| Auto: | all |
| Helios A\Helios B | |
| Mission Type: | Solar observation |
| Cospar Id: | Helios-A: Helios-B: |
| Satcat: | Helios-A: 7567 Helios-B: 8582 |
| Website: | |
| Mission Duration: | Helios-A: Helios-B: |
| Manufacturer: | MBB |
| Launch Mass: | Helios-A: 371.2kg (818.4lb) Helios-B: 374kg (825lb) |
| Power: | 270 watts (solar array) |
| Launch Date: | Helios-A: UTC Helios-B: UTC[1] |
| Launch Rocket: | Titan IIIECentaur |
| Launch Site: | Cape Canaveral SLC-41 |
| Entered Service: | Helios-A: January 16, 1975 Helios-B: July 21, 1976 |
| Deactivated: | Helios-A: Helios-B: December 23, 1979 |
| Last Contact: | Helios-A: February 10, 1986 Helios-B: March 3, 1980 |
| Orbit Reference: | Heliocentric |
| Orbit Eccentricity: | Helios-A: 0.5218 Helios-B: 0.5456 |
| Orbit Periapsis: | Helios-A: 0.31 AU Helios-B: 0.29 AU |
| Orbit Apoapsis: | Helios-A: 0.99 AU Helios-B: 0.98 AU |
| Orbit Inclination: | Helios-A: 0.02° Helios-B: 0° |
| Orbit Period: | Helios-A: 190.15 days Helios-B: 185.6 days |
| Orbit Epoch: | Helios-A: January 15, 1975, 19:00 UTC Helios-B: July 20, 1976, 20:00 UTC |
| Apsis: | helion |
Helios-A and Helios-B (after launch renamed and ) are a pair of probes that were launched into heliocentric orbit to study solar processes. As a joint venture between German Aerospace Center (DLR) and NASA, the probes were launched from Cape Canaveral Air Force Station, Florida, on December10, 1974, and January15, 1976, respectively.
The Helios project set a maximum speed record for spacecraft of 252792km/h. Helios-B performed the closest flyby of the Sun of any spacecraft until that time. The probes are no longer functional, but as of 2024 remain in elliptical orbits around the Sun.
The Helios project was a joint venture of West Germany's space agency DLR (70 percent share) and NASA (30 percent share). As built by the main contractor, Messerschmitt-Bölkow-Blohm, they were the first space probes built outside the United States and the Soviet Union to leave Earth orbit.
The two Helios probes look similar. Helios-A has a mass of, and Helios-B has a mass of . Their scientific payloads have a mass of on Helios-A and on Helios-B. The central bodies are sixteen-sided prisms in diameter and high. Most of the equipment and instrumentation is mounted in this central body. The exceptions are the masts and antennae used during experiments and small telescopes that measure the zodiacal light and emerge from the central body. Two conical solar panels extend above and below the central body, giving the assembly the appearance of a diabolo or spool of thread.
At launch, each probe was tall with a maximum diameter of . Once in orbit, the telecommunications antennae unfolded on top of the probes and increased the heights to . Also deployed were two rigid booms carrying sensors and magnetometers, attached on both sides of the central bodies, and two flexible antennae used for the detection of radio waves, which extended perpendicular to the axes of the spacecraft for a design length of each.[2]
The spacecraft spin around their axes, which are perpendicular to the ecliptic, at 60rpm.
Electrical power is provided by solar cells attached to the two truncated cones. To keep the solar panels at a temperature below when in proximity to the Sun, the solar cells are interspersed with mirrors, covering 50% of the surface and reflecting part of the incident sunlight while dissipating the excess heat. The power supplied by the solar panels is a minimum of 240watts when the probe is at aphelion. Its voltage is regulated to 28volts DC. Silver-zinc batteries were used only during launch.
The biggest technical challenge was to avoid heating during orbit while close to the Sun. At from the Sun, approximate heat flow is 11 solar constants, (11 times the amount of solar irradiance received while in Earth orbit), or 22.4 kW per exposed square meter. At that distance, the probe could reach .
