Phobos Sample Return ProjectSpace Research Institute
Vernadsky Institute of GeochemistryRadioengineering and Electronics Institute
Apply Math Institute
Lavochkin Association

Goals of the Mission••••

Phobos regolith sample return,Phobos in situ study and remote sensing,Martian environment study
Mars monitoring

Peculiarities of the mission:
1. Samples return
2. Mars system science:– Martian moons (regolith, internal structure, origin, evolution),– Martian environment (dust, plasma, fields),– Mars (surface and atmosphere global dynamics)

Phobos and Deimos: similarity and difference
Dimentions

26,6x22,2x18,6 km

15,0x12,4x10,8 km

Dencity

1,9 ±0,1 g/cm3

1,8 ±0,3 g/cm3

Reflectance

0,071 ±0,012

0,068 ±0,007

Taxonomy

T (or B, or D)

D (?)

Morphology pecularities

long fossas

no fossas

Gravity

0,54 cm/c2

0,31 cm/c2

Circular orbit

R=9378 km (2,76 Rm )T=7h 39 min, i=240

R=23459 km (6,9 Rm )T=30h 21 min, i=240

Proper motion

Synchronous rotation,libration: T=10h, A=70

Synchronous rotation

Problems driving to study the Martian satellites:- origin of the Martian satellites,- nature and characteristics of the regolith (relict matter?),- difference in characteristics of the surfaces of Phobos and Deimos,- low density,- internal structure,- peculiarity of the orbital and proper motion,- dust tori ?

Scientific objections•

study physical and chemical characteristics of the Phobos regolith andsubsurface layers in situ and under laboratory conditions - these data can provide
information on properties of primordial matter of the Solar system;•study of the role played by asteroidal impacts in the formation of terrestrial
planets, in the evolution of their atmospheres, crusts, and inventories ofvolatiles;•

study of the origin of the Martian satellites and their relation to Mars - these data

can help in our understanding of their evolution and the origin of satellite systems near otherplanets;•

search of possible trace of life or paleolife;•

study of peculiarities of orbital and proper motion of Phobos, what is important for••understanding their origin, internal structure, celestial mechanics applications;study physical conditions of the Martian environment (dust, gas, plasmacomponents) what is important to study of treatment processes of small body regolith underinfluence of external conditions and creation of engineering model of the Martian environment
for future Martian missions;Monitoring of dynamic of the Martian atmosphere and seasons climatechanging.

PHOBOS SAM PLE RETURNMISSION PROFILE
Earth-Mars
cruise, TCMs

Landing
Returnmodule start
Soilsampling

SC deceleration
by means of PS
into 3-day Mars
orbit

Observation orbit
cruise. Rendezvous
and landing maneuvers

SC insertion into theobservation orbit bymeans of PS
Mars-Earth cruise
TCMs

Re-entry
Descent module braking

SC boost into thehyperbolic trajectory

Injection into theEarth orbit(H=200 km)

Descent module landingPS 1st ignition, injection
into the Earth parking orbit

PS separation
injection phase
PS 2nd ignition,
injection phase

Launch of the spacecraft and transfer into
the interplanetary trajectory

Launch:Baikonur

Base orbit:
circular, 200 km, 2,8 revolutions (4 h.)Intermediate orbit:
A=11100 km, p= 230 km, T=3,65 h. 7
revolutions (26 h.)Interplanetary trajectory:
Asymptotic velocity 3,3 km/s

LAVOCHKIN ASSOCIATION,APPL Y MATH INSTITUTE

The Earth-Mars FlightDSN
Bear Lake (Moscow), Ussuriisk,
Evpatoria

3 corrections
ΣV = 45-60 m/s

LAVOCHKIN ASSOCIATION,APPL Y MATH INSTITUTE

Insertion into the first Martian orbit

Deceleration
V~800 m/s

LAVOCHKIN ASSOCIATION,APPL Y MATH INSTITUTEOrbits around Mars

1-st intermediate orbit
P=800 km, a=79000 km,T=3 d.

2-d intermediate orbit
P=9910 km, a=79000 km, T=3,3 d.

Observation orbit
Circular, 9910 km (about 500 km
higher then the Phobos orbit),
T=8,3 h.

Quasi synchronous orbit
Similar to the Phobos orbit

LAVOCHKIN ASSOCIATION,APPL Y MATH INSTITUTESC at the QSOPhobos mass center

LAVOCHKIN ASSOCIATION,APPL Y MATH INSTITUTEApproaching Phobos and landing

12 km
T ~40 min

LAVOCHKIN ASSOCIATION,APPL Y MATH INSTITUTEShaping of the return sc orbits

LAVOCHKIN ASSOCIATION,APPL Y MATH INSTITUTE

Entry into the atmosphere and landing at the surface of the EarthLAVOCHKIN ASSOCIATION

