Studio AAD, 2012NASA, Mars Habitat

Elevation in meters

Stokes

Lomonosov

Milankovic v

ALBA

FOSSAE

TANTALUS FOSSAE

VA

ST I T A S B O R E

AL

IS

V

AS

TI T A S B O R E

AL

IS

SC

AN

DI A

CO

LL

ES

Korolev

P L A N U M

B O R E U M

Chasma Boreale

O LY MP I A P L A N I T I A

Kunowsky

Cydnus Rupes

Phillips

Maraldi

Von Karman

Darwin

Schmidt

Agassiz

Chamberlin

Stoney

Reynolds

Charlier

Wright

Byrd

RayleighBurroughs

Liais Huxley

Secchi

Gilbert

MitchelHolmes

Main

South

Russell

C A V I

A N G U S T IA O N I A

T E R R A

N O A C H I S

T E R R A

ARGYRE PLANITIA

P L A N U M

A U S T R A L E

T E R R A

S I R E N U M

T E R R A C I M M E R I A

P R O M E T H E I

T E R R A

M A L E A

P L A N U M

PLA

NU

MC

HR

ON

IUM

CHARI TUM M

ONTE

S

PLAN

UM

ANGUS

TUM

Barnard

S I S Y P H I

P L A N U M*

P R O M

E T HE

I PAL

NU

M*

AR

GE NT E A P L A N U M *

Aust

rale

Mon

tes*

Sisyphi Cavi

Sisyphi Montes

Pi tyusaPatera*

Pity

usa

Rup

es

V ishniac

Dor

sa

Brev

ia

Hutton

Weinbaum

Jeans

Uly

xis

Rup

esRichardson

Suess

Steno

LauSmith

Heaviside

DorsaArgentea

JolyDu Toit .

Dana Mellish

Lyell

Daly

Kuiper

TrumplerKeeler

Clark

Dokuchaev

ICARIA

FOSSAE

Lamont

Ross

Bianchini

Coblentz

AONIA

PLANUM*

Fontana

Wegener

Peneus Patera

MaleaPatera*

Amphitr i tes Patera

Axius

Valles

Mad Vallis

Heinlein

Wells

Erid

ania

Sco

pulu

s

Mendel

Chalcoporous

Rupes—

Ar gyre Rupes

PA R V A P LAN

UM

*

Thyles Rupes

Promethe i

Rup

es

Chasma Australe

Promethei Rupes

Bernard

Columbus

Dejnev

Newton

Mariner

Copernicus

PtolemaeusLi Fan

Very

:

Liu Hsin Hussey

Koval'sky

PorterLowell

Fesenkov

Sharanov

Mutch

Vinogradov

Holden

Hale

Hooke

G a l l e

Darwin

Green

Wirtz

Helmholtz

Arkhangelsky

Lohse

Vogel

Newcomb

Galilaei

Becquerel Cassini

Schiaparelli

Flaugergues

Bakhuysen

Le Verrier

KaiserProctor

Schaeberle

Terby

Russell

Krishtofovich

Tikhov

Wallace

Secchi

Arrhenius

Kepler

Molesworth

Graff

Campbell

Roddenberry

A R C A D I A

P L A N I T I A

V A S T I T A S B O R E A L I SA C I D A L I A

P L A N I T I A

C H R Y S E

P L A N I T I A

L U N A E

P L A N U M

X A N T H E

T E R R A

A M A Z O N I S

P L A N I T I A

THAR

SIS

MONTES

D A E D A L I A P L A N U M

SYRIA

PLANUMSINAI

PLANUM

SOLIS

PLANUM

VALLE S

MARINE R IS

M A R G A R I T I F E R

T E R R A

T E R R A

S A B A E A H u y g e n s

ALBA PATERA

TAN

TALU

S

FO

SSAE

MA R E O T I S

F

O S S A E

T E MP E

F O S S A E

T E M P E

T E R R A

U T O P I A P L A N I T I A

Elysium Fossae

ARCADIA

PLANIT IA

Albor Tholus

NEPENTHES MENSAE

IS IDIS

PLANIT IA

Nili

Foss

ae

SYRT IS MAJOR

PLANUM

A R A B I A T E R R A

Aram Chaos

Tharsis Tholus

Echu

s C

hasm

a

Uranius Patera

PAVONIS MONS

Cer

auni

us

Fos

sae

Ulysses Patera

Bibl is

Patera

Gordi i Dorsum

Ereb

us

Mon

tes

ARSIA MONS

CLAR

ITAS FOSSAE

Ius Chasma Melas Chasma Coprates Chasma

Candor Chasma OPHIR

PLANUMAURORAE

PLANUM

Ganges

Capri Chasma

Uzboi

Vallis

Aureum Chaos

T Y R R H E N A

Tyrrhena Patera

HE SPE R IA

PLANUM

Apol l inar is

Patera

T E R R A

C I M M E R I A

P R O M E T H E I

T E R R A

Dao

Vallis

H E L L A S

P L A N I T I A

HEL

LESP

ONT

US

N O A C H I S

T E R R ANEREIDUM

CHARITUM MONTES

A R G Y R E

P L A N I T I A

BOSPOROS

PLANUM

A O N I A

T E R R A

Thau

mas

ia

Foss

ae

ICAR IA

PLANUM

ICARIA

FOSSAE

T E R R A

S I R E N U M

S I R E N U M F O S S A E

.

CHARITUM MONTES

MONTES

Chasma

Lab

ea tis Fossa

NOCTIS LABYRINTHUS

Uly

sse s

Fos

sae

Clark

MO

NTES

Denning

Schroeter

Dawes

Antoniadi

Tikhonravov

NILOSYRTIS MENSAE

Baldet

T E R R A

ELYSIUM MONS

Herschel

Gale

Gusev

LUCUS

PLANUM

Ascuris

Planum

E L Y S I U M P L A N I T I A

THAUMASIA

PLANUM

LIBYA MONTES

Tiu Vall is

Simud Vallis

Sha

lbata

na

Valli

s

M

aja

Va

lles

Ka

sei

Valles

Eos Chasma

Al-Qahira

Val

lis

Harm

akhis

Vallis Reull V a llis

Ismeniae Fossae

Eumenides

Dorsum

Ti

u

Va l

lis

Savich

Niger Vallis

vMilankovic

A

cheron Fossae

Diacr ia Patera

.

ALB

A

F

OSS

AE

Arty

nia

Cat

ena

Cyane

Catena

Alb

a C

aten

a

Ache

ron

Cat

ena

Phl

eget

hon

C

aten

a

Perepelkin

Barabashov

TimoshenkoSytinskaya

Niloke ras Sc op

ulus

Acidal ia

Col les

Acidal ia Mensa

Sklodowska .Cyd

onia

M

ensa

e

LYOT

Semeykin .

DEUTERONILUS MENSAE

Mam

ers Valles

Cerulli Focas

Moreux

Quenisset

PROTONILUS MENSAE

Rudaux

Coloe Fossae

Renaudot

Col les Ni l i

A

uqak

uh Vallis H

uo Hsing Vallis

Mie

Hrad

Vallis

Viking 2Landing Site

Hecates Tholus Adams

Tyndall

Stokes

PHLE

GRA

MO

NTE

S

Mar

te V

allis

Pettit

Nicholson

LYCUS SULCI

OLYMPUS

MONS Olympus R upes

Olym

pus Rupes

Gigas S

ulci

Cyane Sulci

Sulci

Gordii

Olympica Fossae

Jovis Tholus

Poynting

Trac

tus

Foss

ae

Trac

tus

C

aten

a

Uranius Tholus

Ceraunius Tholus

ASCRAEUS MONS

Fort

una

Foss

ae

Sacra MensaSacra

Fossae

Sacra Fossae

Lunae

Mensa

L ob o Va

llis

Bah

ram Vallis

Stege

Chia

..

Naned

i V

alles

V iking 1Landing Si te

.Da Vinci

Ravi Vallis.

OrsonWelles*

Hydraotes Chaos

Ares V a llis

MasurskySagan

Hydaspis Chaos

McLaughlin .

Mawrth

Vallis

Curie

Trouvelot

Rutherford

Crommelin

Radau

Marth

Maggini

Gill

Luzin

Pasteur

Henry

Indus Vallis

Janssen Teisserenc de Bort .

Flammarion

Schöner .

Ni l i PateraMeroe Patera

..

Arena

Col les Peridier

Du Martheray

Amen

thes

Fos

sae

Hephaestus

Fossae

Hyblaeus Fossae

Granicus Valles

Elysium

Chasma

Eddie

Lockyer

Tartarus

Montes

Tartarus

Colles

Orc

us P

ater

a

Hibes Montes

LUCUS PLANUM

Medusae

Fossae

Williams

Burton

Comas Sola

ME MNONIA

FOSSAEMangala

Fossa

Cobres

Mangala Valles

Aganippe Fossa

Noc

tis

Foss

ae

Oudemans

Tithoniae Catena

Tithonium Chasma

Louros Valles

Hebes Chasma

Perrotin Ophir Chasma

Coprates Catena

Lassel

Juve

ntae

C

hasm

a

Sol is

Do

rsa

Fel is

Dor

sa

Mel

asD

orsa

Ibragimov

Nectaris

Fo

ssae

Ritchey

Nirgal Vallis

.

Erythraea Fossa

Lado

n Va

lles

KasimovChekalin.

Jones

Beer

Aurorae Chaos

Arsinoes Chaos

.Pyrrhae Chaos

.

Iani Chaos

Margaritifer Chaos

.Mädler

.

Wislicenus

Pollack

LambertBouguer

Cha

rybd

is

Scyll

a

Scop

ulus

Scop

ulus

Niesten .

Oenotria Scopulus

Fournier

Briault Jarry-Desloges

Millochau

Auso

nia

Mon

tes

Müller

Knobel

AEOLIS MENSAE

WienLasswitz

Hadley

Boeddicker

Reuyl

Ma'adim

de Vaucouleurs ..

Magelhaens

HipparchusEudoxus.

Nordenskiöld

Kuiper

Millman

Pickering

BrashearCoblentz

Slipher

Lampland Babakin

Douglass

Coracis

Fossae

Ogy

gis

Ru

pes

Bosp

oros

Rup

es

Halley

Oceanidum Mons

Bunge

Sumgin

Bond

Bozkir

Hartwig

Shatskiy

. .