The solar cells, and the central compartment of instruments had to be maintained at much lower temperatures. The solar cells could not exceed, while the central compartment had to be maintained between -10and. These restrictions required the rejection of 96 percent of the energy received from the Sun. The conical shape of the solar panels was decided on to reduce heating. Tilting the solar panels with respect to sunlight arriving perpendicularly to the axis of the probe, reflects a greater proportion of the solar radiation. "Second surface mirrors" specially developed by NASA cover the entire central body and 50 percent of the solar generators. These are made of fused quartz, with a silver film on the inner face, which is itself covered with a dielectric material. For additional protection, multi-layer insulationconsisting of 18 layers of Mylar or Kapton (depending on location), held apart from each other by small plastic pins intended to prevent the formation of thermal bridgeswas used to partially cover the core compartment. In addition to these passive devices, the probes used an active system of movable louvers arranged in a shutter-like pattern along the bottom and top side of the compartment. The opening thereof is controlled separately by a bimetal spring whose length varies with temperature and causes the opening or closing of the shutter. Resistors were also used to help maintain a temperature sufficient for certain equipment.[3]
The telecommunication system uses a radio transceiver, whose power could be adjusted to between 0.5 and 20 watts. Three antennas are mounted on top of each probe. A high-gain antenna (23 dB) of 11° beam width, a medium-gain antenna (3 dB for transmission and 6.3 dB for reception) emits a signal in all directions of the ecliptic plane at the height of 15°, and a low-gain dipole antenna (0.3 dB transmission and 0.8 dB for reception). To be directed continuously toward Earth, the high-gain antenna is rotated by a motor at a speed that counterbalances the spin of the probe. Synchronizing the rotation speed is performed using data supplied by a Sun sensor. The maximum data rate obtained with the large antenna gain was 4096 bits per second upstream. The reception and transmission of signals were supported by the Deep Space Network antennas on Earth.
To maintain orientation during the mission, the spacecraft rotated continuously at 60 RPM around its main axis. The orientation control system manages the speed and orientation of the probe's shafts. To determine its orientation, Helios used a crude Sun sensor. Guidance corrections were performed using cold gas thrusters (7.7 kg nitrogen) with a boost of 1Newton. The axis of the probe was permanently maintained keeping it both perpendicular to the direction of the Sun and to the ecliptic plane.
The onboard controllers were capable of handling 256 commands. The mass memory could store 500 kb, (this was a very large memory for space probes of the time), and was mainly used when the probes were in superior conjunction relative to the Earth (i.e. the Sun comes between the Earth and the spacecraft). A conjunction could last up to 65 days.
Helios-A and Helios-B were launched on December 10, 1974, and January 15, 1976, respectively. Helios-B flew closer to the Sun than Helios-A, achieving perihelion on April17, 1976, at a record distance of 43.432e6km,[4] closer than the orbit of Mercury. Helios-B was sent into orbit 13 months after the launch of Helios-A. Helios-B performed the closest flyby of the Sun of any spacecraft until Parker Solar Probe in 2018, 43.432e6km from the Sun.[4]
The Helios space probes completed their primary missions by the early 1980s, but continued to send data until 1985.
Both Helios probes had ten scientific instruments[5] and two passive science investigations using the spacecraft telecommuniction system and the spacecraft orbit.
