Granat
Mission type | Gamma-ray astronomy | ||||||||||||||
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Operator | Soviet space program | ||||||||||||||
COSPAR ID | 1989-096A | ||||||||||||||
SATCAT no. | 20352 | ||||||||||||||
Website | hea.iki.rssi.ru/GRANAT/granat.html | ||||||||||||||
Mission duration | 9 years | ||||||||||||||
Spacecraft properties | |||||||||||||||
NPO Lavochkin[1] | |||||||||||||||
Launch mass | ~ 4,400 kg (9,700 lb) | ||||||||||||||
Payload mass | ~ 2,300 kg (5,100 lb) | ||||||||||||||
Dimensions | 4 m × 2.5 m (13.1 ft × 8.2 ft) | ||||||||||||||
Power | 400 W | ||||||||||||||
Start of mission | |||||||||||||||
Launch date | 20:20:00, December 1, 1989 (UTC) | ||||||||||||||
Launch site | Baikonur Cosmodrome 200/40 | ||||||||||||||
End of mission | |||||||||||||||
Disposal | deorbited | ||||||||||||||
Last contact | 27 November 1998 | ||||||||||||||
Decay date | May 25, 1999[2] | ||||||||||||||
Orbital parameters | |||||||||||||||
Reference system | Geocentric[1] | ||||||||||||||
Regime | Highly elliptical | ||||||||||||||
Eccentricity | 0.92193 | ||||||||||||||
Perigee altitude | 1,760 kilometres (1,090 mi)[4] | ||||||||||||||
Apogee altitude | 202,480 kilometres (125,820 mi) | ||||||||||||||
Inclination | 51.9 degrees | ||||||||||||||
Period | 5,880 minutes | ||||||||||||||
Epoch | 01 December 1989 | ||||||||||||||
Main telescope | |||||||||||||||
Name | SIGMA | ||||||||||||||
Type | MeV ) | ||||||||||||||
Instruments | |||||||||||||||
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The International Astrophysical Observatory "GRANAT" (usually known as Granat;
In September 1994, after nearly five years of directed observations, the gas supply for its
With seven different instruments on board, Granat was designed to observe the universe at energies ranging from
Spacecraft
Granat was a three-axis-stabilized spacecraft and the last of the
Launch and orbit
The spacecraft was launched on 1 December 1989 aboard a
Three days out of the four-day orbit were devoted to observations.
Date | Perigee (km) |
Apogee (km)
|
Arg.perigee (deg) |
Inc. (deg) |
Long.asc.node (deg) |
---|---|---|---|---|---|
December 1, 1989 | 1,760 | 202,480 | 285 | 51.9 | 20.0 |
December 1, 1991 | 23,893 | 179,376 | 311.9 | 82.6 | 320.3 |
December 1, 1994 | 58,959 | 144,214 | 343.0 | 86.5 | 306.9 |
December 1, 1996 | 42,088.8 | 160,888 | 9.6 | 93.4 | 302.2 |
Instrumentation
SIGMA
The hard X-ray and low-energy gamma-ray SIGMA
ART-P
The ART-P X-ray telescope was the responsibility of the
ART-S
The ART-S X-ray spectrometer, also built by the IKI, covered the energy range 3 to 100 keV. Its field of view was 2° by 2°. The instrument consisted of four detectors based on spectroscopic MWPCs, making an effective area of 2,400 cm2 at 10 keV and 800 cm2 at 100 keV. The time resolution was 200 microseconds.[3]
PHEBUS
The PHEBUS experiment was designed by
WATCH
Starting in January 1990, four WATCH instruments, designed by the Danish Space Research Institute, were in operation on the Granat observatory. The instruments could localize bright sources in the 6 to 180 keV range to within 0.5° using a Rotation Modulation Collimator. Taken together, the instruments' three fields of view covered approximately 75% of the sky. The energy resolution was 30% FWHM at 60 keV. During quiet periods, count rates in two energy bands (6 to 15 and 15 to 180 keV) were accumulated for 4, 8, or 16 seconds, depending on onboard computer memory availability. During a burst or transient event, count rates were accumulated with a time resolution of 1 second per 36 energy channels.[3]
KONUS-B
The KONUS-B instrument, designed by the
The KONUS-B instrument operated from 11 December 1989 until 20 February 1990. Over that period, the "on" time for the experiment was 27 days. Some 60 solar flares and 19 cosmic gamma-ray bursts were detected.[3]
TOURNESOL
The French TOURNESOL instrument consisted of four proportional counters and two optical detectors. The proportional counters detected photons between 2 keV and 20 MeV in a 6° by 6° field of view. The visible detectors had a field of view of 5° by 5°. The instrument was designed to look for optical counterparts of high-energy burst sources, as well as performing spectral analysis of the high-energy events.[3]
Science results
Over the initial four years of directed observations, Granat observed many galactic and extra-galactic X-ray sources with emphasis on the deep imaging and spectroscopy of the Galactic Center, broad-band observations of black hole candidates, and X-ray novae. After 1994, the observatory was switched to survey mode and carried out a sensitive all-sky survey in the 40 to 200 keV energy band.
