and at solar surface will change frequencies Magnetic field in solar interior and at solar surface will change frequencies of p-modesof p-modes

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

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

Difference correlated with solar Difference correlated with solar activity cycleactivity cycle

Comparison of measured Comparison of measured signals and model study in signals and model study in Chou & Serebryanskiy (2005) Chou & Serebryanskiy (2005) suggests that temporal suggests that temporal variations of the frequency variations of the frequency change corresponds to a change corresponds to a perturbation of perturbation of δδc/c≈2-6x10-5 c/c≈2-6x10-5 at at r≈ 0.65-0.67r≈ 0.65-0.67 if the width of if the width of the perturbed region is the perturbed region is 0.05 R0.05 R..

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

analysisanalysis

Travel-time difference (Δτ) in Travel-time difference (Δτ) in the meridional plane as a the meridional plane as a function of latitude, for function of latitude, for different depths using 10% of different depths using 10% of low m coefficients. The five low m coefficients. The five ranges of separation ranges of separation distances correspond to distances correspond to different lower turning points different lower turning points (see legend). Lower turning (see legend). Lower turning points for these five ranges points for these five ranges are 0.96, 0.90, 0.79, 0.71 and are 0.96, 0.90, 0.79, 0.71 and 0.64R respectively.0.64R respectively.

First Results of Asteroseismic Observations atFirst Results of Asteroseismic Observations atMaidanak Observatory In UzbekistanMaidanak Observatory In Uzbekistan

We performed several campaigns of CCD-photometry observations inWe performed several campaigns of CCD-photometry observations in 20072007--2009 to2009 to evaluate the possible duration to be achieved and quality ofevaluate the possible duration to be achieved and quality ofobservations inobservations in Maidanak observatory with existent facilities as well as toMaidanak observatory with existent facilities as well as tofigurefigure out what can beout what can be done in near future with respect to some feasibledone in near future with respect to some feasibleimprovements in hardware and software (if necessary) to get higher improvements in hardware and software (if necessary) to get higher quality photometric data. For thesequality photometric data. For these purpose we chose relatively bright purpose we chose relatively bright variablevariable stars (mainly of stars (mainly of δδSct type) with known periods and of pulsations.Sct type) with known periods and of pulsations.

2. Investigation and analysis of solar corona, its small 2. Investigation and analysis of solar corona, its small features such as Coronal Bright Points (CBP)features such as Coronal Bright Points (CBP) in in Ultraviolet and X-ray images of the SunUltraviolet and X-ray images of the Sun

An automatic An automatic procedure of procedure of

CBPs CBPs identification identification

was was developed on developed on the base of the base of IDL softwareIDL software

Complete cycle Complete cycle variationvariations of CBPs number s of CBPs number

(upper curve) vs. sunspot number (lower (upper curve) vs. sunspot number (lower

curve)curve)

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

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

Number ofNumber of CBPs reached its maximum level CBPs reached its maximum level ( the same as in 1996 - previous period of ( the same as in 1996 - previous period of minimum of solar activity).minimum of solar activity).

ResultsResults

3. The study of gravitational lenses and3. The study of gravitational lenses andthe forming non-stationary galaxiesthe forming non-stationary galaxies

The aims:The aims:

• Investigation of a number of unique and Investigation of a number of unique and priority of gravitationally lensed quasars (GLQ)priority of gravitationally lensed quasars (GLQ)

• Identifying the nature of the early stage of Identifying the nature of the early stage of formation of galaxies and some of their formation of galaxies and some of their substructures.substructures.

SBS1520SBS1520

Q2237 – Q2237 – Einstein Cross Einstein Cross UM673=Q0142UM673=Q0142

Q0957Q0957

HH14141313

SBS0909SBS0909

Light curves of GLQ with taking into account time delay and Light curves of GLQ with taking into account time delay and microlensing eventsmicrolensing events

Deconvolution of RXJ1131-123Deconvolution of RXJ1131-123

Deconvolution of Deconvolution of HS0435-1223 HS0435-1223

ResultsResults

• Performing of multi-colour photometric observations of Performing of multi-colour photometric observations of double and quadruple GLQ - Q2237+030, H1413+117, double and quadruple GLQ - Q2237+030, H1413+117, B1422+237, UM673, SBS1520+530, PG1115+080, etc.B1422+237, UM673, SBS1520+530, PG1115+080, etc.

• Analysis of the light curves - calculation of the time delay, Analysis of the light curves - calculation of the time delay, the identification of microlensing, the study of the nature the identification of microlensing, the study of the nature of the radiation source and the galaxy-lensof the radiation source and the galaxy-lens

• Construction of the anisotropic multiparametric models of Construction of the anisotropic multiparametric models of the forming non-stationary galaxies.the forming non-stationary galaxies.

• Research and analysis of gravitational instability of these Research and analysis of gravitational instability of these models, the definition of relations between physical models, the definition of relations between physical parameters that lead to the formation of various large-parameters that lead to the formation of various large-scale structures. scale structures.

