Institute of Cosmophysical Research and Aeronomy SB RAS

Lenin Ave. 31, Yakutsk, 677891, Russia
Phone: 7(411-2) 44-50-26, Fax: 7(411-2) 44-55-51
E-mail: ikfia@yacc.yakutia.su
E-mail: ikfia@sci.yakutia.ru
Internet: http://www.sci.yakutia.ru/YSC/IKFIA/ikfia.html

The Yakutsk Extensive Air Shower Array.
Optical station Maimaga.
The Yakutsk meridional chain of Riometers.
The Yakutsk ground and underground cosmic ray research complex.
The Tixie Bay neutron super-monitor.
190 and 210 MM Chain Stations.
 The Yakutsk Extensive Air Shower Array
The array is located in Lena river valley near village Oktyomtsy (50 km south-west of Yakutsk). Geographical co-ordinates of the array are: latitude 61.70 N, longitude 129.40 E. The observation level is 100 m above the sea level, i.e. 1020 g.cm2.

     The main purposes of the Yakutsk EAS array are related to astrophysics of ultra-high-energy cosmic rays studying extensive air showers (EAS) in the energy range 1017- 1020 eV. The nuclear - electromagnetic cascades in the atmosphere are investigated also measuring charged particles, neutrons generated in EAS, and the Cherenkov light produced in the atmosphere.
The array consists of 58 ground-based and 6 underground detectors of charged particles (electrons and muons), 50 detectors of the atmospheric Cherenkov light. The total area covered by detectors is 12 km2 so the showers of the primary energy above 1017 eV are detected. Acceptance area of the Yakutsk array is the greatest one in the Former Soviet Union, and the variety of components measured simultaneously in the shower is unique over the world. In contrast to arrays in the United States ("Fly's Eye") and in Japan (AGASA) atmospheric Cherenkov light is used to estimate the energy of primary particles.      Possibilities for the performance of joint research or training:
- joint experiments at the Yakutsk array using the facilities running here as far as the supplementary equipment;
- joint analysis of the data accumulated;
- numerical simulations of the showers and modelling of the experimental parameters of the array.

Conditions of life hostel with 3-/4- bedrooms; three meals a day; three conveyance a week to the town; telephone, local TV; it is planned the Internet connection in a near future.

 Optical station Maimaga
      Optical station Maimaga (geographical co-ordinates j=63N; l=129,5E; geomagnetic co-ordinates F=56; L=199,7).
Purposes:
  1. A study of the large scale dynamics and thermal regime of the upper atmosphere.
  2. Internal gravity waves, tide, planetary wave propagation at the mesopause (~87 km) by their influence on the nightglow emission parameters. Long-term temperature trend.
  3. A study of subauroral diffuse luminosity and stable red arcs (SAR-arcs);
Equipment:
  1. Two-channels scanning photometer for registration of 557.7 and 630.0 nm emissions;
  2. four-channels zenith photometer;
  3. multi-channels all-sky photometers,
  4. Fabry-Perot interferometer for the Doppler temperature measurement;
  5. infrared spectrograph;
  6. infrared all-sky imager for the registration of the irregular patterns of the airglow.
Uniqueness: The upper atmosphere is characterised by complex dynamics and photochemistry, which are essentially due to processes occurring both in the lower atmospheric layers and above the region. This region is very sensitive to long-term climatic changes in the terrestrial atmosphere, to short-time ones (e.g. due to upward propagating internal gravity waves from the troposphere) and geomagnetic activity. Studies of this region continue to prove difficult; rocket measurements and lidar techniques can give the altitude distributions of the characteristics, but these are few in number and are expensive. Satellites measurements provide global coverage, but they are not capable of providing simultaneous measurements at a particular time. From this point of view, ground-based optical remote sensing of the airglow emissions continues to be one of the most cost effective methods of study the upper atmosphere. A set of the observatories located at the same latitude and different longitudes can give the information of the zonal changes of the atmosphere characteristics. Such information is necessary to improve current models of the atmosphere. The station Maimaga is located in the most favourable region for the optic measurements - far from big cities, industrial centres. A climate of Central Yakutia is anticyclone therefore the most of nights are cloudiness. The registrations of the SAR-arcs with a very low intensities (~40R) are unique in the world and demonstrate the location advantages. Most of instruments are interfaced with the personal computers and the obtained data are suitable for the exchange and joint analyses.      All instruments are conducted regular observations. Joint researches and training are possible. The station Maimaga is included as a site to the project PSMOS (Planetary Scale Mesosphere Observing System).
The station is situated on the cost of the Lena river in 150 km to the northward of Yakutsk.

