Seal of Venera 14
|Mission type||Venus flyby / lander|
|Operator||Soviet Academy of Sciences|
|Mission duration||Travel: 4 months and 1 day|
Lander: 57 minutes
|Spacecraft type||4V-1 No. 761|
|Launch mass||4,394.5 kg (9,688 lb)|
|Landing mass||760 kilograms (1,680 lb)|
|Dry mass||1,632.71 kilograms (3,599.5 lb)|
|Dimensions||2.7 m × 2.3 m × 5.7 m (8.9 ft × 7.5 ft × 18.7 ft)|
|Start of mission|
|Launch date||November 4, 1981, 05:31:00 UTC|
|Launch site||Baikonur 200/39|
|End of mission|
|Last contact||lander: 5 March 1982 / carrier: 9 April 1983|
|Perihelion altitude||0.71 Astronomical units|
|Aphelion altitude||0.99 Astronomical units|
|Flyby of Venus|
|Spacecraft component||Venera 14 flight platform|
|Closest approach||March 3, 1982|
|Distance||26,050 km (16,190 mi)|
|Spacecraft component||Venera 14 descent craft|
|Landing date||March 5, 1982, 07:00:10 UTC|
|Landing site||Phoebe Regio)(east of|
Venera 14 was identical to the Venera 13 spacecraft and built to take advantage of the 1981 Venus launch opportunity and launched five days apart. It was launched on 4 November 1981 at 05:31:00 UTC and Venera 13 on 30 October 1981 at 06:04:00 UTC, both with an on-orbit dry mass of 760 kg (1,680 lb).
Each mission consisted of a cruise stage and an attached descent craft.
As the cruise stage flew by Venus the bus acted as a data relay for the lander and then continued on into a heliocentric orbit. It was equipped with a gamma-ray spectrometer, UV grating monochromator, electron and proton spectrometers, gamma-ray burst detectors, solar wind plasma detectors, and two-frequency transmitters which made measurements before, during, and after the Venus flyby.
The descent lander was a hermetically sealed pressure vessel, which contained most of the instrumentation and electronics, mounted on a ring-shaped landing platform and topped by an antenna. The design was similar to the earlier Venera 9–12 landers. It carried instruments to take chemical and isotopic measurements, monitor the spectrum of scattered sunlight, and record electric discharges during its descent phase through the Venusian atmosphere. The spacecraft used a camera system, an X-ray fluorescence spectrometer, a screw drill and surface sampler, a dynamic penetrometer, and a seismometer to conduct investigations on the surface.
List of lander experiments and instruments:
After launch and a four-month cruise to Venus the descent vehicle separated from the bus and plunged into the Venusian atmosphere on March 5, 1982. After entering the atmosphere a parachute was deployed. At an altitude of about 50 kilometres (31 mi) the parachute was released and simple airbraking was used the rest of the way to the surface.
The lander had cameras to take pictures of the ground and spring-loaded arms to measure the compressibility of the soil. The quartz camera windows were covered by lens caps that popped off after descent. By mischance Venera 14 measured the compressibility of the lens caps instead, as these had landed in just the place where the probe craned down to measure the soil.
Like its predecessor, the lander was equipped with acoustic microphones designed to record atmospheric noise which was later used in calculations to determine the average wind speed on the Venusian surface. Later analysis of said data determined the average wind speed at the surface to be between 0.3 and 0.5 metres per second (0.98 and 1.64 ft/s).
The lander functioned for at least 57 minutes (the planned design life was 32 minutes) in an environment with a temperature of 465 °C (869 °F) and a pressure of 94 Earth atmospheres (9.5 MPa). Telemetry had been maintained by means of the bus that carried signals from the lander's uplink antenna.
The spacecraft bus ended up in a heliocentric orbit where it continued to make observations in the X-ray and gamma ray spectrum. To provide data for the later Vega mission the bus activated its engine on the 14th November 1982. The last data published for the probe is from 16 March 1983.
American researcher Don P. Mitchell has processed the color images from Venera 13 and 14 using the raw original data. The new images are based on a more accurate linearization of the original 9-bit logarithmic pixel encoding.
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