ISSN 00380946, Solar System Research, 2015, Vol. 49, No. 7, pp. 509–517. © Pleiades Publishing, Inc., 2015. Original Russian Text © L.M. Zelenyi, O.I. Korablev, D.S. Rodionov, B.S. Novikov , K.I. Marchenkov, O.N. Andreev, E.V. Larionov, 2014, published in Vestnik “NPO imeni S.A. Lavoch kina”, 2014, No. 2, pp. 13–21.
Scientific Objectives of the Scientific Equipment of the Landing Platform of the ExoMars2018 Mission L. M. Zelenyia, O. I. Korableva, b, D. S. Rodionova, B. S. Novikova , K. I. Marchenkova, O. N. Andreeva, and E. V. Larionova a Space
Research Institute, Russian Academy of Sciences, Moscow, Russia Moscow Institute of Physics and Technology, Dolgoprudny, Russia email:
[email protected];
[email protected];
[email protected];
[email protected];
[email protected]; oleg
[email protected];
[email protected] b
Received May 29, 2014
Abstract—The paper lists the main objectives of the scientific complex of the landing platform of the ExoMars2018 mission. Scientific instruments of the complex are described including the meteorological complex, Fourier spectrometer, radiothermometer, Martian gas analytical complex, dust complex, seismom eter, etc. The main studies and results that will be obtained using this scientific equipment are presented. Keywords: landing platform, ExoMars2018, Mars, complex of scientific equipment, Fourier spectrometer, meteorological complex DOI: 10.1134/S0038094615070229
INTRODUCTION ExoMars is a joint project of the Russian Space Agency and the European Space Agency (ESA). It consists of two parts (Vago et al., 2014) launched by Proton launch vehicles. In 2016, the Trace Gas Orbiter (TGO) and the Entry, Descent, and Landing Demon strator Module (EDM) will be placed in a Martian orbit. As part of the ExoMars2018 mission, the ESA rover weighing about 300 kg will be delivered to the surface of Mars using the landing module developed in Russia. After the rover leaves the landing platform, the latter will start its own scientific mission as a longlived station with a complex of scientific instruments devel oped under the leadership of the Space Research Institute (SRI) of the Russian Academy of Sci ences (RAS). The scientific mission of the platform is primarily concerned with the monitoring of various processes on the surface of Mars on a scale of days, seasons, and possibly even several Martian years. The monitoring will be carried out in a natural way by the longlived stationary platform. The planned period of operation on the surface is one Martian year, but this time can be significantly increased in the case of the successful progress of the project. The scientific complex of the landing platform of the ExoMars mission makes it possible to solve a num ber of scientific problems typical of the socalled net work landing mission, whose main tasks are monitor ing of the climate of Mars through meteorological observations at the surface and the study of the internal
structure of the planet by means of seismic measure ments. The first longterm observations on the surface were carried out using the Viking Lander (VL) 1.2 in 1976–1982 (Anderson et al., 1976; Hess et al., 1980). Then, an attempt to create such a network was made in the project Mars96 that included the landing of two small stations (Linkin et al., 1998) and the introduc tion of two penetrators (Surkov and Kremnev, 1998). Later, several concepts of network missions were developed, such as the Net Lander (Dehant et al., 2004), Pascal (Haberle et al., 2000), and Met Net (Harri et al., 2006). The fact that there are several sta tions is an important factor: for a detailed study of cli matic processes a network of 18–20 weather stations is recommended (Haberle et al., 2000) and for seismic measurements, at least 3–4 stations (Lognonne, 2005). None of the listed projects was implemented, except for the American lander InSight, a station for seismic exploration of Mars, that should be launched in 2016 (Banerdt et al., 2013). In Russia, the concept of the MarsNET project was developed in 2009–2011 that involved the deploy ment of three or four small stations on the surface of Mars. During the development of the ExoMars project in previous cooperation (without Russia) the concept of a longlived station GEP was developed (Biele et al., 2007). However, because of the limitations on the total weight of the lander this module had to be aban doned, and in the ESA–NASA configuration of the ExoMars project the landing platform was used only to deliver the rover to the surface. The lander EDM of the