Measures the velocity and distribution of solar wind plasma. Developed by the Max Planck Institute for Aeronomy for the study of low-energy particles. Data collected included the density, speed, and temperature of the solar wind. Measurements were taken every minute, with the exception of flux density, which occurred every 0.1 seconds to highlight irregularities in plasma waves. Instruments used included:[6]
The flux-gate magnetometer measures the field strength and direction of low frequency magnetic fields in the Sun's environment. It was developed by the University of Braunschweig, Germany. It measures three-vector components of solar wind and its magnetic field with high precision. The intensity is measured with an accuracy to within 0.4nT when below 102.4nT, and within 1.2nT at intensities below 409.6nT. Two sample rates are available: search every two seconds or eight readings per second.[7]
Measures variations of the field strength and direction of low frequency magnetic fields in the Sol environment. Developed by the Goddard Space Flight Center of NASA; measures variations of the three-vector components of solar wind and its magnetic field with an accuracy to within 0.1nT at about 25nT, within 0.3nT at about 75nT, and within 0.9nT at an intensity of 225nT.[8]
The search coil magnetometer complements the flux-gate magnetometer by measuring the magnetic fields between 0 and 3 kHz. Also developed by the University of Braunschweig, it detects fluctuations in the magnetic field in the 5Hz to 3000Hz range. The spectral resolution is performed on the probe's rotation axis.[9]
The Plasma Wave Investigation developed by the University of Iowa uses two 15 m antennas forming an electric dipole for the study of electrostatic and electromagnetic waves in the solar wind plasma in frequencies between 10 Hz and 3 MHz.[10] [11] [12]
The Cosmic Radiation Investigation developed by the University of Kiel sought to determine the intensity, direction, and energy of the protons and heavy constituent particles in radiation to determine the distribution of cosmic rays. The three detectors (semiconductor detector, scintillation counter, and Cherenkov detector) were encapsulated in an anti-coincidence detector.[13]
The Cosmic Ray Instrument developed at the Goddard Space Flight Center measures the characteristics of protons with energies between 0.1 and 800MeV and electrons with energies between 0.05 and 5MeV. It uses three telescopes, which cover the ecliptic plane. A proportional counter studies the X-rays from the Sun.[14]
Developed by the Max Planck Institute for Aeronomy, the low energy electron and proton spectrometer uses spectrometers to measure particle characteristics (protons) with energies between 20 keV and 2 MeV and electrons and positrons with an energy between 80 keV and 1 MeV.[15]
The Zodiacal light instrument includes three photometers developed by the Max Planck Institute for Astronomy to measure the intensity and polarization of the zodiac light in white light and in the 550nm and 400 nm wavelength bands, using three telescopes whose optical axes form angles of 15, 30, and 90° to the ecliptic. From these observations, information is obtained about the spatial distribution of interplanetary dust and the size and nature of the dust particles.[16]
The Micrometeoroid analyzer developed by the Max Planck Institute for Nuclear Physics is capable of detecting cosmic dust particles if their mass is greater than 10−15g. It can determine the mass and energy of a micro-meteorite greater than 10−14g. These measurements are made by exploiting the fact that micrometeorites vaporize and ionize when they hit a target. The instrument separates the ions and electrons in the plasma generated by the impacts, and measures the mass and energy of the incident particle. A low-resolution mass spectrometer determines the composition of impacting cosmic dust particles with a mass greater than 10−13g.[17] [18]
The Celestial Mechanic Experiment developed by the University of Hamburg uses the Helios orbit specifics to clarify astronomical measurements: flattening of the Sun; verification of predicted general relativity effects; determining the mass of the planet Mercury; the Earth–Moon mass ratio; and the integrated electron density between the Helios spacecraft and the data receivig station on Earth.[19]
The Coronal Sounding Experiment developed by the University of Bonn measures the rotation (Faraday effect) of the linear polarized radio beam from the spacecraft when it passes during opposition through the corona of the Sun. This rotation is a measure of the density of electrons and the intensity of the magnetic field in the traversed region.[20]
Helios-A was launched on December 10, 1974, from Cape Canaveral Air Force Station Launch Complex 41 in Cape Canaveral, Florida.[21] This was the first operational flight of the Titan IIIE rocket. The rocket's test flight had failed when the engine on the upper Centaur stage did not light, but the launch of Helios-A was uneventful.
The probe was placed in a heliocentric orbit of 192 days with a perihelion of 46500000km (28,900,000miles) from the Sun. Several problems affected operations. One of the two antennas did not deploy correctly, reducing the sensitivity of the radio plasma apparatus to low-frequency waves. When the high-gain antenna was connected, the mission team realized that their emissions interfered with the analyzer particles and the radio receiver. To reduce the interference, communications were carried out using reduced power, but this required using the large diameter terrestrial receivers already in place thanks to other space missions in progress.[22]
During the first perihelion in late February 1975, the spacecraft came closer to the Sun than any previous spacecraft. The temperature of some components reached more than, while the solar panels reached, without affecting probe operations. During the second pass on September 21, however, temperatures reached, which affected the operation of certain instruments.