Cha

lcop

oros

Rup

es—

Rabe

Alpheus

Col les

Hellas Chaos

CoronaeScopulus

Gledhill

Hadr iaca Patera .

Teviot

Vallis*

Morpheo s Rupes

Alexey Tolstoy

Haldane

Tycho Brahe .

Eridania Sco

pulus

Martz

Huggins

Bjerknes Cruls

Rossby

Ar iadnes Col les

Nilokeras

Fossae

Kunowsky

Nier

Vallis

AmazonisMensa*

Pathfinder Landing Si te

.

.

.

. Airy

90° W 270° W

30° W

60° W

120°

W

150° W210° W

240° W

300°

W

330° W

270° W90° W

330° W

300° W

240°

W

210° W150° W

120° W

60° W

30° W

150° 021W ° W 90° 06W ° W 30° W 330° 003W ° W 270° W 240° 012W ° W

330° 003W ° 072W ° 042W ° 012W ° W150° 021W ° 09W ° 06W ° 03W ° W

180°

0°

55°

55°

60°

60°

70°

70°

80°

80°

240°

E

210° E 150° E

120° E

90° E

60° E

30° E330° E

300° E

270° E

180°

0°

–55°

–55°

–60°

–60°

–70°

–70°

–80°

–80°

270° E 90° E

120°

E

150° E210° E

240° E

300°

E

330° E 30° E

60° E

180° 0° 180°

180°150° E120° E90° E60° E30° E

0°

150° E120° E90° E60° E30° E

180°330° E300° E270°E240° E210° E

330° E300° E270° E240° E210° E

57°

50°

30°

0°

–30°

–50°

–57°

57°

50°

30°

0°

–30°

–50°

–57°

x ––8,200 m

x 14,028 m

21,229 m

18,225 m

xx

xx14,058 m

xx

17,761 mxx

500

050

010

00

2000 1000 1000500 5000 2000 KILOMETERS

0°±20°±40°

±57°

90°

70°

55°

90°

70°

55°

5000

5001000

–90°–70°–55°

–90°–70°–55°

CONTOUR INTERVAL 1000 METERS0°

±20°±40°

±57°

North

South

East

Wes

t

NORTH POLAR REGION

SOUTH POLAR REGION

MAPPING MARS001

B C’AD E

EARTH

1 YEAR = 365 DAYS 1 YEAR = 686 SOLS

MARS

DIST TO EARTH: 54–401 million km

BASIC INFORMATION: MEAN RADIUS: 3388.0 km

MASS: 0.108 (Earth=1)

DENSITY: 3.94 (g/cm^3)

GRAVITY: 0.380 (Earth=1)

ORBIT PERIOD: 686.98 (Earth days)

ROTATION PERIOD: 1.026 (Earth days)

SEMIMAJOR AXIS OF ORBIT: 1.524 au

ECCENTRICITY OF ORBIT: 0.093

PRESSURE COMPARISON

Where Pressure

Olympus Mons summit 0.03 kilopascals (0.0044 psi)

Mars average 0.6 kilopascals (0.087 psi)

Hellas Planitia bottom 1.16 kilopascals (0.168 psi)

Armstrong limit 6.25 kilopascals (0.906 psi)

Mount Everest summit[11] 33.7 kilopascals (4.89 psi)

Earth sea level 101.3 kilopascals (14.69 psi)

24h24h27m

686 DAYS (687 SOLS)

23.44°25.19°

SUNLIGHT44% OF EARTH

C’ C D’ A’ E ’ B ’

ATMOSPHERE

SEASONS

ROCKS & SOIL

ICE & WATER

ELEMENTS

LIGHT&RADATION

Trace amounts of

methane was recently detected, which may indicate the presence of life on Mars, but may also be produced by a geochemical process, volcanic or hydrothermal activity.

CO295.32%

The atmosphere of Mars is relatively thin and is composed of

Other elemental gases found in the Martian atmosphere:

N2: 2.7%Ar: 1.6%O2: 0.13%CO: 0.08%H2O: 0.021%NO: 0.01%Ne: 0.00025%HDO: 0.000085%Kr: 0.00003%Xe: 0.000008%

O, Oxygen Si, Silicon Fe, Iron Mg, Magnesium Ca, CalciumS, Sulfur Al, Aluminum Na, Sodium K, Potassium Cl, Chlorine

MINERALS OF ABUNDANCE

SOIL COMPOSITION

O, Oxygen Si, Silicon Fe, Iron K, Potassium Ca, CalciumMg, Magnesium S, Sulfur Al, Aluminum Cs, Cesium

40 - 45% 18 -25% 12- 15%8% 3 - 5% 3 - 6% 2 - 5% 2 - 5% 0.1 - 0.5%

Periodic Table of the Elements

1

1

H

Hydrogen 1.007 94

Atomic Number 6

C

Carbon 12.0107

Symbol

Name

Average Atomic Mass

Group 18

Group 2

Group 13 Group 14 Group 15 Group 16 Group 17

2

He

Helium 4.002 60Group 1

2

3

Li

Lithium 6.941

4

Be

Beryllium 9.012 182

5

B

Boron 10.811

6

C

Carbon 12.0107

7

N

Nitrogen 14.0067

8

O

Oxygen 15.9994

9

F

Fluorine 18.998 4032

10

Ne

Neon 20.1797

3

11

Na

Sodium 22.989 769 28

12

Mg

Magnesium 24.3050

13

Al

Aluminum 26.981 5386

14

Si

Silicon 28.0855

15

P

Phosphorus 30.973 762

16

S

Sulfur 32.065

17

Cl

Chlorine 35.453

18

Ar

Argon 39.948Group 3 Group 4 Group 5 Group 6 Group 7 Group 8 Group 9 Group 10 Group 11 Group 12

4

19

K

Potassium 39.0983

20

Ca

Calcium 40.078

21

Sc

Scandium 44.955 912

22

Ti

Titanium 47.867

23

V

Vanadium 50.9415

24

Cr

Chromium 51.9961

25

Mn

Manganese 54.938 045

26

Fe

Iron 55.845

27

Co

Cobalt 58.933 195

28

Ni

Nickel 58.6934

29

Cu

Copper 63.546

30

Zn

Zinc 65.409

31

Ga

Gallium 69.723

32

Ge

Germanium 72.64

33

As

Arsenic 74.921 60

34

Se

Selenium 78.96

35

Br

Bromine 79.904

36

Kr

Krypton 83.798

5

37

Rb

Rubidium 85.4678

38

Sr

Strontium 87.62

39

Y

Yttrium 88.905 85

40

Zr

Zirconium 91.224

41

Nb

Niobium 92.906 38

42

Mo

Molybdenum 95.94

43

Tc

Technetium (98)

44

Ru

Ruthenium 101.07

45

Rh

Rhodium 102.905 50

46

Pd

Palladium 106.42

47

Ag

Silver 107.8682

48

Cd

Cadmium 112.411

49

In

Indium 114.818

50

Sn

Tin 118.710

51

Sb

Antimony 121.760

52

Te

Tellurium 127.60

53

I

Iodine 126.904 47

54

Xe

Xenon 131.293

6

55

Cs

Cesium 132.905 4519

56

Ba

Barium 137.327

57

La

Lanthanum 138.905 47

72

Hf

Hafnium 178.49

73

Ta

Tantalum 180.947 88

74

W

Tungsten 183.84

75

Re

Rhenium 186.207

76

Os

Osmium 190.23

77

Ir

Iridium 192.217

78

Pt

Platinum 195.084

79

Au

Gold 196.966 569

80

Hg

Mercury 200.59

81

Tl

Thallium 204.3833

82

Pb

Lead 207.2

83

Bi

Bismuth 208.980 40

84

Po

Polonium (209)

85

At

Astatine (210)

86

Rn

Radon (222)

7

87

Fr

Francium (223)

88

Ra

Radium (226)

89

Ac

Actinium (227)

104

Rf

Rutherfordium (261)

105

Db

Dubnium (262)

106

Sg

Seaborgium (266)

107

Bh

Bohrium (264)

108

Hs

Hassium (277)

109

Mt

Meitnerium (268)

110

Ds

Darmstadtium (271)

111

Rg

Roentgenium (272)

112

Uub*

Ununbium (285)

114

Uuq*

Ununquadium (289)

116

Uuh*

Ununhexium (292)

Phy

sica

l pro

per

ties

http://pubs.usgs.gov/sim/2005/2888/

http://en.wikipedia.org/wiki/Periodic_table-

fti.neep.wisc.edu/neep533/.../lecture19.pdf-

http://www.agu.org/pubs/crossref/2003/2003JE002060.shtml

Mars has an axial tilt of

25.2°.

middle atmosphere

upper atmosphere

~200km~500km

thermosphere

~80km

mesophere

~50km

stratosphere

`10km

~45km

lower atmosphere

~10kmthin ice clouds

ozone layercirrus clouds

cummulus clouds ~0km

A Comparison of the Atmospheres of Earth and Mars

Earth MarsThe scale height of the atmosphere is about 11 kilometres (6.8 mi), somewhat higher than Earth's 7 km. The atmosphere is quite dusty, giving the Martian sky a light brown or orange color when seen from the surface; data from the Mars Exploration Rovers indicate that suspended dust particles within the atmosphere are roughly 1.5 micrometres across. Mars's atmosphere as observed in layers:

Lower atmosphere: This is a warm region affected by heat from airborne dust and from the ground.

Middle atmosphere: Mars has a jetstream, which flows in this region.

Upper atmosphere, or thermosphere: This region has very high temperatures, caused by heating from the Sun. Atmospheric gases start to separate from each other at these altitudes, rather than forming the even mix found in the lower atmospheric layers.

Exosphere: Typically stated to start at 200 km and higher, this region is where the last wisps of atmosphere merge into the vacuum of space. There is no distinct boundary where the atmosphere ends; it just tapers away.

Source: Robbins, Stuart J.; et al. ,2006 "Elemental composition of Mars' atmosphere". Case Western Reserve University Department of Astronomy.

