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Huygens was an atmospheric entry
that landed successfully on 's moon
in 2005. Built and operated by the
(ESA), it was part of the
mission and became the first spacecraft ever to land on Titan and the furthest landing from Earth a spacecraft has ever made. The probe was named after the Dutch 17th-century astronomer , who discovered Titan in 1655.
The combined Cassini–Huygens spacecraft was launched from
on October 15, 1997. Huygens separated from the Cassini orbiter on December 25, 2004, and landed on Titan on January 14, 2005 near the
region. This was the first and, so far, only
ever accomplished in the . It touched down on land, although the possibility that it would touch down in an ocean was also taken into account in its design. The probe was designed to gather data for a few hours in the atmosphere, and possibly a short time at the surface. It continued to send data for about 90 minutes after touchdown. It remains the most distant landing of any human-made craft.
Huygens was designed to enter and brake in Titan's atmosphere and parachute a fully instrumented robotic laboratory to the surface. When the mission was planned, it was not yet certain whether the landing site would be a
range, a flat , an , or something else, and it was hoped that analysis of data from Cassini would help to answer these questions.
Based on pictures taken by Cassini at 1,200 km above Titan, the landing site appeared to be a shoreline. Assuming the landing site could be non-solid, Huygens was designed to survive the impact, splash down on a liquid surface on Titan, and send back data for several minutes on the conditions. If that occurred it was expected to be the first time a human-made probe would land in an extraterrestrial ocean. The spacecraft had no more than three hours of battery life, most of which was planned to be used during the descent. Engineers expected to get at most only 30 minutes of data from the surface.
Cutaway image of Huygens
The Huygens probe system consists of the 318 kg probe itself, which descended to Titan, and the probe support equipment (PSE), which remained attached to the orbiting spacecraft. Huygens' heat shield was 2.7 m in diameter. After ejecting the shield, the probe was 1.3 m in diameter. The PSE included the electronics necessary to track the probe, to recover the data gathered during its descent, and to process and deliver the data to the orbiter, from where it was transmitted or "downlinked" to the Earth.
The probe remained dormant throughout the 6.7-year interplanetary cruise, except for semiannual health checks. These checkouts followed preprogrammed descent scenario sequences as closely as possible, and the results were relayed to Earth for examination by system and payload experts.
Prior to the probe's separation from the orbiter on December 25, 2004, a final health check was performed. The "coast" timer was loaded with the precise time necessary to turn on the probe systems (15 minutes before its encounter with Titan's atmosphere), then the probe detached from the orbiter and coasted in free space to Titan in 22 days with no systems active except for its wake-up timer.
The main mission phase was a parachute descent through Titan's atmosphere. The batteries and all other resources were sized for a Huygens mission duration of 153 minutes, corresponding to a maximum descent time of 2.5 hours plus at least 3 additional minutes (and possibly a half-hour or more) on Titan's surface. The probe's radio link was activated early in the descent phase, and the orbiter "listened" to the probe for the next 3 hours, including the descent phase, and the first thirty minutes after touchdown. Not long after the end of this three-hour communication window, Cassini's high-gain antenna (HGA) was turned away from Titan and towards Earth.
Very large radio telescopes on Earth were also listening to Huygens' 10-watt transmission using the technique of
and aperture synthesis mode. At 11:25 CET on January 14, the
(GBT) in West Virginia detected the carrier signal from Huygens. The GBT continued to detect the carrier signal well after Cassini stopped listening to the incoming data stream. In addition to the GBT, eight of the ten telescopes of the continent-wide
in North America, ; ; ; ; ; and , also listened for the Huygens signal.