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project ExoMars2016 could be an excellent weather station (Vago et al., 2014), but limited lifetime nullifies all the advantages of instruments installed on the mod ule. Thus, despite the relevance the concept of the net work mission is being implemented very slowly. Until now, such a mission has not been mentioned in the plans of the space agencies. The scientific instruments on the landing platform ExoMars2018 can make a significant contribution to building of the future net work and testing of its elements. Within the national program, the landing platform will make it possible to reach a number of scientific objectives of the Mars NET project and use the acquired knowledge and experience in new missions (Efanov et al., 2012). It is also possible to solve additional problems. The main scientific objectives of the landing plat form are as follows (1) The longterm monitoring of climatic condi tions on the Martian surface at the landing site. (2) The study of the composition of the Martian atmosphere from the surface. (3) The study of the interaction of the atmosphere and surface. (4) The study of the surface composition. (5) The study of the internal structure of Mars. (6) The monitoring of the radiation situation and other factors. In order to address these challenges the scientific equipment complex (SECEM) is designed. Below, a preliminary list of devices is given formed after several stages of selection based on the conceptual design. In the future, this list is subject to change depending on the specification of the resources of the platform. The paper is devoted to the discussion of scientific problems and ways to solve them using the proposed SECEM. 1. THE SCIENTIFIC EQUIPMENT COMPLEX The scientific equipment complex designed for solving scientific problems of the landing platform of the longlived station will have a total weight of not more than 50 kg taking into account interconnecting cables. This figure, as well as other resources allocated for the SECEM, continues to be refined. The compo sition of devices and modules is in the process of rec onciliation and is also subject to further refinement including taking into account the international com petition to participate in the scientific equipment of the platform (scheduled for 2014). The estimated time of operation of the landing platform on the surface is at least one Martian year. It is planned to use the TGO (will be launched in 2016) as a relay satellite to transfer data to the Earth. Devices are placed on thermocell panels (TCP). In addition to scientific instruments, the complex includes a number
of support devices. The preliminary list of scientific instruments is given in Table 1. The experience of development and testing, as well as technological groundwork and calibration tech niques, of similar scientific instruments for space experiments such as PhobosGrunt, LunaGlob, LunaResurs, MSL, MetNet, BepiColombo, and ExoMars2016 were taken into account in SECEM devices. 2. SCIENTIFIC OBJECTIVES OF THE LANDING PLATFORM 2.1. Monitoring of Climatic Conditions on the Surface of Mars The study of the climate of Mars and other planets close to Earth in their properties is the fundamental objective relevant to both the development of Mars and a deeper understanding of the nature of climate processes on the Earth. A relatively simple climate sys tem of Mars is a good extreme case for the Earth’s atmosphere. A thorough understanding of current cli mate processes on Mars makes it easier to assess the features of the climate of past eras and the reasons that led to catastrophic climate changes and atmospheric dissipation processes. The climate is characterized by temporal and spa tial variations of the basic atmospheric parameters (such as temperature, pressure, wind speed, etc.) that are consequences of the global circulation, heat bal ance, and interaction of the atmosphere with the sur face of the planet and outer space. Many of these parameters have been successfully measured as global characteristics for a long time from orbiting space craft. From infrared spectrometers and radiometers that operated and that are operating on spacecraft Mars Global Surveyor (MGS), Mars Odyssey (ODY), Mars Express (MEX), and Mars Reconnaissance Orbiter (MRO), multiyear series of parameters are available such as surface temperature, atmosphere temperature (at the level from 2–5 to 30–40 km), the total amount of dust and condensation clouds in the atmosphere, and the total amount of water vapor (Korablev, 2013). Such measurements are also planned within ExoMars2016 on the TGO (Korablev et al., 2014). However, such characteristics as pressure and wind speed cannot be accurately measured remotely. The atmospheric pressure cycle on Mars is especially important, since a substantial part of the carbon diox ide atmosphere condenses in winter in polar regions. The adjustment of general circulation models without lengthy series of pressure measurements is impossible. Unfortunately, until recently measurements from VL 1, 2 were the only source of such data (Hess et al., 1980). The meteorological complex was also installed on the rover Curiosity (GomezElvira et al., 2012), but the platform mobility is a complicating factor for such SOLAR SYSTEM RESEARCH