Conditions of life:
- hostel with bedrooms for 2 persons;
- three meals a day;
- telephone, TV.

 The Yakutsk meridional chain of Riometers
 The Yakutsk meridional chain of Riometers. Five stations operate from September 1986 on the Yakutsk meridional chain to Island Kotelny . Four of them are located within Zhigansk and the Tixie Bay. The chain covers the latitude range 56.4 (- 69.7 (in corrected geomagnetic co-ordinates (in L co-ordinates from 3.08 to 8.0 ).

 The cosmic radionoise absorption is registered on the frequency 32 MHz by an antenna of the "wave channel" -type directed towards the pole of the world. Registration is carried out by analogy, rate of strength is 60 mm/h.
Possibilities for the performance and training.
Conditions of life: hostel at Tixie and Yakutsk.

  The Yakutsk ground and underground cosmic ray research complex.
The Yakutsk ground and underground cosmic ray research complex.
The cosmic ray research complex is located in city Yakutsk:
Geographical latitude: 62°02' N, longitude: 129°72' E
Altitude: 105 m above sea level
Cut- off Rigidity: 1.70 GV

The cosmic ray research complex is used for the investigation of galactic and solar cosmic ray distribution in heliosphere and Earth's magnitosphere. The particles with energy 2 ¸ 300 GeV are registered. The complex consists of following equipment:

a) The muon telescopes complex is located on the surface of the ground and under ground on depths 7,20 and 60 i w.e. The cosmic ray intensity is registered simultaneously from a vertical direction and from south-north directions under corners 30° and 60° relate to zenith.
Observed counting rates.

Directional component

Ver. Depth from the ground

(m w.e.)

Direction of Viewing

zenith (° ) azimuth (° )

Counting Rates, % /hr

Barometric Coefficient,

% / mb

V

N

S

 

0

0

30

30

 

0

180

950.000

291.000

292.000

-0.13

-0.13

-0.13

V

N

S

 

7

0

30

30

 

0

180

490.000

140.000

140.000

-0.10

-0.10

-0.10

V

N

S

 

20

0

30

30

 

0

180

260.000

78.000

74.000

-0.08

-0.08

-0.08

V

N

S

 

60

0

30

30

 

0

180

59.000

17.000

17.000

-0.04

-0.04

-0.04

V – vertical; N – northern; S - southern

The muon telescopes complex is unique in Russia. It runs in continuous regime with 10-minute and 1-hour accumulation.

b) Ionisation chamber ASK-1 is unique in the World. It intends for the registration of cosmic ray muon components and runs in a continuous mode since 1953. c) The neutron super-monitor of Canadian type consists of 3 sections till 6 counters. Neutron component is registered with 5-minute and 1-hour accumulation. Potential partners from EU countries:
Terra University di Roma, Departmento di Fisica " E. Amaldi", Italy
University of Oulu, Oulu, Dept. of Physical Sciences, Finland
Institute of Mathematics and Physics of Siedlce University, Poland
Institute of Experimental Physics SAS, Slovakia

Opportunity to use joint research and training
- joint experiments at the Yakutsk complex, using the facilities running here as far as supplementary equipment;
- exchange and joint analysis of current and accumulated data.

