Vega program explained

The Vega program (Russian: Вега) was a series of Venus missions that also took advantage of the appearance of comet 1P/Halley in 1986. Vega 1 and Vega 2 were uncrewed spacecraft launched in a cooperative effort among the Soviet Union (who also provided the spacecraft and launch vehicle) and Austria,[1] Bulgaria, France, Hungary, the German Democratic Republic, Poland, Czechoslovakia, and the Federal Republic of Germany in December 1984. They had a two-part mission to investigate Venus and also flyby Halley's Comet.

The flyby of Halley's Comet had been a late mission change in the Venera program, following on from the cancellation of the American Halley mission in 1981. A later Venera mission was canceled and the Venus part of the Vega 1 mission was reduced. Because of this, the craft was designated VeGa, a contraction of Venera and Gallei (Венера and Галлей respectively, the Russian words for "Venus" and "Halley"). The spacecraft design was based on the previous Venera 9 and Venera 10 missions.

The two spacecraft were launched on 15 and 21 December 1984, respectively. With their redesignated dual missions, the Vega probes became part of the Halley Armada, a group of space probes that studied Halley's Comet during its 1985/1986 perihelion.

The Vega spacecraft

Vega 1 and Vega 2 were identical sister ships developed from the earlier Venera craft. They were of the 5VK type, designed by Babakin Space Center and constructed by Lavochkin at Khimki. The craft were powered by twin large solar panels and instruments included an antenna dish, cameras, spectrometer, infrared sounder, magnetometers (MISCHA), and plasma probes. The craft were launched by a Proton 8K82K rocket from Baikonur Cosmodrome, Tyuratam, Kazakh SSR (current Kazakhstan). Both Vega 1 and Vega 2 were three-axis stabilized spacecraft. The spacecraft were equipped with a dual bumper shield for dust protection from Halley's comet.

Bus Instruments

The Venus mission

Vega 1 arrived at Venus on 11 June 1985 and Vega 2 on 15 June 1985, and each delivered a 1500kg (3,300lb), diameter spherical descent unit. The units were released some days before each arrived at Venus and entered the atmosphere without active inclination changes. Each contained a lander and a balloon explorer.

Descent craft

The landers were identical to that of the previous five Venera missions and were to study the atmosphere and surface. Each had instruments to study temperature and pressure, a UV spectrometer, a water concentration meter, a gas-phase chromatograph, an X-ray spectrometer, a mass spectrometer, and a surface sampling device.

The Vega 1 lander's surface experiments were inadvertently activated at from the surface by an especially hard wind jolt, and so failed to provide results. It landed at 7.5°N, 177.7°E.

The Vega 2 lander touched down at 03:00:50 UT on 15 June 1985 at 8.5° S, 164.5° E, in eastern Aphrodite Terra. The altitude of the touchdown site was above the planetary mean radius. The measured pressure at the landing site was 91 atm and the temperature was . The surface sample was found to be an anorthosite-troctolite. The lander transmitted data from the surface for 56 minutes.

Payload

Balloon

The two balloon aerobots were designed to float at from the surface, in the most active layer of the Venusian cloud system. The instrument pack had enough battery power for 60 hours of operation and measured temperature, pressure, wind speed, and aerosol density. The balloon envelopes were surfaced with polytetrafluoroethylene to resist attack by the corrosive atmosphere. Both Vega-1 and Vega-2 balloons operated for more than 46 hours from injection to the final transmission.[2]

The balloons were of spherical superpressure types of diameter, filled with helium. A gondola assembly weighing and long was connected to the balloon envelope by a tether long. Total mass of the entire assembly was .

The top section of the gondola assembly was capped by a conical antenna tall and wide at the base. Beneath the antenna was a module containing the radio transmitter and system control electronics. The lower section of the gondola assembly carried the instrument payload and batteries.

The instruments consisted of:

The small low-power (5 watt) transmitter only allowed a data transmission rate of 2,048 bit/s, though the system performed data compression to squeeze more information through the narrow bandwidth. Nonetheless, the sampling rate for most of the instruments was only once every 75 seconds. The balloons were tracked by two networks (20 radio telescopes total) back on Earth: the Soviet network, coordinated by the Soviet Academy of Sciences, and the international network, coordinated by French: Centre national d'études spatiales of France (CNES).

The balloons were pulled out of the lander at 180000feet above the planet's darkside surface, and fell to 164000feet ASL while they were being inflated. After that, they rose to 177000feet and stabilized.[3] At this altitude, pressure and temperature conditions of Venus are similar to those of Earth at 18,000 feet MSL (5,5 km),[3] though the planet's winds move at hurricane velocity, and the carbon dioxide atmosphere is laced with sulphuric acid, along with smaller concentrations of hydrochloric and hydrofluoric acid.

The balloons moved swiftly across the night side of the planet into the light side, where their batteries finally died, and contact was lost. Tracking indicated that the motion of the balloons included a surprising vertical component, revealing vertical motions of air masses that had not been detected by earlier probe missions.

The Halley mission

After their encounters, the Vega motherships were redirected to intercept Comet Halley, utilizing the gravity of Venus to alter their trajectory.

Vega 1 made its closest approach on 6 March, around from the nucleus, and Vega 2 made its closest approach on 9 March at . The data intensive examination of the comet covered only the three hours around closest approach. They were intended to measure the physical parameters of the nucleus, such as dimensions, shape, temperature, and surface properties, as well as to study the structure and dynamics of the coma, the gas composition close to the nucleus, the dust particles' composition and mass distribution as functions of distance to the nucleus, and the cometary-solar wind interaction.

In total Vega 1 and Vega 2 returned about 1,500 images of Comet Halley. Spacecraft operations were discontinued a few weeks after the Halley encounters.

The on-board TV system was created in international cooperation of the scientific and industrial facilities from the USSR, Hungary, France, and Czechoslovakia. The TV data was processed by an international team, including scientists from the Soviet Union, Hungary, France, East Germany, and the United States. The basic steps of data acquisition and preprocessing were performed in IKI using an image processing computer system based on a PDP-11/40 compatible host.

Vega 1 and Vega 2 are currently in heliocentric orbits.

See also

External links

Notes and References

  1. Book: Besser, Bruno Philipp . European Space Agency . Austria's history in space . ESA Publications Division . Noordwijk, the Netherlands . 2004 . 92-9092-545-0 . 56103655 .
  2. Preston. etal. 1986. Determination of Venus Winds by Ground-Based Radio Tracking of the VEGA Balloons. Science. 231. 4744. 1414–1416. 10.1126/science.231.4744.1414. 1986Sci...231.1414P. 17748082. 29444555.
  3. Web site: The First Flight on Another Planet (from Infinity Beckoned). Air & Space Smithsonian. Jay Gallentine. 2016. 20 April 2021.