The signal strength received on Earth from Huygens was comparable to that from the
(the Jupiter atmospheric descent probe) as received by the , and was therefore too weak to detect in real time because of the signal modulation by the (then) unknown . Instead, wide-band recordings of the probe signal were made throughout the three-hour descent. After the probe telemetry was finished being relayed from Cassini to Earth, the now-known data modulation was stripped off the recorded signal, leaving a pure carrier that could be integrated over several seconds to determine the probe frequency. It was expected that through analysis of the Doppler shifting of Huygens' signal as it descended through the atmosphere of Titan, wind speed and direction could be determined with some degree of accuracy. A position of Huygens' landing site on Titan was found with precision (within one km – one km on Titan measures 1.3' latitude and longitude at the equator) using the Doppler data at a distance from Earth of about 1.2 billion kilometers. The probe landed on the surface of the moon at . A similar technique was used to determine the landing site of the Mars exploration rovers by listening to their telemetry alone.
Huygens landed at around 12:43 UTC on January 14, 2005 with an impact speed similar to dropping a ball on Earth from a height of about one meter (3 feet). It made a dent 12 cm (4.7 in) deep, before bouncing onto a flat surface, and sliding 30 to 40 cm (12 to 16 in) across the surface. It slowed due to friction with the surface and, upon coming to its final resting place, wobbled back and forth five times. Each wobble was about half as large as the previous one. Huygens' sensors continued to detect small vibrations for another two seconds, until motion subsided about ten seconds after touchdown. The probe kicked up a cloud of dust (most likely organic
that drizzle out of the atmosphere) which remained suspended in the atmosphere for about four seconds by the impact.
The first image released, taken from an altitude of 16 km, showing what are speculated to be drainage channels flowing to a possible shoreline. The darker areas are flat plains, while the lighter areas represent high ground.
At the landing site there were indications of pebbles of water ice scattered over an orange surface, the majority of which is covered by a thin haze of . Early aerial imaging of Titan from Huygens was consistent with the presence of large bodies of liquid on the surface. The initial photos of Titan before landing showed what appeared to be large drainage channels crossing the lighter colored mainland into a dark sea. Some of the photos suggested islands and mist shrouded coastline. Subsequent analysis of the probe's trajectory indicated that, in fact, Huygens had landed within the dark 'sea' region in the photos. The photos from the surface of a dry lakebed like landscape suggest that while there is evidence of liquid acting on the surface recently, hydrocarbon lakes and/or seas might not currently exist at the Huygens landing site. Further data from the Cassini Mission, however, definitely confirmed the existence of permanent liquid hydrocarbon lakes in the polar regions of Titan (see ). Long-standing tropical hydrocarbon lakes were also discovered in 2012 (including one not far from the Huygens landing site in the Shangri-La region which is about half the size of Utah's , with a depth of at least 1 meter). The likely supplier in dry desert areas is p in other words, the arid equatorial regions of Titan contain "".
In situ image of Titan's surface from Huygens—the first images from a non-Earth planetary surface beyond Mars and Venus (Left and right images have different image processing). Globules (probably made of water ice) 10–15 cm in size lie above darker, finer-grained substrate in a variable spatial distribution. Brightening of the upper left side of several rocks suggests solar illumination from that direction, implying a southerly view, which agrees with preliminary evidence from other data sets. A region with a relatively low number of rocks lies between clusters of rocks in the foreground and the background and matches the general orientation of channel-like features in the low-altitude images taken from under 7km altitude.
The surface was initially reported to be a -like "material which might have a thin crust followed by a region of relative uniform consistency." One ESA scientist compared the texture and colour of Titan's surface to a
(that is, a hard surface covering a sticky mud like subsurface). Subsequent analysis of the data suggests that surface consistency readings were likely caused by Huygens pushing a large pebble into the ground as it landed, and that the surface is better described as a "sand" made of ice grains or snow that has been frozen on top. The images taken after the probe's landing show a flat plain covered in pebbles. The pebbles, which may be made of hydrocarbon-coated water ice, are somewhat rounded, which may indicate the action of fluids on them. The rocks appear to be rounded, size-selected and size-layered as though located in the bed of a stream within a dark lakebed, which consists of finer-grained material. No pebbles larger than 15 centimeters across were spotted, while rocks smaller than 5 cm are rare on the Huygens landing site. This implies large pebbles cannot be transported to the lakebed, while small rocks are quickly removed from the surface.
