Penetrators are separated from the spacegraft 3 to 5 days prior to the encounter with Mars, and begin their autonomous flight; probes are transferred into a descent trajectory permitting their penetration to the selected areas of Mars.
In the Martian atmosphere probes undergo aerodynamic braking, first using a rigid cone and then, air-inflated braking devic, until a given velocity is reached to provide their penetration into Martian regolith. A probe impacts with the surface at a velocity of 80 m/s with a separation of the forebody and afterbody.The penetrating part of the probe forebody carrying the scientific and housekeeping instrumentation tnters the regolith down to 506m, while the afterbody with the rest of the instrumentation remains on the surface. Scientific studies begin after penetration. Information is transmitted to the orbiter. Duration of a session is about 6 min.
36° N and 161° W (for the penetrator landing near small stations).
36° N and 125° W
Cooperation In the beginning of the chapter
Russia, Finland, Germany, Bulgaria, Roumania, Great Britain. Contact person: Surkov Yu.A. phone +7- 095-137-4763
fax +7-095-939-0186
исследование процессов, происходящих в районах внедрения зондов, таких как эоловая активность, флювиальное воздействие на поверхность, вулканизм и т.д. (съемка в разные сезоны дает информацию о динамике этих процессов).
Main characteristics:
TV-panorama is provided with a camera, using CCD spectrozonal ruler.Each channel of CCD contain 2048 sensitive elements;
TV camera is mounted at 1 m distance above the surface;
the boundaries of spectrometric ranges:
blue region- 0,44 - 0,46 mkm;
green - 0,54 - 0,56 mkm;
red - 0,69 - 0,75 mkm;
near IR - 0,96 - 1,02 mkm.
imaging is performed at the vertical angle of view 60°;
imaging is performed by the optical and mechanical package of the camera rotating around the vertical axis of the penetrator;
Objective:
to estimate the element composition of Martian surface rocks.
Gamma-radiation recorded by the instrument permits to determine the H, Na, Mg, Al, Si, K, Cl, Ca, Ti, Mn, Fe, Th, U abundances in rocks.
Method of measurements is based on recording gamma-rays from natural radionuclides K,Th, U and nuclear interaction of cosmic rays with elements of Martian rocks.
Main performance characteristics:
radiation energy range
0,3-9,0 MeV
energy resolution for E = 0,661MeV
not worse than 8%
measurement accuracy of the elemental composition of rocks:
- for major rock-forming elements
- for natural radionuclides
Objective:
to estimate the elemental composition of the subsurface rocks, including the abundance of the rock-forming elements (Mg, Al, Si, K, Cf, Ti, Fe), volatiles (S,Cl) and minor elements.
Method of measurements is based on the excitation of X-ray fluorescent radiation of rock sample using radioactive sources Fe-55 and Cd-109.
Main performance characteristics:
energy range
0,9-7,8 keV;3,0-24 keV
sensibility
0,2-0,5 W %
measurement duration
0,5hour
power consumption
1,7 W
mass
0,8 kg
Cooperation: Russia Contact person: A.G. Dunchenko, phone +7- 095-939-7088
Objective:
to estimate the element composition of the rocks, including the abundance of light elements (C, N, F) and major rock-forming elements (O, Na, Mg, Al, Si, S, K, Ca, Fe) in small-size soil sample.
Method of measurements is based on irradiation of the sample of Martian soil with -particles of an isotope sourse Cm-244 of 60 - 80 mCurie activity. The instrument records particle scattering spectra and secondary proton spectra..
Main performance characteristics:
energy range
0,8-6,3 MeV
resolution
7%
sensitivity
0,1- 0,5 W.%
data transmission rate
10 kbit/s
measurement
16 hours
power consumption
0,2 W
mass
0,35 kg
Cooperation: Russia, Germany<Россия, Германия. Contact person: H.Waenke(PI), waenke@mpch-mainz.mpg.dbp.de
Objective:
to measure humidity and density of the rocks Method of measurements is based on the recording of secondary neutrons scattered on the nuclei of rock elements.
The humidity is determined in 0,3 m3 volume of rock.
Objective:
to study the structure of the planet's crust, its stratification and heteroqeneousness.
Recording of seismic noise and natural oscillations of the planet will provide data on the inner structure and dynamics of the planet's interior.
Method of measurements is based on recording the seismic noise of the planet.
studies of Mars' intrinsic magnetic field, magnetic properties of rocks and their paleomagnetism Method of measurements is based on recording three magnetometry components on the surface of Mars
MARS-96 