 The Tixie Bay neutron super-monitor. The Tixie Bay neutron super-monitor:
Geographical latitude: 71°60' N, longitude: 128°40' E
Cut - off Rigidity: 1.70 GV

The cosmic ray research complex is intended for the investigation of galactic and solar cosmic ray distribution in heliosphere and Earth's magnitosphere. The neutron supermonitor of Canadian type consists of 3 sections till 6 counters. Neutron component is registered with 5-minute and 1-hour accumulation in a continuous mode. Potential partners from EU countries: Terra University di Roma, Departmento di Fisica " E. Amaldi", Italy
University of Oulu, Oulu, Dept. of Physical Sciences, Finland
Institute of Mathematics and Physics of Siedlce University, Poland
Institute of Experimental Physics SAS, Slovakia

Opportunity to use joint research and training
- joint experiments at the Tixie Bay Observatory, using the facilities running here as far as supplementary equipment;
- exchange and joint analysis of current and accumulated data.
- hostel with 1-2 bed rooms.

 190 and 210 MM Chain Stations. 190 and 210 MM Chain Stations consists of six stations - isl. Kotelny (76.0(N, 137.9(E), Tixie (71.6(N, 128.9(E), Chokurdakh (70.6(N, 147.9(E), Zyryanka (65.8(N, 150.8(E), Zhigansk (66.8(N, 123.4(E) and Yakutsk (62.0(N, 129.7(E).
Complex of geophysical observatories are located at Tixie, Zhigansk and Yakutsk. Within framework of the 210 (magnetic meridian network project (PI - Prof. K.Yumoto, Kyushu University, Japan) the digital magnetometer systems were installed at isl.Kotelny in October 1994, Tixie and Chokurdakh in August 1992, Zyryanka in April 1994 and all-sky TV cameras - at Tixie in late March 1994 and Zhigansk in November 1995.

Magnetic field and aurora observation data from co-ordinated ground stations make possible to study magnetospheric processes by separating temporal and spatial variations of the phenomena, to clarify global and latitudinal structures, and to understand the global generation mechanisms of the magnetospheric phenomena. Complex of geophysical observatories at Tixie, Zhigansk and Yakutsk are equipped by identical magnetic variations stations IZMIRAN-4, high-sensitive induction magnetometers to register the ULF waves and other instruments.
Magnetic variations data from digital magnetometer systems at isl. Kotelny, Tixie, Chokurdakh, Zyryanka are obtained with ring-core flux-gate magnetometers with identical logging systems (DSR-3, KOSMO Ltd.) and time signal generators. The six magnetic signals ((H, (D, (Z, dH/dt, dD/dt, dZ/dt) and time pulses (1 min, 1 hr, 24 hr) are registered on a digital cassette tape using the digital data logger with sampling rate of 1 sec and 16 bit resolution of 0.0369nT/LSB at Zyryanka and 0.738nT/LSB at isl.Kotelny, Tixie, Chokurdakh. Each cassette tape holds 21 days of data. The time signal generator is maintained accurate to within (25 ms by automatic comparisons with standard radio transmissions from WWV (Boulder, USA). The all-sky TV camera consists of a fish-eye lens (Nikon, 8 mm, f2.8), an image intensifier (Hamamatsu, Night Viewer), a relay lens (Hamamatsu, 1/3.8) and a Charge Coupled Device (CCD) camera (Hamamatsu, C3077). All-sky images from the TV camera are recorded by a time-lapse 8-mm video recorder with a sampling interval of 4 sec. From these sampling intervals a one video tape is capable of recording for 1 month. A personal computer (NEC PC9801) controls the all-sky TV camera. The clock of the computer is always corrected to standard time by receiving a Global Positioning Satellite (GPS) time signal. 190( and 210( MM Chain Stations are extended in auroral and sub-auroral zones (L~3-8).

Possibilities for the performance and training joint experiments at complex geophysical observatories using the facilities running here as far as supplementary equipment. joint analysis of accumulated 1-sec digital magnetic data from 1992 to present time and aurora observation materials from 1994 to present time.

Conditions of life: hostel at Tixie and Yakutsk.