The temperature at the landing site was 93.8  (-179.3 °C; -290.8 °F) and pressure of 1467.6
(1.448 atm), implying a methane abundance of 5 ± 1% and methane
of 50% near the surface. Therefore, ground fogs caused by methane in the neighborhood of the landing site are unlikely. Thermometers indicated that heat was wicked away from Huygens so quickly that the ground must have been damp, and one image shows light reflected by a dewdrop as it falls across the camera's field of view. On Titan, the feeble sunlight allows only about one centimeter of evaporation per year (versus one meter of water on Earth), but the atmosphere can hold the equivalent of about 10 meters of liquid before rain forms vs. only a few centimeters on Earth. So Titan's weather is expected to feature torrential downpours causing flash floods, interspersed by decades or centuries of drought.
Huygens found the brightness of the surface of Titan (at time of landing) to be about one thousand times dimmer than full solar illumination on Earth (or 500 times brighter than illumination by full moonlight). That is, the illumination level experienced about ten minutes after sunset on Earth, approximate late . The color of the sky and the scene on Titan is mainly orange due to the much greater attenuation of blue light by Titan's haze relative to red light. The Sun (which was comparatively high in the sky when Huygens landed) would be visible as a small, bright spot, one tenth the size of the solar disk seen from Earth, and comparable in size and brightness to a car headlight seen from about 150 meters. It casts sharp shadows, but of low contrast as 90% of the illumination comes from the sky.
Huygens separated from Cassini orbiter at 02:00
on December 25, 2004 in .
Huygens entered Titan's atmosphere at 10:13 UTC on January 14, 2005 in SCET, according to ESA.
The probe landed on the surface of the moon at about 10.2°S, 192.4°W around 12:43 UTC in SCET (2 hours 30 minutes after atmospheric entry).(1.)
There was a transit of the Earth and Moon across the Sun as seen from Saturn/Titan just hours before the landing. Huygens entered the upper layer of Titan's atmosphere 2.7 hours after the end of the transit of the Earth, or only one or two minutes after the end of the transit of the Moon. However, the transit did not interfere with the Cassini orbiter or Huygens probe, for two reasons. First, although they could not receive any signal from Earth because it was in front of the Sun, Earth could still listen to them. Second, Huygens did not send any readable data to the E it transmitted data to the Cassini orbiter, which relayed the data received to the Earth later.
Huygens had six complex instruments aboard that took in a wide range of scientific data after the probe descended into Titan's atmosphere. The six instruments are:
This instrument contains a suite of sensors that measured the physical and electrical properties of Titan's atmosphere.
measured forces in all three axes as the probe descended through the atmosphere. With the aerodynamic properties of the probe already known, it was possible to determine the density of Titan's atmosphere and to detect wind gusts. The probe was designed so that in the event of a landing on a liquid surface, its motion due to waves would also have been measurable. Temperature and pressure sensors measured the thermal properties of the atmosphere. The Permittivity and Electromagnetic Wave Analyzer component measured the
(i.e., positively charged particle) conductivities of the atmosphere and searched for electromagnetic wave activity. On the surface of Titan, the
(i.e., the ratio of
to its ) of the surface material was measured. The HASI subsystem also contains a microphone, which was used to record any acoustic events during probe's this was the first time in history that audible sounds from another planetary body had been recorded.
This experiment used an ultra-stable
to improve communication with the probe by giving it a very stable . This instrument was also used to measure the wind speed in Titan's atmosphere by measuring the
in the carrier signal. The swinging motion of the probe beneath its parachute due to atmospheric properties may also have been detected. Failure of ground controllers to turn on the receiver in the Cassini orbiter caused the loss of this data.[] Earth-based
were able to reconstruct some of it. Measurements started 150 kilometres above Titan's surface, where Huygens was blown eastwards at more than 400 kilometres per hour,[] agreeing with earlier measurements of the winds at 200 kilometres altitude, made over the past few years using . Between 60 and 80 kilometres, Huygens was buffeted by rapidly fluctuating winds, which are thought to be vertical wind shear. At ground level, the Earth-based doppler shift and
measurements show gentle winds of a few metres per second, roughly in line with expectations.