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The list of scientific instruments and support devices of the SECEM Instrument
Function
Key parameters
TVSLP
A TV system for the video recording of panoramas of the landing site, dynamics of atmospheric processes, stereo recording of the Martian landscape, and monitoring of the manipulator operation
Four PTZ cameras, field of view of 100°, stereocamera, field of view of 50°, the module for the collection and processing of data (2–20 com pression, storage capacity of 64 GB). All cameras have the resolution of 2048 × 2048 pixels, 3 colors
MM
Module of interfaces and 18 interfaces, the buffer memory memory, a common interface of 128 Gbps of commands and SECEM data
MMC
Sampling of soil from the sur face and placing it in soil receivers of scientific instru ments. The placement of sen sors and instruments on the surface
MC
Weight (taking into account the Head, cooperation system reserve) 3.9 kg
R.V. Bessonov, ISR RAS
2.5 kg
K.V. Anufreichik, ISR RAS
5.6 kg
O.E. Kozlov, ISR RAS, Poland
The meteorological complex. Eight temperature sensors, two pressure sensors, two humidity Measurements during the sensors, twocomponent ane descent mometer, aerosol sensors (nephelometer lidar and solar radi ation sensors), threeway acceler ometer, threecomponent angular velocity sensor, magnetometer, and microphone
3.5 kg rod
A.V. Lipatov, ISR RAS, TsNII MASH, Finland, Spain
STEM
Measurements of heat capac Four probe sensors, the penetratin ity , thermal diffusivity, ther to a depth of ~200 mm is required mal conductivity, and electri cal conductivity
1.4 kg
R.O. Kuzmin, Institute of Geochemistry and Analytical Chemis try
RATM
Microwave radiometer at 3 fre Radiothermometrical con tactless microwave measure quencies (6–20 GHz) ments. The estimation of the surface temperature on 3 lev els of depth, the optical thick ness of the atmosphere during the dust storm
0.6 kg
D.P. Skulachev, ISR RAS
FACT
Fourier spectrometer for the study of the atmosphere and monitoring of the climate of Mars
3.5 kg
O.I. Korablev, ISR RAS, Germany, Italy
DC
The dust complex for the con Shock sensor, laser turbidimeter, tact study of the properties of and electric field sensor dust particles carried by the wind near the surface of Mars
1.6 kg
A.V. Zakharov, ISR RAS, Italy
SEM
Seismometer for the study of microvibrations near the surface of Mars
Two axis horizontal seismometer
1.5 kg
A.B. Manukin, Institute of Physics of the Earth RAS
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Robotic arm, the range of 1.2 m. It includes the bucket, penetration device (up to 100 mm), and con textual camera
Observations of the Sun and atmo spheric radiation. The spectral range of 2–17 mm, the spectral resolution of 0.05 cm–1
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Table (Contd.) Instrument
Weight (taking into account the Head, cooperation system reserve)
Function
Key parameters
MGAC
The Martian gas analytical system for studying the dynamics of the microcom ponents of the atmosphere near the surface
The analysis of gases produced by heating of soil samples. The thermal analyzer (up to 1000°C, reusable pyrolytic cell), gas chromatograph, and mass spectrometer (mass reso lution of 1000, 2–1000 amu)
10 kg*
M.V. Gerasimov, ISR RAS, Switzer land, France, Ger many
MDLS
The laser spectrometer for the study of the chemical and isotopic composition of the atmosphere near the surface of Mars and volatiles of the Martian soil
Five lasers in the range of 1.4–1.6 µm and 2.5–2.7 µm, three atmo spheric cuvettes, and heterodyne atmospheric channel. The cuvette for the analysis of soil volatiles (in the MGAC)
2.6 kg rod
I.I. Vinogradov, ISR RAS, A.V. Ro din, Moscow Insti tute of Physics and Technology, France
ADRONEM Detectors of neutrons and gammarays with the possi bility of active sensing in order to determine the water content and the elemental composition of near surface soil, monitoring of the radia tion situation
The neutron generator, neutron detectors (0.001 eV–1 keV), gamma spectrometer (100 keV–8 MeV, resolution of 3%), dosimeter
5.6 kg
ABIMAS
The mass spectrometer with The mass range of 1–1000 amu, laser ablation for the analysis the resolution is 600 of the elemental composition of the soil
MEGRE
Monitoring of electromag The magnetic field in the range up netic emissions on the surface to 30 kHz. The electric field at fre quencies up to 3 MHz
I.G. Mitrofanov, ISR RAS
5 kg
G.G. Managadze, ISR RAS
1.5 kg * rod
* The refined weight of instruments is given after EP.