Before Helios-B was launched, some modifications were made to the spacecraft based on lessons learned from the operations of Helios-A. The small engines used for attitude control were improved. Changes were made to the implementation mechanism of the flexible antenna and high gain antenna emissions. The X-ray detectors were improved so that they could detect gamma ray bursts, allowing them to be used in conjunction with Earth-orbiting satellites to triangulate the location of the bursts. As temperatures on Helios-A were always greater than 20C-change below the design maximum at perihelion, it was decided that Helios-B would orbit even closer to the Sun, and the thermal insulation was enhanced to allow the satellite to resist 15 percent higher temperatures.
Tight schedule constraints pressed on the Helios-B launch in early 1976. Facilities damaged during the launch of the Viking 2 spacecraft in September 1975 had to be repaired, while the Viking landing on Mars in summer 1976 made the Deep Space Network antennas that Helios-B needed to conduct its science while at perihelion unavailable.
Helios-B was launched on January 10, 1976, using a Titan IIIE rocket. The probe was placed in an orbit with a 187-day period and a perihelion of 43500000km (27,000,000miles). The orientation of Helios-B with respect to the ecliptic was reversed 180 degrees compared to Helios-A so that the micrometeorite detectors could have 360 degree coverage. On April 17, 1976, Helios-B made its closest pass of the Sun at a record heliocentric speed of 70km/s. The maximum recorded temperature was 20C-change higher than measured by Helios-A.
The primary mission of each probe spanned 18 months, but they operated much longer. On March3, 1980, four years after its launch, the radio transceiver on Helios-B failed. On January7, 1981, a stop command was sent to prevent possible radio interference during future missions. Helios-A continued to function normally, but with the large-diameter DSN antennae not available, data was collected by small diameter antennae at a lower rate. By its 14th orbit, Helios-As degraded solar cells could no longer provide enough power for the simultaneous collection and transmission of data unless the probe was close to its perihelion. In 1984, the main and backup radio receivers failed, indicating that the high-gain antenna was no longer pointed towards Earth. The last telemetry data was received on February10, 1986.[23]
Both probes collected important data about solar wind processes and the particles that make up the interplanetary medium and cosmic rays. These observations were made over a period from solar minimum in 1976 to a solar maximum in the early 1980s.
The observation of the zodiacal light established some of the properties of interplanetary dust present between 0.1 and 1 AU from the Sun, such as their spatial distribution, color and polarization. The amount of dust was observed to be 10 times that around the Earth. Heterogeneous distribution was generally expected due to the passage of comets, but observations have not confirmed this.
Helios collected data about comets, observing the passage of C/1975 V1 (West) in 1976, C/1978 H1 (Meir) in November 1978 and C/1979 Y1 (Bradfield) in February 1980. During the last event, probe detected disturbances in solar wind later explained by a break in the comet's tail. The plasma analyzer showed that the acceleration phenomena of the high-speed solar wind were associated with the presence of coronal holes. This instrument also detected, for the first time, helium ions isolated in the solar wind. In 1981, during the peak of solar activity, the data collected by Helios-A at a short distance from the Sun helped to complete visual observations of coronal mass ejections performed from the Earth's orbit. Data collected by Helios magnetometers supplemented data collected by Pioneer and Voyager and were used to determine the direction of the magnetic field at staggered distances from the Sun.
The radio and plasma wave detectors were used to detect radio explosions and shock waves associated with solar flares, usually during solar maximum. The cosmic ray detectors studied how the Sun and interplanetary medium influenced the spread of the same rays, of solar or galactic origin. The cosmic ray gradient, as a function of distance from the Sun, was measured. These observations, combined with those made by Pioneer11 between 1977 and 1980 in a distance of 12–23AU from the Sun produced a good model of this gradient. Some features of the inner solar corona were measured during occultations. For this purpose, either a radio signal was sent from the spacecraft to Earth or the ground station sent a signal that was returned by the probe. Changes in signal propagation resulting from the solar corona crossing provided information on density fluctuations.
As of 2020, the probes are no longer functional, but remain in orbit around the Sun.[24] [25] [26] [27]