Potential Uses

The atmosphere of Mars is a resource of known composition available at any landing site on Mars. It has been proposed that human exploration of Mars could use carbon dioxide (CO2) from Martian atmosphere to make rocket fuel for the return mission. Mission studies that propose using the atmos-phere in this way include the Mars Direct proposal of Robert Zubrin and the NASA Design reference mission study. Two major chemical pathways for use of the carbon dioxide are the Sabatier reaction, converting atmospheric carbon dioxide along with additional hydrogen (H2), to produce methane (CH4) and oxygen (O2), and electrolysis, using a zirconia solid oxide electrolyte to split the carbon dioxide into oxygen (O2) and carbon monoxide (CO).

The incidence of the solar radiation on the surface of a planet depends on: 1. atmospheric turbitity 2. planetary latitude 3. planetary seasons

During the great martian dust storm of 1971, the daily insolation in the planet decreased because the global atmospheric turbitity increased and consequently, the temperature of the atmosphere too. It is expressed as

I0= incidence of solar radiation per cm2 (cal/cm2) (planetary day)

S0= solar constant. distance from the sun to earthr = instantaneous dist from sun to mars that is determined by planet’s semimajor axis and eccentricity of the planetAe = semi major axis of the earth’s orbitz = zenith angle of the incident solar radiation, depending on planetary latitude, solar declination and local hour angle of the sun

Mars has experienced extensive cyclical variation in the intensity and distribution of incidence solar radiation.

Variation of obliquity = 14.9º to 35.5ºVariation of eccentricty = 0.004 to 0.741

0º northern hemisphere, vernal equinox90º northern hemisphere summer solitisce180º northern hemisphere, autumn equinox270º northern hemisphere winter solstice (angle of declination of the sun)

Maximum radiation in the Northern and Southern Poles because of the continuous daylightin Martian poles: S: 600 cal/cm2 N: 400 cal/cm2

in Earth poles: S: 1100 cal/cm2 N: 1000 cal/cm2

Clear sky conditions: Greater insolation in the soutern polar region than the northern, thus southern winter is longer and colder.

Solar radiation incident at top of Martian Atmosphere

SOLAR LONTITUDE (SEASON)

600 100

270º180º90º

0

100

100

300

300

35030

0200

350

350

350

200

200

0º9080706050403020100102030405060708090

360º

500400

LATI

TUD

E

0

0

100

300

30020

0

200

9080706050403020100102030405060708090

270º180º90º0º 360º

100

500400

Solar radiation incident on Martian surface


LATI

TUD

E

100300 2000

Middle conditions: Maximum incidence in the equator.

9080706050403020100102030405060708090

270º180º90º0º 360º



100200

200

150

150

325200

100

100

100

50

5050

0

Martian dust storms: Maximum insolation in the tropics, and only small amounts of solar radiation are reaching the polar regions.



LATI

TUD

E

9080706050403020100102030405060708090

270º180º90º0º 360º

101520

35

40

0 1020

0

00

I0 = (S0 / (r/Ae)2) cos z

Season Sols Days Northern Spring, Southern Autumn: 193.30 92.764Northern Summer, Southern Winter: 178.64 93.647Northern Autumn, Southern Spring: 142.70 89.836Northern Winter, Southern Summer: 153.95 88.997

This implies that there are seasons on Mars, like on Earth. The eccentricity of Mars' orbit is 0.1, ( Earth's 0.02). The large eccen-tricity causes the insolation on Mars to vary as the planet orbits the Sun. As on Earth, Mars' obliquity dominates the seasons but deu to the large eccentricity, winters in the south are long and cold while those in the North are short and warm.

Like Earth, the obliquity of Mars undergoes periodic changes which can lead to long-lasting changes in climate. Once again, the effect is more pronounced on Mars because it lacks the stabilizing influence of a large moon. As a result the obliquity can alter by as much as 45°. The effects of these periodic climate changes can be seen in the layered nature of the ice cap at the Martian north pole. Current research suggests that Mars is in a warm interglacial period which has lasted more than 100,000 years.

Because the Mars Global Surveyor was able to observe Mars for 4 Martian years, it was found that Martian weather was similar from year to year. Any differences were directly related to changes in the solar energy that reached Mars. Scientists were even able to accurately predict dust storms that would occur during the landing of Beagle 2. Regional dust storms were discovered to be closely related to where dust was available.

The dark areas of Mars are characterised by the mafic rock-forming minerals olivine, pyroxene, and plagioclase feldspar.

The mineral olivine occurs all over the planet, but some of the largest concentrations are in Nili Fossae, an area containing Noachian-aged rocks. Another large olivine-rich outcrop is in Ganges Chasma, an eastern side chasm of Valles Marineris (pictured). Olivine weathers rapidly into clay minerals in the presence of liquid water. Therefore, areas with large outcroppings of olivine-bearing rock indicate that liquid water has not been abundant since the rocks formed.Pyroxene minerals are also widespread across the surface. Both low-calcium and high-calciumpyroxenes are present, with the high-calcium varieties associated with younger volcanic shields and the low-calcium forms more common in the old highland terrain. Because enstatite melts at a higher temperature than its high-calcium cousin, some researchers have argued that its presence in the highlands indicates that older magmas on Mars had higher temperatures than younger ones.

Due to the thin atmosphere on mars and the lack of magnetic field around it, Mars is highly vulnerable from space, mainly

solar and cosmic rays.

Sedimentary rocksCross-bedded sandstones inside Victoria Crater.

Layered sedimentary deposits are widespread on Mars. These deposits probably consist of both sedimentary rock and poorly indurated or unconsoli-dated sediments. Thick sedimentary deposits occur in the interior of several canyons in Valles Marineris, within large craters in Arabia and Meridiani Planum (e.g. Henry Crater ), and probably comprise much of the deposits in the northern lowlands (e.g., Vastitas Borealis Formation). The Mars Exploration Rover Opportunity landed in an area containing cross-bedded (mainly eolian) sandstones. Fluvial-deltaic deposits are present in Eberswalde Crater and elsewhere, and photogeologic evidence suggests that many craters and low lying intercrater areas in the southern highlands contain Noachian-aged lake sediments.

New estimates of water ice on Mars suggest there may be larger reservoirs of underground ice at non-polar latitudes. The map here shows “water-equivalent hydrogen”. Oranges and redson the map (values greater than weight 4.5 % water-equivalent hydrogen at the surface) point out areas where the amount of deeply buried water ice is greater than what can fit in the pore spaces of the surface rocks.

The deep blue areas in the polar regions are believed to contain up to

in the upper 1m of the soil.

50% water ice

0.0 1.5 3.0 4.5 6.0

90

45

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-90

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Observations by NASA's 2001 Mars Odyssey spacecraft show a global view of Mars in intermediate-energy, or epith-ermal, neutrons. Soil enriched by hydrogen is indicated by the deep blue colors on the map, which show a low intensity of epithermal neutrons. Progressively smaller amounts of hydrogen are shown in the colors light blue, green, yellow and red. The deep blue areas in the polar regions are believed to contain up to 50 percent water ice in the upper one meter (three feet) of the soil. Hydrogen in the far north is hidden at this time beneath a layer of carbon dioxide frost (dry ice). Light blue regions near the equator contain slightly enhanced near-surface hydrogen, which is most likely chemically or physically bound because water ice is not stable near the equator. The view shown here is a map of measurements made during the first three months of map-ping using the neutron spectrometer instrument, part of the gamma ray spectrometer instrument suite. The central meridian in this projection is zero degrees longitude. Topo-graphic features are superimposed on the map for geo-graphic reference.

Source: http://photojournal.jpl.nasa.gov/catalog/PIA03800

ASA's Mars Reconnaissance Orbiter (MRO) data have recored evidence of CO2 snowfalls on Mars, unveiling the only known example of CO2 snow falling in our solar system.

CO2 freezes at -125ºC to become what is known as dry ice. The recent discovery established clouds that are composed of CO2 - flakes of Martian air - which are thick enough to result in snowfall accumulation at the surface. The snow falls occurred from clouds around the south pole in winter (NASA's Phoenix Lander mission in 2008 observed falling water-ice snow on northern Mars.) The new analysis based on data from observations in the south pole during southern Mars winter in 2006-07, identifys a tall CO2 cloud about 500 km diameter persisting over the pole and smaller, shorter-lived, lower-altitude CO2 ice clouds at latitudes from 70 to 80 degrees south.

Mars' south polar residual ice cap is the only place on Mars where frozen CO2 persists on the surface year-round. How the CO2 from Mars' atmosphere gets deposited is still in question. These results shows that snowfall is espe-cially vigorous on top of the residual cap.The finding of snowfall could mean that the type of deposition - snow or frost - is somehow linked to the year-to-year preservation of the residual capSource: Nasa News Room, released : 11 Sep 2012

DRY ICE SNOWFALL ON MARS

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SOUTHERN POLAR CAP1000 km

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RESIDUAL CAP

WINTER CAP (DRY ICE)

(OUTLINE SHOWS WATER ICE CAP UNDERGROUND)

SWEDEN

MARCHAPRIL

MAY

JUNE

JULYAUGUST

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INITIAL CRYSTALIZATIONEUTECTIC STAGE FULLY CRYSTALIZED

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SULPHIDE CORE SENARIOSulphur 14-16 % (by weight)

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COMPLETELY MOLTEN CORE

Just like the core of the earth the core of mars is under transformation. The final stage of this transformation is a completely crystalized, solid core. The graphic show two different senarios of this transformation depending on the amount of sulphur in the core

(The crust of the Earth is only one third as thick as Mars's crust, relative to the sizes of the planets.)

CRUST THICKNESS

80km (max)

35km (min)

40km (avg)

Just like Earth, Mars is a Terrestrial planet. Mean-ing that they have approximately the same type of structure: a central metallic core, mostly iron, with a surrounding silicate mantle. The crust of Terres-trial planets have canyons, craters, mountains, and volcanoes.