measurements. For example, it is very difficult to take into account distortions of the measurement series because of changes in the local topography. In this regard, the interest to meteorological stations on Mars is understandable (see INTRODUCTION). The main studied processes include the general cir culation, major climatic cycles, hydrological cycle and dust, mesoscale phenomena, processes in the bound ary layer, and the heat balance of the atmosphere. These processes will be studied by continuous monitoring and analysis of cycles of different time scales of parameters such as the atmospheric pressure, temperature, surface temperature, state (thermal structure) of the boundary layer, the content of water vapor in the atmosphere, the dust content and con densation of the aerosol in the atmosphere, and the state of cloudiness. Furthermore, the profile of the atmosphere will be obtained during the descent of the lander. The number of such profiles is very limited (Avduevskii et al., 1975; Magalhaes et al., 1999; Seiff and Kirk, 1976). The main instrument for carrying out such mea surements on the surface of Mars and during the
descent in the atmosphere is the meteorological com plex (MC). It consists of eight temperature sensors developed in Russia, two barosensors with the com pensation for the absolute pressure developed jointly by Russia and Finland, two humidity sensors devel oped in Finland, a twocomponent anemometer developed in Russia, and a number of optical sensors for aerosols. Pressure and infrasound sensors make it possible to investigate such mesoscale processes as infrasound, sound, and gravity waves. Using the MC the atmosphere profile will be mea sured on the descent: a threecomponent acceleration sensor with the capacitive resilient element and a threecomponent angular velocity sensor will operate at the braking phase via the aerodynamic screen, and during the descent on parachute, pressure and tem perature sensors will collect data. The prototype of the MC is a set of instruments designed for small stations MetNet (Harri et al., 2013). Another important tool for the study of the bound ary layer is a Fourier spectrometer for atmospheric constituents and temperature (FACT). The Fourier spectrometer measures the intrinsic radiation of the atmosphere in the thermal infrared range (up to SOLAR SYSTEM RESEARCH
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20 µm, the spectral resolution of 2 cm–1). It makes it possible to measure the temperature profile of the atmosphere at altitudes ranging from 0 to 50 km. The characteristics of the boundary layer can be deter mined in particular detail (Smith et al., 2006). Exper iment results will also make it possible to determine the characteristics of the aerosol and measure the total amount of water vapor in the atmospheric column. FACT is a new version of the Fourier spectrometer, the development of which is based on the experience of the development of similar instruments for Phobos Grunt (Korablev et al., 2012) and ExoMars2016 (Korablev et al., 2014) projects. Important information about the dynamics of the atmosphere can be obtained using the Martian diode laser spectrometer (MDLS). In the case of solar observations using the optical heterodyne spectros copy, the contour of the absorption line of a gas is determined, such as CO2, which makes it possible to accurately measure the Doppler shift of the line and directly estimate the wind speed at altitudes of the effi cient absorption in the line (from the surface to ~10 km). Such measurements are demonstrated on a prototype (Rodin et al., 2014). The following devices will provide more informa tion about the aerosol component: dust complex (DC), soil radiometer (RATM), and the TV system of the landing platform (TVSLP). The DC includes several types of sensors designed to study the dust component on Mars, as well as pro cesses in the atmosphere and near the surface of Mars associated with the dynamics of dust. Shock DC sen sors are designed for the direct measurement of flows of dust particles in the near surface layer and research of processes of saltation and dust devils. The turbi dimeter will make it possible to accurately describe the optical properties of the dust particles. The electric field sensor will detect electric fields and electromag netic noise generated by moving dust particles in the atmosphere and on the surface of Mars. The experi ence in the development of similar devices for projects PhobosGrunt (Esposito et al., 2011) and