Some of the highlights included:
- A very deep imaging (more than 5 million seconds duration) of the Galactic Center region.[10]
- Discovery of electron-positron annihilation lines from the galactic microquasar 1E1740-294 and the X-ray Nova Muscae.[7]
- Study of spectra and time variability of black hole candidates.[7]
- Across eight years of observations, Granat discovered some twenty new X-ray sources, i.e. candidate black holes and neutron stars. Consequently, their designations begin with "GRS" meaning "GRANAT source".[8] Examples are GRS 1915+105 (the first microquasar discovered in our galaxy) and GRS 1124-683.[8][9]
Impact of the dissolution of the Soviet Union
After the end of the
The main and most urgent problem, however, was in finding funds to support the continued operation of the spacecraft amid the spending crunch in post-Soviet Russia. The French space agency, having already contributed significantly to the project (both scientifically and financially), took upon itself to fund the continuing operations directly.[1]
See also
References
This article incorporates public domain material from websites or documents of the
- ^ a b c d e "Granat X-ray and Gamma-ray Observatory". The Federation of American Scientists. Archived from the original on 2007-02-06. Retrieved 2007-12-06.
- ^ a b c "1999 Reentries" (PDF). The Aerospace Corporation, Center for Orbital and Reentry Debris Studies. Archived from the original (PDF) on 2005-01-22. Retrieved 2007-12-06.
- ^ a b c d e f g h i "GRANAT". NASA HEASARC. Retrieved 2007-12-05.
- ^ NPO Lavochkin, Orbital Astrophysical Observatory "Granat": Problems of Control Archived 2007-10-31 at the Wayback Machine, Zemlya i Vselennaya, 1994, no. 2. Only four rows from a table of twenty used here.
- ^ A&A Supplement Series, 1993, no. 97.
- ^ a b Molkov, S.V., Grebenev, S.A., Pavlinsky, M.N., Sunyaev. "GRANAT/ART-P OBSERVATIONS OF GX3+1: TYPE I X-RAY BURST AND PERSISTENT EMISSION", Mar 1999. 4pp. arXiv e-Print (astro-ph/9903089v1).
- ^ a b c d e f "The Granat Satellite". NASA HEASARC Imagine the Universe!. Archived from the original on 2014-05-14. Retrieved 2007-12-05.
- ^ IKI RAN. Retrieved 2007-12-05.
- ^ a b M.G. Revnivtsev, R.A. Sunyaev, M.R. Gilfanov, E.M. Churazov, A. Goldwurm, J. Paul, P. Mandrou and J. P. Roques "A hard X-ray sky survey with the SIGMA telescope of the GRANAT observatory", (2004) Astronomy Letters, vol. 30, p.527-533
- IKI RAN. Retrieved 2008-05-25.
External links
- Media related to Granat (space observatory) at Wikimedia Commons
- Official GRANAT Observatory homepages: English Russian
- NASA's HEASARC – Observatories – Granat
- Encyclopedia Astronautica: On This Day
- Global Telescope Network: Granat
- Gunter's Space Page: Granat (Astron 2)