Institute of Solar-Terrestrial Physics SB RAS

P.O.Box 4026, Irkutsk, 664033, Russia
Phone: 7(395-2) 46-34-91, Fax: 7(395-2) 46-25-57
Internet: http://www.iszf.irk.ru

The Baikal astrophysical observatory
The Norilsk Comprehensive Magneto-Ionospheric Station of the ISTP SD RAS.
Incoherent scatter radar
The cosmic-ray spectrograph
The Sayan solar observatory (SSO)
Siberian Solar Radio Telescope
  The Baikal astrophysical observatory (BAO) The Baikal astrophysical observatory is located in the outskirts of the settlement of Listvyanka on the shore of Lake Baikal 7 km from Irkutsk. Interurban bus service between Irkutsk and Listvyanka is available, 2-3 trips per day, 1.5 hour under way.
The BAO includes four solar telescopes in operation:
  1. Large Solar Vacuum Telescope (LSVT). Tower 25 meters in height. Siderostat, mirror 1 meter in diameter, evacuated tube, main objective lens 760 mm in diameter. Equivalent focal length 40,000 mm. Field of view 32 arcmin. Solar image 380 mm in diameter. Spatial resolution 0.18 arcsec. Spectrograph. The telescope is equipped with a CCD-system produced by Princeton Instruments; camera with TEK CCD matrix 512x512 pixels in size. Spectro-polarimetric observations are being carried on both in the visible and in the infrared. The telescope features the world's best optical characteristics among solar vacuum telescopes.
  2. H-alpha telescope for the full solar disk. Main objective lens 180 mm in diameter. Equivalent focal length 5,432 mm. Field of view 34 arcmin. Solar image 50 mm in diameter. Spatial resolution 0.92 arcsec. Spectral wavelength 6,563 Anstrom. Photographic film 80 mm in width is used, frame size 70x70 mm. Flare observations (patrol) and investigations of chromospheric fine structure are being carried on. In its characteristics, is highly comparable with its Lockheed analogue (USA) and is superior to its Opton analogue (Germany).
  3. KCaII-telescope for the full solar disk. Main objective lens 180 mm in diameter. Equivalent focal length 5,154 mm. Field of view 34 arcmin. Solar image 48 mm in diameter. Spatial resolution 0.44 arcsec. Spectral wavelength 3,934 Angstrom. Photographic film 80 mm in width is used, frame size 70x70 mm. Observations of magnetic fields and filament appearance are being carried on.
  4. H-alpha telescope for large-scale images. Main objective lens 255 mm in diameter. Equivalent focal length 15,406 mm. Field of view 9 arcmin. Solar image 142 mm in diameter. Spatial resolution 0.65 arcsec. Spectral wavelength 6,563 Angstrom. Photographic film 35 mm in width is used, frame size 24x36 mm. High-resolution investigations of fine structure of individual active regions are being carried on.
      Astronomical institutions of the following countries: Germany, France, and Spain.

     The telescopes are already used in joint research work between the Institute and other observatories and can be employed in similar co-operative activities. Two little habitable houses are available plus bath-house (under construction); meals are provided in an on-site room. Telephone radio-relay communication and radio station are available. Accommodation and meals expenses are in the limits of Russian travel allowances.


 The Norilsk Comprehensive Magneto-Ionospheric Station of the ISTP SD RAS. Geographical co-ordinates of the station: latitude - 69.3 , longitude - 88.2 ;
respectively, geomagnetic: 64.2 and 160.4 .
The station incorporates equipment for monitoring the state of different ionospheric layers, the Earth's magnetic field in the frequency range from 0 Hz to 5 Hz, the natural emission of cosmic radio noise, and auroras borealis, as well as equipment for conducting narrow-directed experiments within special programs, including a complex of instruments for receiving information from satellites. Such a complex of instruments permits the station's staff to carry out:
- continuous observations of the ionospheric conditions
- continuous observations of variations of the Earth's magnetic field
- continuous recordings of geomagnetic pulsations
- observations of auroras with the all-sky camera (occasionally)
- photometric observations of auroras with scanning photometers at different wavelengths
     Data of continuous observations are stored in the Institute's archives or directly in the observatory's archives and are available to the interested user.