EARTH

OXYGEN

SILICON 27.7%

ALUMINIUM 8.1%

IRON 5.0%

CALCIUM 3.6%

SODIUM 2.8%

POTASSIU

M 2

.6 %

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NESIU

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SOIL COMPOSITION

MARS

OXYG

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SILICON 27.7%

ALUMINIUM 8.1%IRON 5.0%

CALCIUM 3.6%

SODIUM

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FACTORSCONDITIONS

VOLCANOESVALLEYS

PLAINSCRATERS

SAND DUNESPOLAR CAPS

EQUATORIAL

L owest ni httime temperature [K ]

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H ighest daytime temperatures during one M ars year [K ]1 61 126 193 257 317 371 421 468 514 562 612 668

Ls 0 30 60 90 120 150 180 210 240 270 300 330 350

φ87654321012345678

K303293283273263258253243213203183173163153148143

°C302010

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L egend

of Martian surface is covered by volcanic areas

10%

Ancient cratered terrain

Presence of fewer impact craters

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Olympus Mons

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Mount Everest

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Relief in Mars: 29km Relief in Earth: 20km

Highest point in Mars

Lowest point in Mars

Lowest point in Earth

Highest point in Earth

E’ x100 vertical exaggerationE C’ C D’ D B’ BA’A

ATMOSPHERE& CLIMATE

RADIATION

CORE

1 Gullies, streaks, ripples and dust devil tracks on Russell Crater Dunes. 2 Exposure of Layers and Minerals in Candor Chasma. Cliff along a layered deposit in Valles Marineris. Erosion by wind has carved V-shaped patterns along the edges of layers.

3 Victoria Crater at Meridiani Planum(~ 800m). Layered sedimentary rocks are exposed along the inner wall of the crater, and boulders fallen from the crater wall are visible on the crater.

4 Dark sand cascades down top of dunes leaving dark surface streaks - streaks that might appear at first to be trees standing in front of the lighter regions.

5 Part of the Abalos Undae dune field. The sands appear blueish because of their basaltic composition, while the lighter areas are probably covered in dust.

6 A 4 km diameter "swiss cheese" terrain typical of the south polar cap. The bright areas in this image are covered by carbon dioxide frost.

7 Avalanches on Mars' North Polar Scarps. Material, likely including fine-grained ice, dust and large blocks, has detached from a towering cliff and cascaded to the gentler slopes below.

8 Dunes in a crater in Newton Basin that are eroding or covering a more coherent rock structure below.

9 Fuzzy-looking landscape near Tharsis Montes. The out-of-focus regions indicates an extremely smooth surface, which is due to a thick layer of dust blanketing the landscape.

10 A valley in Elysium region volcanic rise region. 11 Scalloped sand dunes in the southern hemisphere, displays seasonal frost on S-facing slopes, highlighting some regular patterns, as the frost forms only on parts of the ripples.

12 Serpent Dust Devil of Mars by HiRISE camera on NASA Mars Reconnaissance Orbiter. 13 Intersecting swirling trails left by the earlier passage of dust devils across sand dunes, as they lifted lighter reddish-pink dust and exposed the darker material below.

14 A large barchan (crescent-shaped) dune, in a region where some dunes have been observed shrinking over several years.

15 Linear dunes in the north polar region. Networks of cracks between the linear dunes and may indicate that ice-rich permafrost is present or was geologically present recently.

16 The dark fans of dust seen in this image comes from the surface below the layer of ice, carried to the top by gas venting from below. Bright streaks in this image are fresh frost.

GLACIERS

NORTH POLE

During the summer, the caps recede but never com-pletely disappear. The permanent cap at the Martian north pole is formed not of dry ice, but of water ice. The residual north polar cap has been measured to be about 1000 km in diameter with a thickness of about 3 km.

SOUTH POLE

The south polar cap is much smaller, ~350 km in size and thicker than the north cap. It is formed of dry ice with an unknown thickness of water ice. Here, the temperature never gets above 150K, so the dry ice survives the summer. The caps are different because of the eccentricity of the Martian orbit which is over five times that of the Earth, and larger than all planets except Mercury and Pluto. This results in the planet being significantly further from the sun during summer at the south pole.

NORTHERN POLAR CAP

SOUTHERN POLAR CAP

1000 km

If the ice from the south pole was distributed uniformly over the Martian surface, it would cover the planet 36 feet deep in liquid water. But the flood plains seen on the surface suggest that there was over 10 times as much water originally present on Mars.

EQUATORIAL

Recent discovery of the presence of water ice in the euquatorial belt of Mars has lead to change in directioin of rover missions. Studies of water on Mars can now be carried out in the more tolerable climate in the Equator, where previous studies were made inaccesible in the polar regions by its harsh climate.

The Medusae Fossae Formation is a soft, easily eroded deposit that extends for nearly 1,000 km along the equator of Mars

Due to the thin atmosphere on Mars and no mag-netic field around it, Mars is highly vulnerable to radiation from space, namely solar radiation and cosmic rays.

DUST DEVILS

Dust devils occur when the sun warms up the air near a flat, dry surface. The warm air then rises quickly through the cooler air and begins spinning while moving ahead. This spinning, moving cell may pick up dust and sand and leave behind a clean surface. Martian dust devils can be up to fifty times as wide and ten times as high as terrestrial dust devils, and large ones may pose a threat to terrestrial technology sent to Mars. Dust devils have been reported to clean dust of the solar panels of two Rovers in Mars, restoring power levels and exapanding work productivity.

These dune fields cover an area the size of Texas in a band at the edge of Mars' north polar cap. Most data suggested they were fairly static, but new satellite observations have shown that towering sand dunes are actually dynamic and active.

MOVEMENT OF SAND

The dunes are covered by a seasonal CO2 frost that forms in early autumn and remains until late spring. Grainflow is triggered by when the CO2 frost sublimes seasonally.

This gas flow destabilizes the sand on Mars' sand dunes, causing sand avalanches and creating new alcoves, gullies and sand aprons on Martian dunes. In some places, hundreds of cubic yards of sand have avalanched down the face of the dunes.

Polar caps on Mars changes dramatically with the seasons. In winter, the caps become much larger as CO2 freezes on the surface . This happens when the temperature drops to about 150K, and the cap extends down to about latitude 50° by the beginning of spring.

oerkeokroeakrpeare iejrieamo

Image Credit: HiRISE, MRO, LPL (U. Arizona), NASA

Effusive eruptions

SIZE

THARSIS PLANITA VALLES MARINERIS

SIZEFEATURES FEATURES FEATURES

10-100X

largerthan earth volcanoes

Magma chambers larger than in earth

Flows longer than in earth

1-2km 2000km

across long

Rivers, lakes and deltas

Quiet volcanic eruption/ basaltic lava / explosive ash eruption

(longer than valley)CHANNELS

VALLEYS

Probably formed by release of water from lakes and explosive eruptions of groundwater

Dry; resembles terrestial river. Systems probably formed by slow erosion of running water

NORTHERNPLAINS

VOLCANICPLAINS

Little relief;Probably formed by oceans and its surface is composed of sediments.e.g. Utopia Planita, Chryse Planita

Composed of lava flowseg. Tharsis Planita

It is a large plain of volcanic rock, measuring more than 8000km across and up to 8km in height. It is the center of volcanic activity on Mars.

Several interconnected canyons.Formed by erosion, but mostly by deformation of crust.

HELLAS PLANITACraters in old surfaces are more erodedØ: 7000 kmdepth: 8 km

CUENCA BOREALISCraters in young surfaces are lesserodedØ: 8500 km

OLYMPUS MONS ASCRAEUS MONS

PAVONIS MONS MOUNT EVERESTMAUNA LOA

ARSIA MONS

Ø: 624 km

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Mauna Loa

Olympus Mons

Everest

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Olympus mons is the highest peak in solar system.

Sea level

Hecates Tholus

Elysium Mons

Albor Tholus

ELYSIUM PLANITAA smaler volcanic rise, measuring 2000km across and 6 km high. Main volcanoes:

Ø: 180 kmht: 7 km

240 km15 km

160 km4.5 km

Vertical scale exagerated 4 times

Valles Marineris

Depth: 7 km Length: 4000 km

Width: 200 km

Grand Canyon Colorado

Depth: 1.6 km Length: 446 km

Width: 6-29 km

Valles Marineris

USA

FEATURES FEATURES ICE AND WATER ON MARS

NORTHERNHEMISPHERE

SOUTHERNHEMISPHERE

Sparsely crateredeg. Cuenca Borealis(Formed ~3900 mil years ago)

Heavily crateredeg. Hellas Planita (Largest impact on mars)

Though Mars is smaller than Earth, its reliefs are larger than Earth’s. Also, Mars has larger land mass when as compared to Earth.

hot rock

cold rock

less density

more density

push the surface up

pull the surface down

MANTEL CONVECTION

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ELYSIUM PLANITIA

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TYRRHENA PATERA

SABIS VALLISABUS VALLIS

MAMERS VALLIS

APSUS VALLISTINJAR VALLIS

HERBUS VALLIS

HECATES THOLUS

HECATES THOLUSASCRAEUS MONS

PAVONIS MONS

ARSIA MONS

UTOPIA PLANITIA

MOREUX DUNES

GALLE DUNES

SAND DUNES

SEA OF SAND

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Mars dust storms are of great interest to scientists. Even though several space-craft have observed the storms first hand, scientists are no closer to a definitive answer. For now, the storms on Mars are going to continue to present chal-lenges to planning a human mission to the planet.

All dust storms on Mars, no matter what size, are powered by sunshine. Solar heating warms the martian atmosphere and causes the air to move, lifting dust off the ground.

Because the martian atmosphere is thin--about 1% as dense as Earth's at sea level--only the smallest dust grains hang in the air. Airborne dust on Mars is about as fine as cigarette smoke.

Dust storms often begin in Hellas Basin, the biggest hole in the ground in the entire solar system ( 6 km deep and 2000 km across), Over the years since it has accumulated plenty of dust, and because the basin is so deep, air at the bottom is about 10 degrees or so warmer than air at the top. This gradient drives winds, which can carry dust all the way out of the crater, and envelops up to a quarter of the Martian surface.

It was also reported that an enormous dust storm that exploded on Mars in 2001, which shrouded the planet in haze and raised the temperature of its upper atmosphere 30 deg. C.(article-Planet Gobbling Dust Storms (Science@NASA))

RECONSTITUTING SANDa self-constructing air-born(e) typology

Dolly Foo

<what to build with>

The atmosphere of Mars is a resource of known composition avail-able at any landing site on Mars. It has been proposed that human exploration of Mars could use carbon dioxide (CO2) from Martian atmosphere to make rocket fuel for the return mission.Two major chemical pathways for use of CO2 are the Sabatier reaction, con-verting atmospheric CO2 along with additional hydrogen (H2), to produce methane (CH4) and oxygen (O2), and electrolysis, using a zirconia solid oxide electrolyte to split the carbon dioxide into oxygen (O2) and carbon monoxide (CO).