MAIN CHARACTERISTICS OF THE MISSION

Launch site………………………………….................Baikonur Cosmodrome
Interplanetary Earth – Mars cruise time………..…....10 – 11.5 months
Interplanetary Mars – Earth cruise time.....................10.5 – 11.5 months
Mission total time………………………………….....…~ 33-34 months
SC mass………………………..………………………..8,120 kg
Scientific equipment mass……………………………..50 kg
Phobos soil samples mass……..……………….……..0.2 kg

LAVOCHKIN ASSOCIATION

P H O B O S SAM PLE RETURNSC MARS ORBIT INSERTION CONFIGURATION

Descent module

Return vehicle

Cruise module
PS

Cruise module

Insertion PS

LAVOCHKIN ASSOCIATIONPayload
Instruments for sc navigation and samplingTV-system
Mechanical device for sampling

Instruments for study of Phobos regolith and internal structure
Panoramic camera
Gas-chromatograph
Messbauer spectrometer
Gamma-spectrometer
Neutron spectrometer
Laser TOF spectrometer
Mass-spectrometer of secondary ionsIR spectrometers
Thermoprobe
Long wave radar
Seismometer

Instruments for Martian environment study
Plasma, waves and magnetic field detectors
Dust particles detector

Manipulator andsampling device

Manipulator Instrument
MESSBAUER
SPECTROMETER• pointing ±5 mm• length – till 1000 mm• presure – till 5 N• sample volume - 0,5–1,5 cm3• mass - 3,5 kg

mass 0,3кг
Source Fe57
Cooperation – IKI, “RAROS”, Lavochkin Association

Cooperation –Mainz University, Germany, IKI,

Gas-Chromatograph Complex
Device for delivery andhandling of samples

Therm.-Differenc.Analyzer
TDA (pyrolytic cells)Образец

Chromatograph
ChМS-1Mass-spectrometer
MAL-1Эталон
W2

W1

T1 T2
∆TW

Эндотермический
переход
Экзотермический
переход

∆W
T

Cooperation
IKI, GEOHI, Chromatec,Germany, France

Objectives

Mass 0,5 kg
Т till 10000

Mass 4,5 kg
Sensitivity > 10-9

Mass 3,5 kg
Mass range 1-150 а.е.м.

Investigation of the ability and chemical composition of volatile components in the soil of Phobos(bound water, organics, noble gases, etc.)•••

to measure of the quantity of individual gas components in a complex gas mixture, which is evolved from the soil sample bypyrolysis, due to their separation by the time of retention in a chromatographic columns and detection by TCD sensor.
to identifiy chemical composition of gas components by their calibrated time of retention and by spectroscopy of specificabsorption lines for H2O, CO2 , and CH4 gases.
to measure isotopic composition of C, H, and O elements by spectroscopy of specific absorption lines for H2O and CO2gases.

Nucler – physical experiments
GAMMA-SPECTROMETERPhGS

NEURTON SPECTROMETER
HEND

2

3
1

The study of the Phobos rocks
chemical composition The
measurement of the chemicalelements concentration on thePhobos surface: the rock-formed
elements (from H to Fe) and thenatural radioactive (K, Th, U) ones.

41 – module ofscintillation detector
2 – module ofneutron counter
with moderator
3 – module ofcounters of thermaland epithermal
neutron4 –module ofgammaspectrometer

Scientific tasks:- studying composition of Phobos regolith;- searching of hydrated materials or / and water ice on thesubsurface of Phobos;- development of physical model of radiation background on thesurface of Phobos and on Martian orbits

resolution – 1-2 %Range of measurement::• Neutrons– 0.4 eV – 15.0 Me V
• Gamma-rays – 100 keV – 10 Me V
Energy resolution of LaBr3 crystal 3% for 662 keV (sizeh=5,08cm d=5,08cm).

Mass 5,5 kg

Cooperation: IKI

Range of measurements 0,3 - 9,0 MeV

Cooperation: GEOHI, SNIIPMass spectrometry
Laser Time-of-flight Mass Spectrometer
LASMA

Mass Spectrometer of secondary ions
MANAGA-F

Quantitative analysis ofelemental and isotopic
composition of Phobos’
regolith at 30-50 µm
Mass range - 1-250 а.е.м.
resolution
300
Mass 1.4 kg

Cooperation –IKI, Belorussia
Cooperation
IKI,«Polus»,Mass range - 1-300 а.е.м.
resolution> 100
sensitivity 1 ppm
mass 1.4 kg.

IR - spectroscopy
Thermal Infrared Multispectral Mapper
TIMM

Fourier Spectrometer
AOST

Measurements of the Phobos thermal radiance in 35
spectral channels. The instrument produces spectral
images up to 40x40 pixels. Each pixel represents
the interferogram of the corresponding surface on
Phobos. By means of Fourier analysis, eachinterferogram is transformed to a spectrum.
Study surface mineralogy and physical properties of Phobos using
multi-spectral thermal-infrared images (7 - 15 µm).
Mapping Phobos in both day and night multi-spectral infrared
images at 0.4-1.0 km per pixel resolution.
The specific objectives(1)

determine the mineralogy andpetrology of localized deposits(1)study the surface temperatureand thermal inertia.