Luna Resurs was taken into account in the DC design. The RATM device has an additional scientific objective of the measurement of brightness tempera ture of the Martian atmosphere in the direction of the zenith. During a dust storm at high optical densities the brightness temperature will make it possible to draw conclusions about the density and physical com position of the dust. The TVSLP is a set of six cameras designed to mon itor the environment within the range of 360° horizon tally and 60° vertically and to obtain color images of atmospheric processes in the visible range (0.45, 0.55, and 0.65 µm). Under conditions of the limited amount of data transmitted to Earth it will periodically moni tor the cloud cover, fog, and smoke, as well as carry out remote detection of dust devils. Developments of the SOLAR SYSTEM RESEARCH
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Department of Optical and Physical Research of the ISR RAS characterized by a high degree of technolog ical readiness will be used in the development of the TVSLP. The surface temperature will be measured by a spe cial sensor of the meteorological complex and the fol lowing devices: a system of the thermoelectric moni toring of Martian soil (STEM) and RATM. 2.2. Studies of the Composition of the Martian Atmosphere Measurements of the atmospheric composition on the surface of Mars have undoubted advantages over the orbital and groundbased observations. The search and refinement of the upper limits of trace gases that can be localized in the lower atmosphere due to degas sing from the surface is more reliable to carry out in situ and with sufficient signal accumulation. The same applies to measurements of isotope ratios. Inert gases and their isotopes are not measured remotely. The SECEM has a number of instruments for the study of the atmospheric composition: FACT MDLS, and Martian gas analytical complex (MGAC) (Gerasimov et al., 2014). Studies of the atmospheric composition are the main scientific objective of the FACT. The main observation mode for the detection of absorption lines of trace gases in the atmospheric column is observation of the solar disk. By measuring the absorption of gas lines and isotopes with high spec tral resolution of 0.05 cm–1 in the range of 2–10 µm, the device makes it possible to measure methane, monitor the content of H2O and HDO and the rela tionship D/H, CO, H2O2, and O3. The FACT will help to refine upper limits or to discover new compounds: organic (C2H2, C2H4, C2H6, and CH2O), nitrogen containing (NH3 and NO2), chlorine (HCI, CH3CI), sulfur (OCS and SO2), etc. The water vapor and CO are also measured in the mode of the observation of the atmospheric selfradiation that in combination with observations on inclined paths can make it possi ble to obtain limits on the vertical distribution of these gases. The MDLS is designed for the study of the chem ical and isotopic composition of the atmosphere near the surface of Mars, its daily and seasonal variations by means spectral analysis of atmospheric samples (in the case of measurements using laser absorption spectros copy in cuvettes) and the integral content of atmo spheric components in the lower scales of altitudes (in the case of solar observations by the optical hetero dyne spectroscopy). The main scientific objective of the device is to study variations in the isotopic compo sition of water vapor associated with the fractionation in the processes of condensation and sublimation of ice particles in clouds. The isotopic fractionation is a sensitive marker of this key process of the atmospheric hydrological cycle of water on Mars, but until now it
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has not been studied. The MDLS is a new develop ment. Many of its concepts were shown in the devel opment of the gas chromatographic complex for the PhobosGrunt project (Durry et al., 2010; Gerasimov et al., 2011) and in the development of a similar instru ment for the LunaResurs project. Atmospheric problems can be solved by the chro matographymass spectrometer MGAC. In addition to its main scientific objective of studying the atmo sphere–surface interaction, it will measure the isoto pic ratio of volatile basic elements (D/H, 17O/16O, 18 O/16O, 13C/12C, 34S/32S, 37Cl/35Cl), as well as the content and isotopic composition of noble gases that are not measured by other methods. 