     Parameters of the station's main instruments

Automatic ionospheric station (AIS):
- range of working frequencies - 1-18 MHz
- pulse repetition frequency - 50 Hz
- pulse duration - 70 ms
- Pulse power of radio transmitter - 10 kW
- manner of recording - photo
- parameters recorded - ionogram
- data archiving - cine-film
Digital magnetic-variation station:
(after August 1998)
- number of measured components - 3 (H,D,Z)
of the Earth's magnetic field
- dynamic range - +/-2000 nT
- resolution - 0.1 nT
- interrogation frequency - 1 min
- manner of recording - PC
- data archiving - diskette
Before the indicated date, data are recorded on photo-tape.

Induction nanoteslameter (for recording geomagnetic pulsations in the range 5 - 0.005 Hz).
- number of components recorded - 3 (H,D,Z)
- number of filters for each component - 4
- parameters of filters - P4 10-5 Hz
- P3 5-0.25 Hz
- P2 0.25-0.01 Hz
- P1 0.01-0.005 Hz
- range of measured amplitudes - 0.001-100 nT
- manner of recording - - analogue at MF magnetograph and recorders
- data archiving - magnetic tape and paper medium

In 1999, it is planned to bring into use a digital recording of geomagnetic pulsations on PC.

The all-sky camera S-180 (for observation of auroras) is installed at the remote point Istok 70 km to the north of Norilsk:
- angle of view - 120 degrees
- method of recording - system of mirrors
- manner ofrecording - photo
- frequency of photography - 1 frame per min
- data archiving - cine-film
The camera is operated occasionally.

In Norilsk, there are hotels, restaurants, cafes, etc.
City buses run between Norilsk and the station. The Norilsk CMIS has its own motor transport.

 Incoherent scatter radar
Incoherent scatter radar, located 120 km north-eastward of Irkutsk (53 degr.N, 103 degr.E).

The Irkutsk IS radar is a monostatic pulsed radar with frequency-controlled scanning. Its main characteristics are:
Working frequencies....................154-162 MHz
Pulse power..................................2.5-3.2 MW
Pulse duration..............................140-820 ms
Repetition frequency....................24.4 Hz
Antenna array..............................sectoral horn
Antenna gain...............................38 dB
Angular dimensions.....................0.5 degr. (N-S) 10 degr. (E-W)
Scan sector...................................60 degr. (N-S)
Polarisation...................................linear
System's noise temperature...........400-500 K

     Siberian The Irkutsk radar forms part of the world-wide network of IS radars, consisting of nine facilities, each of which is a unique research instrument. In its main parameters it is similar to the facilities abroad. For example, the IS radar of the European EISCAT Association has the following parameters: frequency - 224 MHz, power - 1.5 MW, antenna gain - 43 dB, and system's noise temperature - 250-350 K.
     Siberian In addition to technical data, the uniqueness of IS radars is also determined by their geographical location because of particular importance are data of co-ordinated observations of a global distribution of ionospheric parameters. The Irkutsk IS radar closes a substantial gap in the longitudinal chain of US, European and Japanese radars. It is the only radar in Russia.

EISCAT Scientific Association, Norway
Since 1993, the IS radar has been carrying on regular observations within the international program of World Days (20-30) days in the height range 200-500 km. Power height profiles and power spectra are recorded in digital form. In the immediate future it is planned to introduce the operating mode of emitting coded signals and a correlation treatment. Observational data are used to investigate the characteristics of variations in electron and ion temperature, velocity and ionospheric plasma density under different heliogeophysical conditions.
The Institute is ready to receive, on an exchange basis, 1-2 researchers for a period from two weeks to one month. Accommodation and boarding are available, communication by telephone only. Expected expenses:
Electric power for 24 hours of operation - 1680 rubbles
Hotel accommodation for 24 hours - 160 rubbles
Meals - 60-80 rubbles.