DISR data visualisation during Huygens' descent
As Huygens was primarily an atmospheric mission, the DISR instrument was optimized to study the radiation balance inside Titan's atmosphere. Its visible and infrared
and violet
measured the up- and downward radiant flux from an altitude of 145 kilometers down to the surface. Solar aureole cameras measured how scattering by
varies the intensity directly around the Sun. Three imagers, sharing the same , periodically imaged a swath of around 30 degrees wide, ranging from almost
to just above the horizon. Aided by the slowly spinning probe they would build up a full mosaic of the landing site, which, surprisingly, became clearly visible only below 25 kilometers altitude. All measurements were timed by aid of a shadow bar, which would tell DISR when the Sun had passed through the field of view. Unfortunately, this scheme was upset by the fact that Huygens rotated in a direction opposite to that expected. Just before landing a lamp was switched on to illuminate the surface, which enabled measurements of the surface reflectance at wavelengths which are completely blocked out by
absorption.
DISR was developed at the
under the direction of Martin Tomasko, with several European institutes contributing to the hardware. "The scientific objectives of the experiment fall into four areas including (1) measurement of the solar heating profile for studies of the thermal balance of T (2) imaging and spectral reflection measurements of the surface for studies of the composition, topography, and physical processes which form the surface as well as for direct measurements of the wind profil (3) measurements of the brightness and degree of linear polarization of scattered sunlight including the solar aureole together with measurements of the extinction optical depth of the aerosols as a function of wavelength and altitude to study the size, shape, vertical distribution, optical properties, sources and sinks of aerosols in Titan’ and (4) measurements of the spectrum of downward solar flux to study the composition of the atmosphere, especially the mixing ratio profile of methane throughout the descent."
A worker in the Payload Hazardous Servicing Facility (PHSF) stands behind the bottom side of the experiment platform for Huygens.
This instrument is a versatile gas chemical analyzer that was designed to identify and measure chemicals in Titan's atmosphere. It was equipped with samplers that were filled at high altitude for analysis. The , a high-voltage quadrupole, collected data to build a model of the molecular masses of each gas, and a more powerful separation of molecular and isotopic species was accomplished by the gas chromatograph. During descent, the
also analyzed pyrolysis products (i.e., samples altered by heating) passed to it from the Aerosol Collector Pyrolyser. Finally, the
measured the composition of Titan's surface. This investigation was made possible by heating the
instrument just prior to impact in order to vaporize the surface material upon contact. The GC/MS was developed by the
and 's Space Physics Research Lab.
The ACP experiment drew in
particles from the atmosphere through filters, then heated the trapped samples in ovens (using the process of ) to vaporize
and decompose the complex organic materials. The products were flushed along a pipe to the
instrument for analysis. Two filters were provided to collect samples at different altitudes. The ACP was developed by a (French)
team at the Laboratoire Inter-Universitaire des Systèmes Atmosphériques (LISA).
The SSP contained a number of sensors designed to determine the physical properties of Titan's surface at the point of impact, whether the surface was solid or liquid. An acoustic , activated during the last 100 meters of the descent, continuously determined the distance to the surface, measuring the rate of descent and the surface roughness (e.g., due to waves). The instrument was designed so that if the surface were liquid, the sounder would measure the speed of sound in the "ocean" and possibly also the subsurface structure (depth). During descent, measurements of the
gave information on atmospheric composition and temperature, and an accelerometer recorded the deceleration profile at impact, indicating the hardness and structure of the surface. A tilt sensor measured
motion during the descent and was also designed to indicate the probe's attitude after landing and show any motion due to waves. If the surface had been liquid, other sensors would also have measured its , temperature, , heat capacity, electrical properties ( and conductivity) and refractive index (using a critical angle refractometer). A
instrument, that protruded 55 mm past the bottom of the Huygens descent module, was used to create a penetrometer trace as Huygens landed on the surface by measuring the force exerted on the instrument by the surface as the instrument broke though the surface and was pushed down into the planet by the force of the probe landing itself. The trace shows this force as a function of time over a period of about 400 ms. The trace has an initial spike which suggests that the instrument hit one of the icy pebbles on the surface photographed by the DISR camera.