TIMM is imaging Fourierinterferomete
Spectral range: 625 – 1333 cm-1
Resolution 20 cm -1
Mass 2,5 kg
Cooperation IKI, Italy

Spectral range 2,5 – 25 µresolution: 0.45 cm -1
Field of view - 2.3 deg
Mass 4 kgКооперация: IKI, Italy, Germany, FranceTV cameras
TV system for observation and navigation
TSNN

F = 500 и 18 мм
Field of view 0,85х0,85 и 23,2 х 23,2
mass 1,8 и 1,2 kg

Characteristics of the matrix
Kodak-1020
1004 х 1004
Size of the elements, µм 7,4 х 7,4
Spectral range, µм 0,4 – 1,0

Panoramic TV camera
PANCAM
resolution 3 arc min.
Dynamic range 1000
Field of view 60х360 gradSpectral chanals
0.45± 0.05
0.65±0.05
0.95±0.05
Matri x 1280х1024 pix
mass 0,45 kg

Cooperation –IKI, INFR ATRON, LITMO

Sounding instruments
Seismometer
MUSS

Termoprobe
TERMOFOB

Registration of seismic signals and wave
fields of Phobos, measurement seismogravitational fluctuations on a surface ofPhobos
Internal structure and energy state ofPhobos;

Acti ve thermal measurements of Phobos
surface based on the heat conductivity
inverse problem solutions

Long waves planetary radar
DPR

Frequency range 150
150±±25 МГц
Vertical resolution 2 m
mass 3,5 kgrange 3 10-5 -10Hz
20G – 10-6G
2 – 10-4 м/с210м/с
10-3 м/с2 – 10-8 м/с2oscillator

receiverAntenna
Cooperation ,IRE

Spectral range, µm 0.45, 0.55, 0.65
Temperature range 160-380 К
Resolution 0,1 grad.
Масса 0,3 кг
Cooperation
IPhE,VNIIFTRI
NPO, IKI,
GEOHI

Cooperation AMI

Investigation of the Martian environment
Plasma-waves systemFPMS
STUDYOF PLASMA-WAVE
PROCESSES OF SOLAR
WIND INTERACTION WITH
THE MARTIAN PLASMA
Measurements: 3d distributionfunctions of protons, electrons
and ion components; quasistaticand variable magnetic fields,
electric field and plasma current
fluctuations

Micrometeorites detector
METEOR
Investigation of parameters ofmicrometeors (m, v).
Control micrometeor situation
during the flight.
Velocity range 3 до 35 km/sec
Mass range 10 –14 до 10 –6 gMass 3,5 kg

Cooperation:
GEOHI, АВЕРС, NPO
Lavochkin

Dust particle detector
DIAMOND
Registration of dust particles
in the Martian dust belts.
planetary ionsspectrometer
10 eV – 15 keVHigh energy ionsspectrometer
10 eV – 50 keVArea of the sensor 10-2 m2
Sensitivity 6,6,5⋅ 10-10 kgkg⋅⋅ m/c
Max moment 4,4,0⋅ 10 4 kgkg⋅⋅ m/c

Magnetic
field sensors

Mass 3,0 kg
Cooperation – IKI,
Hungary, Austria,
Germany, France, Holland

Cooperation:
Italy and IKI

Celestial mechanic experiments
ULTRASTABLE OSCILLATORUSOINVEST IGATION OF PROPER AND FORCED
LIBRATION OF PHOBOSLIBRATION•Investigation of internal structure of Phobos:••••

Inhomogeneity of the bodyCenter of mass and momentum of inertia
Average density
Proper and forced motion•••••Resolution:- obscure camera 1 arc min.
- star sensor 10 min.
- dynamic range 1000
Number of obscure cameras 7
Field of view – half of spherematrix 1280 х 1024 pix
mass 0,5 kg

refinement of solar system parameters (astronomical unit,orbital parameters of Mars and Phobos);
experimental estimation of Phobos lifetime on its orbit;
determination of the mass distribution inside Phobos;
refinement of masses of large asteroids from main belt;
refinement of experimental limit of the constancy (ordetection of time variations) of universal gravitational
constant;
refinement of the geometrical connection of dynamicalcoordinate system with origin in solar systemcenter of mass and quasar coordinate system
based on the measurements of relative angularcoordinates of quasars.

USO

RADIO
SYSTEMstability 10-12
mass 0,35 kg

Cooperation: – IKI,INFRATRON, LITMO

Cooperation: IKI, MARIONGROUNDBASEDSTATIONFREQUANCYSTAND ART++++

Plasma, waves, fieldMartian environment+

Dust Detector

Internal structure+Long Wave Radar

Geochemistry

Seismometer+

Neutron spectrom/+

Gamma spectrom.

Morphology

Instruments

Chromatograph

Manipulator

Science fields

Panoramic cameraRelevance of the instruments tothe mission scientific objectives++