 The cosmic-ray spectrograph The cosmic-ray spectrograph of the Institute of Solar-Terrestrial Physics SB RAS consists of three cosmic-ray stations. The statistical accuracy of observations for one-hour period of data accumulation is not worse than 0.1%.
The stations of the spectrographic complex are located:
- 435 m above sea level in Irkutsk (52.47 N, 104.03 E)
- 2000 m above sea level 300 km from Irkutsk (Mondy, Buryatia, 52.28 N, 104.022 E)
- 3000 m above sea level 300 km from Irkutsk (Mondy, Buryatia, 52.28 N, 104.022 E)

Research area - investigations of processes in interplanetary space, in the solar wind, and in the Earth's magnetosphere.
Diagnostics of the inhomogeneous large-scale structure of the solar wind and the interplanetary magnetic field.
The uniqueness and principal advantage of the spectrographic complex are that the three cosmic-ray stations are located at points with the same geomagnetic cut-off rigidity (4 GV) at different levels in the Earth's atmosphere, which permits primary cosmic rays to be methodologically separated in energy.

Irkutsk, hotel, restaurant, e-mail, telephone, living expenses ~$70.

 The Sayan solar observatory (SSO)      The Sayan solar observatory (SSO) is located in the mountains at about 2000 meters above sea level, in the territory of the Republic of Buryatia (on the Mongolian frontier) 320 km to the south-west of Irkutsk. The time taken to reach the SSO from Irkutsk by the Institute's motor transport is 6-7 hours.

The SSO includes three (3) operating solar instruments.
  1. Automated solar telescope (AST). A horizontal solar telescope with coelostat mirrors 80 cm in diameter. It is equipped with several measuring systems, including the vector-magnetograph. It is intended for the investigation of magnetic fields and line-of-sight velocities on the Sun with high spatial resolution.
  2. Solar telescope for operative predictions (STOP). A horizontal special-purpose solar telescope with the coelostat mirrors 30 cm in diameter; the objective lens is 18 cm in diameter, and its focal length is 5 meters. It is equipped with the magnetograph for observation of large-scale solar magnetic fields and with the CCD-photometer for recording the Stokes parameters in several spectral lines simultaneously. It is most analogous to the J.Wilcox solar observatory telescope at Stanford University (USA).
  3. Coronograph. The objective lens is 40 cm in diameter, and the focal length is 12 meters. It is equipped with photographic recording systems and with a state-of- the-art CCD system. It is designed for observations of the solar corona, dynamic processes in spicules, and of the chromosphere.
  • Astronomical institutions of the following countries:
    Germany, France, Italy, and Switzerland.
    • All instruments are operable and can be used in co-operative research. Habitable premises are available, which are cosy and reasonably comfortable for expedition conditions. High-caloric diet is provided just as at home. Telephone and teletype communication channels are available. Living expenses are to be agreed upon, but they would be quite moderate.

     Siberian Solar Radio Telescope      Siberian Solar Radio Telescope (SSRT) of the Radioastrophysical Observatory at the ISTP SB RAS, Badary 250 km from Irkutsk.
         The SSRT is a unique modern solar radio telescope providing an all-weather monitoring of the state and development of solar activity in the lower corona. Therefore, the SSRT can be used to record one- and two-dimensional distributions of the intensity and circular polarisation of microwave emission with angular resolution as high as 15 arcsec, respectively, at 5.2 cm wavelength. At this wavelength, all phases of active regions and flares manifest themselves most effectively. A time resolution of up to 14 ms make sit possible to record a fine temporal picture of development of active processes. The spectrum of spatial frequencies and the dynamic range permit low-contrast features to be recorded: filaments, and coronal holes. The SSRT is a 256-antenna radio interferometer, consisting of two equidistant antenna arrays oriented in the East-West and North-South directions. The instrument is automated, and data are recorded in digital form during the daytime. E-mail is available, and access to Internet is possible, but communication is limited by local telephone lines. It is intended to improve substantially the sensitivity and to convert the SSRT to multi-wavelength observations of the quasi-three-dimensional picture of manifestations of solar activity in the corona. A further development of existing co-operation is possible both in doing joint research and in the advancement and modernisation of the SSRT. The SSRT is incorporated in the program of ground-based support of the Solar and Heliospheric Observatory of EAS+NASA, it works closely with the Nobeyama observatory (Japan) which has a similar radio telescope, and the Beijing observatory (China).      The instrument is operable and can be used in co-operative research. The SSRT provides good (if the money is available) meals. Weekly trips of a minibus are used to carry out special operations on a watch basis. Living expenses at the SSRT are in the limits of travel allowance. Expenses incurred by using solar activity monitoring data available for the time interval 1985-1998 or by using the SSRT on a target-oriented basis - to be agreed upon with due regard for the contribution of the interested scientist or his/her observatory.