<Material study>

Sand, dust and powderWhat is the composite of Marsian sand, what are the properties, how different it is from sand on earth. Also study the extend and periods of sandstorm and how it affects NASA’s explorations. Identify similar conditions on Earth for case study. Study sand and its structural properties in existing constructional technology. <Topological study>

Features on Mars – sand dunes, volcanoes, tunnels, Hellas Planita, equatorial belt, wind patterns, heating patterns

C

This is a perspective view of the Nili Patera dune �eld. A HiRISE image has been draped over a digital elevation model of Mars. Colors corre-spond to the amplitude of the ripple's displacement extracted by image correlation between two HiRISE observations separated by 105 days. Cool colors (blue) correspond to less than 75 cm of displacement whereas warm colors (red) correspond to 4.5+ meters.

3D PRINTING WITH SANDCase study: ETH Digital Fabrications and Robotic Systemshttp://www.dfab.arch.ethz.ch/web/e/forschung/index.html

Flight Assembled Architecture, 2011-2012, FRAC Centre OrléansFlight Assembled Architecture is the first architectural installa-tion assembled by flying robots, free from the touch of human hands. The installation is an expression of a rigorous architec-tural design by Gramazio & Kohler and a visionary robotic system by Raffaello D’Andrea. Flight Assembled Architecture consists of over 1.500 modules which are placed by a multitude of quadrotor helicopters, collaborating according to mathematical algorithms that translate digital design data to the behavior of the flying machines. In this way, the flying vehicles, together, extend them-selves as “living” architectural machines and complete the com-position from their dynamic formation of movement and building performance. Within the build, an architectural vision of a 600m high “vertical village” for 30’000 inhabitants unfolds as model in 1:100 scale. This newly founded village is located in the rural area of Meuse, taking advantage of an existing TGV connection that brings its inhabitants to Paris in less than one hour. It is from this quest of an “ideal” self-sustaining habitat that the authors pursue a radical new way of thinking and materializing verticality in architecture, Flight Assembled Architecture.

<SAND + ROBOTICS = FLIGHT ASSEMBLED ARCHITECTURE>

SALTATION OF SAND

Image credit: Bagnold’s illustration on salation of sand

From the Latin verb “to jump,” this is the process whereby sand grains move in the wind by individual leaps, and, landing on a hard surface, bounce off again; if a grain lands amongst other grains on the surface of a dune, the impact kicks some of them up into the wind and the crowd of flying grains grows. It is these two contrast-ing behaviours – bouncing versus splashing – that explain the self-accumulating nature of dunes. Over a hard surface of rocks and pebbles, the trajectories of individual grains are high into the air, and they keep on bouncing. As soon as they hit a soft surface of a dune, they kick off more grains, but the trajectories are lower and shorter – the dune grows.

How strong a wind is necessary to move sand? The threshold velocities of the wind.Why do dunes form at all? Why is the sand not spread evenly over the desert floor? Whether on Earth or Mars (or, indeed, Venus or Titan), dunes appear to be self-accumulating, seeming to vacuum up sand from the bare stony areas between them – they grow by attracting more sand. “Why did they absorb nourishment and continue to grow instead of allowing the sand to spread out evenly over the desert as finer dust grains do?” was one of Bagnold’s questions. This was, he thought, something that “could be explored at home in England under laboratory-controlled conditions” - and so began his rigorous science. Two of the most important revela-tions of Bagnold’s work are the process of saltation and the role of two different threshold velocities for the wind.

SAND BAGSThe project – a kind of bio-architectural test-landscape – would thus "go from a balloon-like pneumatic structure filled with bacillus pasteurii, which would then be released into the sand and allowed to solidify the same into a permacultural architec-ture."

Different types of construction methods involving pile systems that could probably be used to get the bacteria down into the sand – a procedure that would be analogous to using an over-sized 3D printer, solidifying parts of the dune as needed. The piles would be pushed through the dune surface and a first layer of bacteria spread out, solidifying an initial surface within the dune. They would then be pulled up, creating almost any conceivable (structurally sound) surface along their way, with the loose sand acting as a jig before being excavated to create the necessary voids. If we allow ourselves to dream, we could even fantasise about ways in which the wind could do a lot of this work for us: solidifying parts of the surface to force the grains of sand to align in certain patterns, certain shapes, having the wind blow out our voids, creating a structure that would change and change again over the course of a decade, a century, a millenium.

<SAND + BACTERIA = BIO- ARCHITECTURAL LANDSCAPE>

BACTERIA AS GLUECase study: Dune, Magnus Larsson(http://www.magnuslarsson.com/architecture/dune.asp)

A particular microorganism, Bacillus Pasteurii, is flushed through the dunescape (an analogy could be made to an over-sized 3d printer), which causes a biological reaction that turns the sand into solid sandstone. The initial reactions finish within 24 hours; it would take about a week to saturate the sand enough to make the structure habitable. The bacteria are non-patogenic and die in the process of solidifying the sand. This part of the project relies upon research carried out by professor Jason De Jong's team at the Soil Interactions Labo-ratory, UC Davis (http://www.sil.ucdavis.edu/people-jason.htm)

Dust storm on Mars. Image credit: NASA/JPL

ACOUSTIC LEVITATION - DISLODGING MARTIAN DUST

<SAND + SONAR = ACOUSTIC LEVITATION>

Finding ways of dealing with the fine dust is a high priority because the problems it can cause could drastically affect any long-term exploration. The thin atmosphere on Mars means dust particles are not as rounded as they would be on Earth and can remain quite sharp and abrasive, and they have a high electrostatic charge, which means the fine dust clings to everything and can penetrate space suit air locks, and make solar panels inoperable. The researchers from the Department of Physics and Materials Science Program carried out a feasibility study to develop an acoustic dust removing system for use in space stations or habitations on the Moon or Mars. They found a high-pitched (13.8 kHz, 128 dB) stand-ing wave of sound emitted from a 3 cm aperture tweeter and focused on a reflector 9 cm away was strong enough to dislodge and move extremely fine (<2 µm diameter) dust particles on the reflector surface. The sound waves overcome the van der Waals adhesive force that binds dust particles to the surface, and creates enough pressure to levitate the dust, which is then blown away. The team tested the system on a solar panel coated with mock lunar and Martian dust. The output of the clean panel was 4 volts, but when coated with dust it produced only 0.4 volts. After four minutes of acoustic levitation treatment the output returned to 98.4% of the maximum. Study co-author Junrun Wu said acoustic levitation is not new, but this is the first time it has been considered for applications away from Earth. The technology is cheap and uses readily found parts, but there is one enormous problem: it will only work when it is sealed inside a space station or other habitation. It will not work where there is no atmosphere (such as the moon) or where the atmosphere is low pressure and thin (such as Mars) because sound is a pressure wave that travels through the air. This limits its usefulness because inside an enclosed space station there would be relatively little dust, and probably other readily-available means of removing it without resorting to acoustic levita-tion.

The paper is published in the Journal of the Acoustical Society of America in January.

SOLAR SINTERSCase study: markus kayser, 2011

The Solar Sinter - The Potential of Desert ManufacturingIn a world increasingly concerned with questions of energy pro-duction and raw material shortages, the Solar Sinter project explores the potential of desert manufacturing, where energy and material occur in abundance. In this experiment sunlight and sand are used as raw energy and material to produce glass objects using a 3D printing process, that combines natural energy and material with high-tech production technology. Solar-sintering aims to raise questions about the future of manufactur-ing and trigger dreams of the full utilisation of the production potential of the world’s most efficient energy resource - the sun. Whilst not providing definitive answers this experiment aims to provide a point of departure for fresh thinking.

This was a solar-powered, semi-automated low-tech laser cutter, that used the power of the sun to drive it and directly harnessed its rays through a glass ball lens to ‘laser’ cut 2D components using a cam-guided system. The Sun-Cutter produced compo-nents in thin plywood with an aesthetic quality that was a curious hybrid of machine-made and “nature craft” due to the crudeness of its mechanism and cutting beam optics, alongside variations in solar intensity due to weather fluctuations.

SUN+SAND: Silicia sand when heated to melting point and allowed to cool solidifies as glass. This process of converting a powdery substance via a heating process into a solid form is known as sintering and has in recent years become a central process in design prototyping known as 3D printing. By using the sun’s rays instead of a laser and sand instead of resins, The basis of an entirely new solar-powered machine and production pro-cess for making glass objects that taps into the abundant sup-plies of sun and sand to be found in the deserts of the world.

<SAND + SOLAR = SOLAR SINTER>

Image credit: Markus Kayser

Self-supporting structural unit having a series of repititious geometrical modules. (Patented, Ron Resch ,1968)

SI, SILICON + + = ???FE, IRON SUN

MG, MAGNESIUM LIGHTING

CA, CALCIUM WIND

0, OXYGEN RADIATION

CA, CALCIUM WATER

S, SULFUR BACTERIA

AL, ALUMINUM .NA, SODIUM .K, POTASSIUM CL, CHLORINE

AGENDAHarnessing dust storms and suspended sand particles to create local building material, while clearing up the atmosphere to improve visibility and habitability of Mars. To explore new methods of production for sustainable , self-deployed construc-tion. To discuss the immanence and potentials of dust - by convention defined to be kept out and away - into a handy, accessible resource, working in line with natural phenomenons and not against it. In the process of which, translating immaterial moments to spatial ecstasies in the unyieldingly harsh landscape of Mars.

This investigation seeks take on a multidisciplinary character in the search of emerging realities and parallels, in a trans-planetary fashion.

Site: Current choice of location includes the Nili Patera dune field in the Syrtis Major. Ideal location will in in the equatorial tropics where there will be maximum insolation even during dust storms (20-40 cal/cm2).

Sand storms are inextricably tied to the micro climate and temperatures on Mar. While it could be that sand storm occurs because of a rise in temperature (variance), it could also be that the sand in the atmosphere itself becomes an insulating.

LOCATION

My project presents a support infrastructure for production of built material, which doubles up asOption 1: Materials/ Geological research facilityOption 2: Launching/landing base.

The structure I propose in my project is modular to allow for growth of the base according to the arising needs. Similar modules can arrive depending on functional demands. Flexibility of the base modules themselves allows them to be assembled in various ways to attain different structures.