The Huygens SSP was developed by the Space Sciences Department of the
and the Rutherford Appleton Laboratory Space Science Department under the direction of Professor . The SSP research and responsibility transferred to the
when John Zarnecki transferred in 2000.
Application of
shimmers under bright lighting during final assembly. The gold colour of the MLI is due to light reflecting from the
coating on the back of sheets of amber coloured .
Huygens was built under the Prime Contractorship of
in its , France, now part of . The heat shield system was built under the responsibility of Aérospatiale near Bordeaux, now part of .
Space Systems was responsible for Huygens'
systems and the structural components, mechanisms and pyrotechnics that control the probe's descent onto Titan.
was responsible for the definition of the structure of each of Huygens' parachutes. Irvin worked on the probe's descent control sub-system under contract to .
Long after launch, a few persistent engineers discovered that the communication equipment on Cassini had a potentially fatal design flaw, which would have caused the loss of all data transmitted by Huygens.
Since Huygens was too small to transmit directly to Earth, it was designed to
data obtained while descending through Titan's atmosphere to Cassini by , which would in turn relay it to Earth using its large 4-meter diameter main antenna. Some engineers, most notably ESA
and , felt uneasy about the fact that, in their opinion, this feature had not been tested before launch under sufficiently realistic conditions. Smeds managed, with some difficulty, to persuade superiors to perform additional tests while Cassini was in flight. In early 2000, he sent simulated telemetry data at varying power and
levels from Earth to Cassini. It turned out that Cassini was unable to relay the data correctly.
The reason: under the original flight plan, when Huygens was to descend to Titan, it would have accelerated relative to Cassini, causing the
of its signal to vary. Consequently, the hardware of Cassini's receiver was designed to be able to receive over a range of shifted frequencies. However, the
failed to take into account that the Doppler shift would have changed not only the
frequency, but also the timing of the
, coded by
Reprogramming the firmware was impossible, and as a solution the trajectory had to be changed. Huygens detached a month later than originally planned (December 2004 instead of November) and approached Titan in such a way that its transmissions travelled perpendicular to its direction of motion relative to Cassini, greatly reducing the Doppler shift.
The trajectory change overcame the design flaw for the most part, and data transmission succeeded, although the information from one of the two radio channels was lost due to an unrelated error.
Huygens was programmed to transmit
and scientific data to the Cassini orbiter for relay to Earth using two redundant
radio systems, referred to as Channel A and B, or Chain A and B. Channel A was the sole path for an experiment to measure wind speeds by studying tiny frequency changes caused by Huygens's motion. In one other deliberate departure from full redundancy, pictures from the descent imager were split, with each channel carrying 350 pictures.
Cassini never listened to channel A because of a software design error. The receiver on the orbiter was never commanded to turn on, according to officials with the European Space Agency. ESA announced that the program error was a mistake on their part, the missing command was part of a software program developed by ESA for the Huygens mission, and that it was executed by Cassini as delivered.
Because Channel A was not used, only 350 pictures were received instead of the 700 planned. All
radio measurements between Cassini and Huygens were lost as well. Doppler radio measurements of Huygens from Earth were made, although they were not as accurate as the lost measurements that Cassini made. The use of accelerometer sensors on Huygens and
tracking of the position of the Huygens probe from Earth allowed reasonably accurate wind speed and direction calculations to be made.
The probe landed on the surface of Titan at .
Black ellipse shows approximate landing site on this image taken earlier by Cassini. The bright region to the right is .
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