2.3. Investigation of the Atmosphere and Surface Interaction The problem of studying the interaction of the atmosphere and the surface is solved in complex using special means of physical and chemical surface diag nostics and analysis of atmospheric processes. Many instruments contribute to the solution of this problem, but the study of volatiles in the soil and their distribu tion in the nearsurface atmosphere of Mars has a spe cial place. Volatile components can interact with sur face regolith at both physical level (freezing and adsorption to the cooled regolith in the night and the emission from the regolith with heating during the day) and through a variety of chemical reactions. Devices RATM, STEM, and the active neutron and gamma ray detector (ADRON EM) are designed to analyze and estimate the conditions on and below the surface. A laser mass spectrometer ABIMAS can contribute to the analysis of the content of volatiles in the soil. Atmospheric processes will be analyzed by the MDLS, MC, and FACT. The interaction of the atmosphere and the surface is the main task of the MGAC, which is designed for the study of volatiles in the ground and in the atmosphere. The main scientific objective of RATM is the non contact measurement of brightness temperature of the Martian soil (regolith) at depths of up to half a meter. The physical temperature of the Martian regolith at these depths will vary and depend on the local time of day and season. Information about the brightness tem perature of the regolith at different depths makes it possible to consider the parameters of regolith, such as thermal conductivity, heat capacity, and dielectric properties. The analysis of the dependence of the regolith temperature on the depth can also help to detect certain inclusions, such as ice. A similar proto type of the RAT device is developed for lunar landers. One of the main scientific objectives of the ADRONEM experiment is to determine the content of bound water in the composition of the Martian soil to a depth of 0.5–1.0 m and its continuous monitor ing. The device also makes it possible to study the
physical properties of the surface soil (layered struc ture, density, and temperature effects). Joint measure ments of the ADRONEM and ADRONPM (Niki forov et al., 2013) mounted on a mobile platform (of the ESA rover) will make it possible to study the profile in terms of the depth more detailed and measure the decay of the neutron signal from the pulsed neutron generator as the rover moves away from the landing platform. ADRONEM is based on developments for projects MSL (Mitrofanov et al., 2012), BepiColombo (Mitrofanov et al., 2010), etc., and has a high degree of technological readiness. The STEM instrument is designed for the long term monitoring of the physical properties of the sur face layer of the Martian soil. Studies suggest measure ments of thermal and electrical characteristics. The exchange of water between the surface soil and the atmosphere of the planet has a pronounced seasonal variation and depends on the latitude. The seasonal occurrence of water ice and bound water in the surface layer can cause a change in its thermophysical charac teristics. The simultaneous presence of salts and ice in the Martian soil can result in the temporary occur rence of the liquid phase in it in the form of films of saline solutions that will increase the electrical con ductivity and dielectric permeability of the soil. STEM is a new development, in which the experience of cre ating TERMOFOB for the PhobosGrunt project was used (Marov et al., 2011). The MDLS together with the FACT will make it possible to study the chemical and isotopic composi tion of the atmosphere near the surface of Mars, its daily and seasonal variations, and together with the MGAC the chemical and isotopic composition of the volatiles in the soil. The MGAC will make it possible to examine the contents of water and other volatile compounds in the rocks on the surface by the occurrence depth (within the possible depth of the dredge sampling device), to determine the forms of connections of volatiles with particles of regolith, to measure daily and seasonal variations of the content of water and other volatile compounds in the rocks of the upper surface layer (within the possible number of samples), and to mea sure daily and seasonal variations of the water content and other microcomponents of the atmosphere in the surface layer. 2.4. Investigations of the Surface Composition Investigations of the surface composition on the stationary platform are an additional scientific task. However, its solution using Russian instruments will significantly complement the rover measurements, especially considering possible restrictions on the number of cores analyzed by it. The sampling will be carried out using the Martian manipulator complex (MMC). It will make it possible to take soil samples from the surface using a dredger SOLAR SYSTEM RESEARCH