4. Asteroids: MBA, NEA, young family4. Asteroids: MBA, NEA, young familyCurrently gathered observations on the families:Currently gathered observations on the families:((2005-2008, 2005-2008, more thenmore then 150 150 asteroidsasteroids, , NAO Japan)NAO Japan)

• Karin - 832, 1998sq81, 10783, 28271, 33143, 79213

• Lannini -1929cz, 2000oh45, 2000oz7, 2000ro76, 2001xg241, 2003af89, 2001pu35, 4652, 81550, etc.

• Veritas - 1902jp, 1964tn2, 1975sb1, 1976us, 1982an, 1997ro7, 1998rp80, 1998ry63, 1999xf8, 2000ck92, 2000dm102, 2000ef148, 2000fk2, 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 astrophysicsTheoretical astrophysics 1. Research of the group is mainly devoted to the general-1. Research of the group is mainly devoted to the general-relativistic electrodynamics of continuous media such as relativistic electrodynamics of continuous media such as superconductor, conductor, plasma etc and its application superconductor, conductor, plasma etc and its application for theoretical explanation and analysis of electromagnetic for theoretical explanation and analysis of electromagnetic and astrophysical processes in external gravitational fields.and astrophysical processes in external gravitational fields. 2. Experimental tests of general relativity, general relativistic 2. Experimental tests of general relativity, general relativistic electromagnetic effects and fields for pulsars and magnetized electromagnetic effects and fields for pulsars and magnetized rotating and oscillating neutron stars are also in our rotating and oscillating neutron stars are also in our scientific interests. scientific interests.

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

We also focus on space weather applications:We also focus on space weather applications:

1. R1. Radio transparency, its variation and correlation adio transparency, its variation and correlation with meteoparameters and active processes on the with meteoparameters and active processes on the

Sun and Sun and in in heliosphere heliosphere ((at the plateau Suffa) at the plateau Suffa)

2. Ionosphere investigation is carry out with the 2. Ionosphere investigation is carry out with the VLF-receiver supplied by the Stanford University VLF-receiver supplied by the Stanford University

under IHY-2007. This equipment provides under IHY-2007. This equipment provides monitoring of the ionosphere over the territory of monitoring of the ionosphere over the territory of

Tashkent on the permanent basis. Tashkent on the permanent basis.

Radio observatory at the plateau Suffa Radio observatory at the plateau Suffa 70 m radiotelescope in mm range70 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)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 Affiliations astronomy centers under leadership of the Astronomical Instituteunder leadership of the Astronomical Institute

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

the great astronomer Ulughbekthe great astronomer Ulughbek..

Parkent (1100m) Solar furnaceParkent (1100m) Solar furnace

In the frame of the IYA-2009 Program:In the frame of the IYA-2009 Program:

• The International Conference “Mirzo Ulughbek and his The International Conference “Mirzo Ulughbek and his contribution to the development of the contribution to the development of the World ScienceWorld Science" " was organized was organized   in in   Samarkand, Samarkand, 9-11 9-11 June, 2009.June, 2009.• The Museum of astronomic instruments of the 18-19th The Museum of astronomic instruments of the 18-19th century with unique instruments and appliances have been century with unique instruments and appliances have been created in the Astronomical Institute this year. created in the Astronomical Institute this year. • The training astronomical Seminar for university The training astronomical Seminar for university lecturers and students Uzbekistan was organized by UzAI lecturers and students Uzbekistan was organized by UzAI in April 2009.in April 2009.• Every week we organize open lectures and excursions Every week we organize open lectures and excursions for scholars, students and amateurs in the Astronomical for scholars, students and amateurs in the Astronomical Institute. Institute.

Ulughbek Observatory in SamarkandUlughbek Observatory in Samarkand

Museum of the Astronomical InstituteMuseum of the Astronomical Institute

Telescopes of the 18th CenturyTelescopes of the 18th Century

Our International LinksOur International Links• Astronomical Institute of Moscow University (Russia) Astronomical Institute of Moscow University (Russia) • Astrophysical Institute of Potsdam (Germany) Astrophysical Institute of Potsdam (Germany) • Van Vlec Observatory of Wesleyan University (USA) Van Vlec Observatory of Wesleyan University (USA) • Harvard-Smithsonian Center for Astrophysics (USA)Harvard-Smithsonian Center for Astrophysics (USA)• Stanford University (USA) Stanford University (USA) • Grenoble Observatory of J. Fourier University (France) Grenoble Observatory of J. Fourier University (France) • University de Nice (France)University de Nice (France)• National Astronomical Observatory (Japan)National Astronomical Observatory (Japan)• Astronomical Institute of Amsterdam University (Holland) Astronomical Institute of Amsterdam University (Holland) • Astrophysical Laboratory of National Tsing Hua University Astrophysical Laboratory of National Tsing Hua University

(Taiwan)(Taiwan)• Astronomical Consortium of Korean Universities (Korea)Astronomical Consortium of Korean Universities (Korea)

Coming together is the beginning. Keeping together is progress. Coming together is the beginning. Keeping together is progress. Working together is success. Henry FordWorking together is success. Henry Ford

We are open for new scientific cooperation We are open for new scientific cooperation and collaborations and collaborations

Thank you