The foundation of the base does not require terrain leveling, instead the base columns are strengthen over time as sand and dust composite deposits on it, until it reaches a certain stiffness and stability for human inhabitation.

ModularityThe proposed solution is characterized by a high level of unification of elements, to the furthest possible extent. It allows exchange of functions between the individual domes in case one of them is damaged. Each module also serves as pressurised volumes in which various functions can take place in each of the four wings, with a central atrium where one access the vertical circulation tunnel.

Pneumatic architecture.While adapting the technologies of portable architecture to the construction potential of space architecture three concepts were deemed most suitable: metal, mixed and pneu-matic structures. Pneumatic architecture allows structure to be taken down easily and reconstructued at another location. The skin can also be prefabricated to suit the adher-ance property of sand and dust particles in Mars that determines the movement or saltation of sand. S

PROGRAMME

Intermediate stage between I &II will be the focus of the project, where few small and tight research base are set up in anticipation of more teams working on Mars. More dwelling structure have to be built to increase habitable space in a short span of time, and limited resource from Earth. An infrastructural set up for the production of local built materials will have to be set up. Large structure need not always require specific ground preparation, a combination of portable instal-lations, robotics assembly and working with natural elements can yield quick results.

Base development stages. Stage I: Manned missions to Mars can be launched every 3 years. Slowly more and more small modules will appear on Mars and a settlement of such metal cylinders, linked with airlocks will appear, enlarging the usage surface of the growing Martian base. Various scientific equipment and robots can be sent, including ones enabling production based on local resources.

Stage II: These resources will allow construction of habitats for several dozen or more people. Also deployable habitats can be brought from Earth. A transport module 8 m in diameter and height, instead of a return vehicle can contain struc-tures packed in a way portable architecture is packed on Earth. Thus, without using local resources or more complex methods large habitable space can be gained. This is the issue I am trying to solve in this paper.

Stage III: In the future large human settlements may appear on the surface of the Red Planet. They will be covered by great domes or placed underground. Terra-forming and change of the atmosphere into one suitable for breathing will last for 100 years.

WHEN

WHY

living unit

accumulated sand adds to performace of structure

sand as insulation

DESIGN PROPOSAL CONCEPT EXPLORATION







Dolly Foo



<Material study>



C





SALTATION OF SAND























CA, CALCIUM WIND

0, OXYGEN RADIATION

CA, CALCIUM WATER

S, SULFUR BACTERIA






LOCATION






PROGRAMME





WHEN

WHY

living unit


sand as insulation








Dolly Foo



<Material study>



C





SALTATION OF SAND























CA, CALCIUM WIND

0, OXYGEN RADIATION

CA, CALCIUM WATER

S, SULFUR BACTERIA






LOCATION






PROGRAMME





WHEN

WHY

living unit


sand as insulation



Dolly Foo

AGENDAHarnessing dust storms and suspended sand particles to create local building material, while clearing up the atmosphere to improve visibility and habitability of Mars. To explore new methods of production for sustainable , self-deployed construction. To discuss the immanence and potentials of dust - by convention defined to be kept out and away - into a handy, accessible resource, working in line with natural phenom-enons and not against it. In the process of which, translating immaterial moments to spatial ecstasies in the unyieldingly harsh landscape of Mars.


Harnessing dust storms and suspended sand particles to create local building material, while clearing up the atmosphere to improve visibility and habitability of Mars. To explore new methods of production for sustainable , self-deployed construction. To discuss the immanence and potentials of dust - by convention defined to be kept out and away - into a handy, accessible resource, working in line with natural phenom-enons and not against it. In the process of which, translating immaterial moments to spatial ecstasies in the unyieldingly harsh landscape of Mars. New technology could also be applied back on Earth to counter the destructive forces of sandstorms and desertification.


Mars dust storms are of great interest to scientists. Even though several spacecraft have observed the storms first hand, scientists are no closer to a definitive answer. For now, the storms on Mars are going to continue to present challenges to planning a human mission to the planet.

All dust storms on Mars, no matter what size, are powered by sunshine. Solar heating warms the martian atmos-phere and causes the air to move, lifting dust off the ground.Because the martian atmosphere is thin--about 1% as dense as Earth's at sea level--only the smallest dust grains hang in the air. Airborne dust on Mars is about as fine as cigarette smoke.



Option 1: Materials production and storage infrastructure and research base.Option 2: Landing/lauchning pad and materials facility.





Site: Current choice of location includes the Nili Patera dune field in the Syrtis Major. Ideal loca-tion will in in the equatorial tropics where there will be maximum insolation even during dust storms (20-40 cal/cm2). and parallels, in a trans-planetary fashion.

Sand storms are inextricably tied to the micro climate and temperatures on Mar. While it could be that sand storm occurs because of a rise in temperature (variance), it could also be that the sand in the atmosphere itself becomes an insulating (or heating?) agent itself? To be researched on in detail.

LOCATION

PROGRAMME

WHEN

DESIGN

living unit


sand as insulation



Dolly Foo

AGENDAHarnessing dust storms and suspended sand particles to create local building material, while clearing up the atmosphere to improve visibility and habitability of Mars. To explore new methods of production for sustainable , self-deployed construction. To discuss the immanence and potentials of dust - by convention defined to be kept out and away - into a handy, accessible resource, working in line with natural phenom-enons and not against it. In the process of which, translating immaterial moments to spatial ecstasies in the unyieldingly harsh landscape of Mars.


Harnessing dust storms and suspended sand particles to create local building material, while clearing up the atmosphere to improve visibility and habitability of Mars. To explore new methods of production for sustainable , self-deployed construction. To discuss the immanence and potentials of dust - by convention defined to be kept out and away - into a handy, accessible resource, working in line with natural phenom-enons and not against it. In the process of which, translating immaterial moments to spatial ecstasies in the unyieldingly harsh landscape of Mars. New technology could also be applied back on Earth to counter the destructive forces of sandstorms and desertification.






Option 1: Materials production and storage infrastructure and research base.Option 2: Landing/lauchning pad and materials facility.





Site: Current choice of location includes the Nili Patera dune field in the Syrtis Major. Ideal loca-tion will in in the equatorial tropics where there will be maximum insolation even during dust storms (20-40 cal/cm2). and parallels, in a trans-planetary fashion.

Sand storms are inextricably tied to the micro climate and temperatures on Mar. While it could be that sand storm occurs because of a rise in temperature (variance), it could also be that the sand in the atmosphere itself becomes an insulating (or heating?) agent itself? To be researched on in detail.

LOCATION

PROGRAMME

WHEN

DESIGN

living unit


sand as insulation








Dolly Foo



<Material study>



C





SALTATION OF SAND























CA, CALCIUM WIND

0, OXYGEN RADIATION

CA, CALCIUM WATER

S, SULFUR BACTERIA






LOCATION






PROGRAMME





WHEN

WHY

living unit


sand as insulation


A B

reco

nstit

utin

g sa

nd -

self-

cons

truct

ing

airb

orn(

e) ty

polo

gy

<wha

t>Har

ness

ing

dust

stor

ms t

o cr

eate

new

bui

ldin

g m

ater

ial,

while

clea

ring

up th

e at

mos

pher

e to

impr

ove

visib

ility

and

habi

tabi

lity o

f Mar

s. To

exp

lore

new

met

hods

of p

rodu

c-

tion

for s

usta

inab

le , s

elf-d

eplo

yed

cons

truct

ion.

To

expl

ore

the

act o

f filte

ring

- the

filte

r as a

shie

ld, a

nd al

so as

a . T

o di

scus

s the

imm

anen

ce an

d po

tent

ials

of d

ust -

by

conv

entio

n de

fined

to b

e ke

pt o

ut an

d aw

ay -

into

a ha

ndy,

acce

ssib

le re

sour

ce, w

orki

ng in

line

with

nat

ural

phe

nom

enon

s and

not

agai

nst i

t. In

the

proc

ess o

f whi

ch, t

rans

-

latin

g im

mat

eria

l mom

ents

to sp

atia

l ecs

tasie

s in

the

unyie

ldin

gly h

arsh

land

scap

e of

mar

s.

This

inve

stig

atio

n se

eks t

ake

on a

mul

tidisc

iplin

ary c

hara

cter

in th

e se

arch

of e

mer

ging

real

ities

and

para

llels

, in a

trans

-pla

neta

ry fa

shio

n.

<why

> M

ars d

ust s

torm

s are

of g

reat

inte

rest

to sc

ient

ists.

Even

thou

gh se

vera

l spa

cecr

aft h

ave

obse

rved

the

stor

ms fi

rst h

and,

scie

ntist

s are

no

clos

er to

a de

finiti

ve an

swer

. For

now, t

he st

orm

s on

Mar

s are

goi

ng to

cont

inue

to p

rese

nt ch

alle

nges

to p

lann

ing

a hum

an m

issio

n to

the

plan

et.

All d

ust s

torm

s on

Mar

s, no

mat

ter w

hat s

ize, a

re p

ower

ed b

y sun

shin

e. S

olar

hea

ting

warm

s the

mar

tian

atm

osph

ere

and

caus

es th

e ai

r to

mov

e, li

fting

dus

t off

the

grou

nd.

Becau

se th

e m

artia

n at

mos

pher

e is

thin

--ab

out 1

% as

den

se as

Ear

th's

at se

a lev

el--

only

the

smal

lest

dus

t gra

ins h

ang

in th

e ai

r. Ai

rbor

ne d

ust o

n M

ars i

s abo

ut as

fine

as

cigar

ette

smok

e.

Dust s

torm

s ofte

n be

gin

in H

ella

s Bas

in, t

he b

igge

st h

ole

in th

e gr

ound

in th

e en

tire

sola

r sys

tem

( 6 k

m d

eep

and

2000

km

acro

ss),

Ove

r the

year

s sin

ce it

has

accu

mul

ated

plen

ty o

f dus

t, an

d be

caus

e th

e ba

sin is

so d

eep,

air a

t the

bot

tom

is ab

out 1

0 deg

rees

or s

o war

mer

than

air a

t the

top.

Thi

s gra

dien

t driv

es w

inds

, whi

ch ca

n ca

rry d

ust a

ll

the

way o

ut o

f the

crat

er, a

nd e

nvel

ops u

p to

a qu

arte

r of t

he M

artia

n su

rface

.