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and deliver them to soilreceivers of scientific instru ments for research. The MMC is equipped with a bucket for digging in the loose soil to a depth of 10– 15 cm and a drilling device that makes it possible to carry out multiple drilling of the solid (strength up to 20 MPa) soil to a depth of 10 cm. The MMC is also used to place the STEM on the ground. It may even help to solve additional technical problems. The com plex includes a manipulator camera for the selection of sampling sites and soil studies, as well as for the con trol of the loading of soil in scientific instruments. The instruments that directly explore the composi tion of the soil include ADRONEM, ABIMAS, and MGAC. The gamma spectrometer, which is part of the ADRONEM, makes it possible to determine the ele mental composition of the subsurface soil to a depth of 0.5 m by measuring secondary neutrons and gamma rays. An opportunity to do without sampling and prep aration of soil samples obtained as a result of active pulse sensing is an important advantage of the ADRONEM that provides high measurement reli ability. Devices ABIMAS and MGAC analyze samples taken using the MMC. Samples are delivered to the sample stage of the laser mass spectrometer ABIMAS or to the sample preparation system that loads the sample into the reusable pyrolytic cell of the MGAC. The complex consists of three instruments: thermal analyzer (TAM), gas chromatographer (GCHM), and mass spectrometer (NGMS). TAM performs all work on reception and process ing of soil samples. It also heats the sample and mea sures the temperature at which various volatiles emit. The instrument is based on two reusable pyrolytic cells. The GCHM carries out a subtle chemical analysis of components of the complex gas mixture released from the soil sample in the TAM and measures their absolute amount. The device has a gas distribution sys tem, adsorption storage, chromatographic capillary columns, detectors, and control electronics. The final analyzer is the mass spectrometer of neutral gases NGMS. When MGAC was designed experience of the development of the gas chromatographic complex for projects PhobosGrunt and LunaResurs was taken into account (Gerasimov et al., 2011; Gerasimov et al., 2011). A Swiss mass spectrometer (Wurz et al., 2012) with a pumping system is planned for use as a mass spectrometer. ABIMAS makes it possible to carry out massspec trometer (elemental) analysis of samples of regolith vaporized and ionized by a powerful laser pulse. In the case of the repeated evaporation the laser pulse gradu ally digs into the sample that makes it possible to investigate the substance under the changed surface. The concept of the device ABIMAS is based on the development of LASMA for the PhobosGrunt SOLAR SYSTEM RESEARCH
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project (Managadze et al., 2010) but requires evac uation. 2.5. Mars Internal Structure Seismic measurements on the surface of Mars should contribute to the solution of fundamental questions of the research of the internal structure of the planet, such as the size of the core, mantle and crust composition, and the crust thickness. These data are important for the solution of the problem of the planets' origin and laws of their evolution, as well as to answer questions about Mars tectonic activity, the nature of magnetism, the problem of water, etc. While up until now no seismicity has been detected on Mars, the history of the Earth and lunar seismology makes it possible to expect that on Mars seismology will also be the leading method in the study of the internal struc ture. The only measurements of the Viking spacecraft using the seismometer that had very limited resources made it possible to obtain only one entry similar to the seismic one. The bulk of the data was wind noise. In rare calm periods estimates of seismic signals were obtained that constitute units of µm in the frequency range of 1–8 Hz (Anderson et al., 1977). The US InSight mission planned for 2016 is almost entirely devoted to the seismic experiment. The French seismometer SEIS (VBB) has a sensitivity bet ter than 10–9 m s–2 Hz1/2 (