It was

also

repo

rted

that

an e

norm

ous d

ust s

torm

that

exp

lode

d on

Mar

s in

2001

, whi

ch sh

roud

ed th

e pl

anet

in h

aze

and

raise

d th

e te

mpe

ratu

re o

f its

upp

er at

mos

pher

e 30

deg.

C.(a

rticl

e-Pl

anet

Gob

blin

g Dus

t Sto

rms (

Scie

nce@

NASA)

)

Wha

t doe

s thi

s im

ply?

San

d st

orm

s are

inex

trica

bly t

ied

to th

e m

icro

clim

ate

and

tem

pera

ture

s on

Mar

. Whi

le it

coul

d be

that

sand

stor

m o

ccur

s bec

ause

of a

rise

in

tem

pera

ture

(var

ianc

e), it

coul

d al

so b

e th

at th

e sa

nd in

the

atm

osph

ere

itsel

f bec

omes

an in

sula

ting

(or h

eatin

g?) a

gent

itse

lf? T

o be

rese

arch

ed o

n in

det

ail.

New te

chno

logy

coul

d al

so b

e ap

plie

d ba

ck o

n Ea

rth to

coun

ter t

he d

estru

ctive

forc

es o

f san

dsto

rms a

nd d

eser

tifica

tion.

<what exactly to build?>

To build machine

<where exactly to build?>

Current choice of location includes the Nili Patera dune field in the Syrtis Major. Ideal

location will in in the equatorial tropics where there will be maximum insolation even

during dust storms (20-40 cal/cm2).

<what to build with?>

The atmosphere of Mars is a resource of known composition available at any landing site on

Mars. It has been proposed that human exploration of Mars could use carbon dioxide (CO2)

from Martian atmosphere to make rocket fuel for the return mission.Two major chemical

pathways for use of the carbon dioxide are the Sabatier reaction, converting atmospheric

carbon dioxide along with additional hydrogen (H2), to produce methane (CH4) and oxygen

(O2), and electrolysis, using a zirconia solid oxide electrolyte to split the carbon dioxide into

oxygen (O2) and carbon monoxide (CO).

<how to start >

<Material study>

Sand, dust and powder

What is the composite of Marsian sand, what are the properties, how different it is from

sand on earth. Also study the extend and periods of sandstorm and how it affects NASA’s

explorations. Identify similar conditions on Earth for case study.

Study sand and its structural properties in existing constructional technology.

Read: Sand: The Never-Ending Story, Michæl Welland

<Topological study>

Features on Mars – sand dunes, volcanoes, tunnels, Hellas Planita, equatorial belt, wind

patterns, heating patterns

<Technological study>

SOLAR SINTERS

Case study: markus kayser, 2011

This was a solar-powered, semi-automated low-tech laser cutter, that used the power of

the sun to drive it and directly harnessed its rays through a glass ball lens to ‘laser’ cut 2D

components using a cam-guided system. The Sun-Cutter produced components in thin

plywood with an aesthetic quality that was a curious hybrid of machine-made and “nature

craft” due to the crudeness of its mechanism and cutting beam optics, alongside variations

in solar intensity due to weather fluctuations.

SUN+SAND: Silicia sand when heated to melting point and allowed to cool solidifies as

glass. This process of converting a powdery substance via a heating process into a solid

form is known as sintering and has in recent years become a central process in design

prototyping known as 3D printing. By using the sun’s rays instead of a laser and sand

instead of resins, The basis of an entirely new solar-powered machine and production

process for making glass objects that taps into the abundant supplies of sun and sand to be

found in the deserts of the world.

C

This is a perspective view of the Nili Patera dune �eld. A HiRISE image has been

draped over a digital elevation model of Mars. Colors correspond to the amplitude

of the ripple's displacement extracted by image correlation between two HiRISE

observations separated by 105 days. Cool colors (blue) correspond to less than 75

cm of displacement whereas warm colors (red) correspond to 4.5+ meters.

[Credit: California Institute of Technology]

3d printing with sand

Case study: ETH Digital Fabrications and Robotic Systems

http://www.dfab.arch.ethz.ch/web/e/forschung/index.html

Flight Assembled Architecture, 2011-2012, FRAC Centre Orléans

Flight Assembled Architecture is the first architectural installation assembled

by flying robots, free from the touch of human hands. The installation is an

expression of a rigorous architectural design by Gramazio & Kohler and a

visionary robotic system by Raffaello D’Andrea. Flight Assembled Architecture

consists of over 1.500 modules which are placed by a multitude of quadrotor

helicopters, collaborating according to mathematical algorithms that translate

digital design data to the behavior of the flying machines. In this way, the flying

vehicles, together, extend themselves as “living” architectural machines and

complete the composition from their dynamic formation of movement and

building performance. Within the build, an architectural vision of a 600m high

“vertical village” for 30’000 inhabitants unfolds as model in 1:100 scale. This

newly founded village is located in the rural area of Meuse, taking advantage of

an existing TGV connection that brings its inhabitants to Paris in less than one

hour. It is from this quest of an “ideal” self-sustaining habitat that the authors

pursue a radical new way of thinking and materializing verticality in architec-

ture, Flight Assembled Architecture.

<what exactly to build?>To build machine

<where exactly to build?>Current choice of location includes the Nili Patera dune field in the Syrtis Major. Ideal


during dust storms (20-40 cal/cm2). <what to build with?>The atmosphere of Mars is a resource of known composition available at any landing site on






oxygen (O2) and carbon monoxide (CO).<how to start ><Material study>Sand, dust and powderWhat is the composite of Marsian sand, what are the properties, how different it is from


explorations. Identify similar conditions on Earth for case study. Study sand and its structural properties in existing constructional technology.

Read: Sand: The Never-Ending Story, Michæl Welland<Topological study>Features on Mars – sand dunes, volcanoes, tunnels, Hellas Planita, equatorial belt, wind

patterns, heating patterns<Technological study>SOLAR SINTERSCase study: markus kayser, 2011This was a solar-powered, semi-automated low-tech laser cutter, that used the power of





in solar intensity due to weather fluctuations.SUN+SAND: Silicia sand when heated to melting point and allowed to cool solidifies as







C





cm of displacement whereas warm colors (red) correspond to 4.5+ meters.[Credit: California Institute of Technology]

3d printing with sandCase study: ETH Digital Fabrications and Robotic Systemshttp://www.dfab.arch.ethz.ch/web/e/forschung/index.html Flight Assembled Architecture, 2011-2012, FRAC Centre Orléans

















<what exactly to build?>To build machine

<where exactly to build?>Current choice of location includes the Nili Patera dune field in the Syrtis Major. Ideal


during dust storms (20-40 cal/cm2). <what to build with?>The atmosphere of Mars is a resource of known composition available at any landing site on






oxygen (O2) and carbon monoxide (CO).<how to start ><Material study>Sand, dust and powderWhat is the composite of Marsian sand, what are the properties, how different it is from


explorations. Identify similar conditions on Earth for case study. Study sand and its structural properties in existing constructional technology.

Read: Sand: The Never-Ending Story, Michæl Welland<Topological study>Features on Mars – sand dunes, volcanoes, tunnels, Hellas Planita, equatorial belt, wind

patterns, heating patterns<Technological study>SOLAR SINTERSCase study: markus kayser, 2011This was a solar-powered, semi-automated low-tech laser cutter, that used the power of





in solar intensity due to weather fluctuations.SUN+SAND: Silicia sand when heated to melting point and allowed to cool solidifies as







C





cm of displacement whereas warm colors (red) correspond to 4.5+ meters.[Credit: California Institute of Technology]

3d printing with sandCase study: ETH Digital Fabrications and Robotic Systemshttp://www.dfab.arch.ethz.ch/web/e/forschung/index.html Flight Assembled Architecture, 2011-2012, FRAC Centre Orléans

















C SAND BAGSThe project – a kind of bio-architectural test-landscape – would thus "go from a balloon-like pneumatic structure filled with bacillus pasteurii, which would then be released into the sand and allowed to solidify the same into a permacultural architecture."

Different types of construction methods involving pile systems that could probably be used to get the bacteria down into the sand – a procedure that would be analogous to using an oversized 3D printer, solidifying parts of the dune as needed. The piles would be pushed through the dune surface and a first layer of bacteria spread out, solidifying an initial surface within the dune. They would then be pulled up, creating almost any conceivable (structurally sound) surface along their way, with the loose sand acting as a jig before being excavated to create the necessary voids. If we allow ourselves to dream, we could even fantasise about ways in which the wind could do a lot of this work for us: solidifying parts of the surface to force the grains of sand to align in certain patterns, certain shapes, having the wind blow out our voids, creating a structure that would change and change again over the course of a decade, a century, a millenium.

INFLATING WITH SAND

PNEUMATIC ARCHITECTURE


A particular microorganism, Bacillus Pasteurii, is flushed through the dunescape (an analogy could be made to an oversized 3d printer), which causes a biological reaction that turns the sand into solid sandstone. The initial reactions finish within 24 hours; it would take about a week to satu-rate the sand enough to make the structure habitable. The bacteria are non-patogenic and die in the process of solidifying the sand. This part of the project relies upon research carried out by professor Jason De Jong's team at the Soil Interactions Laboratory, UC Davis



CA, CALCIUM WIND

0, OXYGEN RADIATION

CA, CALCIUM WATER

S, SULFUR BACTERIA

AGENDA

SYSTEM

Harnessing dust storms and suspended sand particles to create local building material on Mars, through a combina-tion of low technology (wind movement) and advanced material science, to create a landscape of infrastructural entities. In a intermediate stage of human exploration on Mars, where few small research base have already been set up in anticipation of a larger human colony on Mars. More infrastructure will have to be built to increase habitable space, without adding to the ever increasing pay load. An infrastructural system for the production of local built materials will have to be set up. Large structure need not always require specific ground preparation, a combination of deployable installations, robotics assembly, working with natural elements can yield quick results. SAND + DEPOSITION = SHELTER + LANDSCAPE

The structures are deployed and are allowed to grow for an appropriate amount of time before it gains sufficient stiffness and insulating factor for human occupany. In this interim period of construct, the structure will serve as temporary storm shelters for rovers and other space explora-tion vehicles, and also as the begining attempts at introducing human landmarks and artifacts for our navigational instincts.

ORIGAMI ARCHITECTURE = MODULAR SYSTEM + DEPLOYABLE STRUCTURE + PNEUMATIC SKIN

The foundation of the base does not require terrain leveling, instead the base structure strengthen over time as sand and dust composite deposits on it, until it reaches a certain stiffness and stability for human inhabitation. The proposal is based on systematic growth by algo-rithm. The goal is to find a sequence that is allows for universal growth in various configurations for a fixed set of modules. Each module serves as unpressurised volumes in which various functions and plug-in vehicu-lar programs can take place .

While adapting the technologies of portable architec-ture to the construction potential of space architecture three concepts were deemed most suitable: metal, mixed and pneumatic structures. Pneumatic architec-ture allows structure to be taken down easily and reconstructued at another location. The skin can also be prefabricated to suit the adherance property of sand and dust particles in Mars that determines the move-ment or saltation of sand. S

DEPLOYMENT / DEPOSITION

SYSTEM

ENDEAVOUR CRATER & DUNESCAPEMORE THAN 10% OF THE SURFACE AREA ON MARS IS COVERED BY WINDBLOWN SAND DUNES. IN 2008 SAND DUNES WAS RE-PORTED TO BE ACTIVE ON MARS.

Studies shown that two 20m wide dome dune disappeared and a thrid shrank by 15%, though larger dunes did not show apparant change

ENDEAVOUR IS AN IMPACT CRATER LOCATED IN MERIDIANI PLANUM ON MARS. DIAMETER: 22KM, DEPTH: 300M

Ideal location will in in the equatorial tropics where there will be maximum insolation even during dust storms (20-40 cal/cm2).

Sand storms are inextricably tied to the micro climate and temperatures on Mar. While it could be that sand storm occurs because of a rise in temperature (variance), it could also be that the sand in the atmosphere itself becomes an insulating agent that triggers the

SITE & ENVIRONMENT

Mars Global Surveyor (MGS) images of sand dunes on Mars (courtesy of NASA/JPL/MSSS). L-R: a. Barchan dunes at Arkhangelsky crater, near 41.0◦S, 25.0◦ W; b. north polar dunes near 77.6◦N, 103.6◦ W; bimodal sand dunes near c. 48.6◦S, 25.5◦ W; d. 49.6◦S, 352.9◦ W, and e. 76.4◦N, 272.9◦W.

WIND TUNNEL TESTS

M SERIES SHELTERDEPLOYABLE RAPID ASSEMBLY SHELTERS (MARTIAN)FOO YU YU DOLLY

ABOUTSingle exterior cover DRASH Series Shelters provide emergency response personnel with a variety of rapidly-deployable, rugged, lightweight, man-portable and user-friendly soft-walled shelters.

Deployed or taken down by only 2 - 4 personnel within a matter of minutes without the need for special tools or dealing with loose parts, the shelter design is based on the the folding patterns of origami science. DRASH is a free-standing, self-supporting structure that requires no power or air to erect. Additionally, there are no obstructions such as center poles or locking devices needed to keep the shelter erect. The frame of the Shelter is manufactured from reinforced Mylar® and Titanite®, a rugged and durable aerospace material, with a flex strength 270% greater than that of aluminum, giving the DRASH Shelter the ability to withstand dust storms, solar radiation and the harsh Martian environment.

Kit of Parts(K.O.P): Each shelter comes with a retainer/housing case, repair kit, Velcro belt, wind lines and a steel pin stake set.

ITERATIONSShelter Model: Exterior Interior Weight Dimensions: Dimensions : (kg): AD2SEVA 12 x 10 x 14 6 x 10 x 8 40 AD3SEVA 12 x 15 x 14 6 x 15 x 8 50 AD4SEVA 12 x 20 x 10 6 x 20 x 8 56 AD5SEVA 12 x 25 x 10 6 x 25 x 8 50 AD6SEVA 12 x 30 x 10 6 x 30 x 8 65 AD2SEVB 12 x 8 x 10 6 x 8 x 8 40 AD3SEVB 12 x 12 x 10 6 x 12 x 8 40 AD4SEVB 12 x 15 x 10 6 x 16 x 8 50 AD5SEVB 12 x 20 x 12 6 x 20 x 8 60 AD6SEVB 12 x 20 x 14 6 x 24 x 8 65

(W x L x H)

THE SITUATION...

Sequence of structural components of SEV

Superior (70°)

Superior Temporal (62°)

Temporal (85°)

Inferior Temporal (85°)

Inferior (70°)

Field of view Dimensions

81.3 cm

Max 66 cm

53 cm

58.4 cm

18 Average 191.9 cm

Max 84.8 cm

Working range

45.72 cm

66.04 cm diagonally

40.64 cm diagonally

15°

33.02 cm

12.7Optimum one-handed work envelope.

Optimum two-handed work envelope

137.16 cm

140.97 cm

Mobility range measured in: Torque (Nm) and Angle of motion (degrees)

Shoulder movement(lateral-medial)

1.3 Nm 20°

1.3 Nm150°

4.5 Nm180°Shoulder flexion/extension

1.3 Nm 150°

Shoulder adduction/abduction

Waist mobility side to side rotation

12.4 Nm150°

Elbow flexion/extension

1.3 Nm130°

Forearm mobility and wrist rotation

0.68 Nm180°

1.3 Nm40°

1.3 Nm40°

A B

Ankle extension (A)and flexion (B)

2.7 Nm 10°Hip abduction(leg straight)

Hip and waist flexion/extension

5.4 Nm90°

1.3 Nm 150°

Knee flexion: kneeling

1.3 Nm 120°

Knee mobility:flexion standing

2.7 Nm 70°

Hip flexion

The Astronaut Scale

!!!

AM

BA

M

BAAMM

uh-oh.

HOUSTON,WE’VE GOT A PROBLEM...

S.O.P1. Phone Mission Control

2. Check IMV meter 3. Await instructions

SUIT UP

GUYS!!

and get

DRASHout of the

bag.We’re sending

Beetle 2 over to take a look.

IT’S LITERALLY A

MICRO-METEORITE!

WE SURE GOT LUCKY...

HOUSTON, WE’RE LOSING

PRESSURE IN HERE!

Darn those dust

devils!

Okay, you two set up the shelter, I’ll be

inspecting the damage.

WHAT IS

?

THE VEHICLE (SEV)

FUNCTIONAL REQUIREMENTS• PASSENGER CAPACITY: Crew of 2, up to 4 in emergencies• MOBILITY: Up to 10km/ hour, mobility chassis wheel able to pivot 360º, allowing it to drive in any direction

SPECIFICATIONS:Weight: 3,000 kg Payload: 997 kgLength: 4.48 m Wheelbase: 3.9 mHeight: 3.048 m feet Wheels: 4.7x 1 m in diameter, 0.3 m wide

On planetary surfaces, astronauts will need surface mobility to ex-plore multiple sites across the lunar and Martian surfaces. The SEV surface concept has the small, pressurized cabin mounted on a wheeled chassis that would enable a mobile form of exploration. These two components could be delivered to the planetary surface together, or as separate elements. The SEV can provide the astro-nauts’ main mode of transportation, and – unlike the unpressurized Apollo lunar rover – also allow them to go on long excursions with-out the restrictions imposed by spacesuits. The pressurized cabin has a suitport that allows the crew to get into their spacesuits and out of the vehicle faster than before, enabling multiple, short spacewalks as an alternative to one long spacewalk.

The Space Exploration Vehicle Characteristics (Surface Concept)

ounded by 2.5 cm

y

Ice-shielded Lock / Fusible Heat Sink: Lock surrof frozen water provides radiation protection. Same ice is used as a fusible heat sink, rejecting heat energby melting ice instead of evaporating water to vacuum.

1

3

47

96

5 8

2

6

5

8

9

Docking Hatch: Allows crew members to move fr om the rover to a habitat, an ascent module or another rover.

Suit PortableLife SupportSystemReduces mass, cost, volume and complexity.

Suitports: Allow suit donning and vehicle egress in less than 10 minutes with minimal gas loss.

Pressurized Rover: Low-mass, low-volume design makes it possible to have two vehicles on a planetary lunar surface, greatly extending the range of safe exploration.

Chariot Style Aft Driving Station: Enables crew to drive rover while conduct-ing moonwalks.

Pivoting Wheels:

Enables crab-style driving for docking and maneuvering on steep terrain.

Work Package Interface: Allows attachment of modular work packages (e.g. winch, cable, backhoe or crane).

Modular Design: Pressurized Rover and chassis may be deliveron separate landers or pre-integrated on one lander.

SEVTYPE A

DIM: (WxLxH)4 x 8 x 3m

capacity:4 person, in emergency;6 person

SEVTYPE A

DIM: (WxLxH)4 x 4.5 x 3m


THE SITUATION...

Sequence of structural components of SEV

Superior (70°)

Superior Temporal (62°)

Temporal (85°)

Inferior Temporal (85°)

Inferior (70°)

Field of view Dimensions

81.3 cm

Max 66 cm

53 cm

58.4 cm

18 Average 191.9 cm

Max 84.8 cm

Working range

45.72 cm

66.04 cm diagonally

40.64 cm diagonally

15°

33.02 cm

12.7Optimum one-handed work envelope.

Optimum two-handed work envelope

137.16 cm

140.97 cm

Mobility range measured in: Torque (Nm) and Angle of motion (degrees)

Shoulder movement(lateral-medial)

1.3 Nm 20°

1.3 Nm150°

4.5 Nm180°Shoulder flexion/extension

1.3 Nm 150°

Shoulder adduction/abduction

Waist mobility side to side rotation

12.4 Nm150°

Elbow flexion/extension

1.3 Nm130°

Forearm mobility and wrist rotation

0.68 Nm180°

1.3 Nm40°

1.3 Nm40°

A B

Ankle extension (A)and flexion (B)

2.7 Nm 10°Hip abduction(leg straight)

Hip and waist flexion/extension

5.4 Nm90°

1.3 Nm 150°

Knee flexion: kneeling

1.3 Nm 120°

Knee mobility:flexion standing

2.7 Nm 70°

Hip flexion

The Astronaut Scale

!!!

AM

BA

M

BAAMM

uh-oh.

HOUSTON,WE’VE GOT A PROBLEM...

S.O.P1. Phone Mission Control

2. Check IMV meter 3. Await instructions

SUIT UP

GUYS!!

and get

DRASHout of the

bag.We’re sending

Beetle 2 over to take a look.

IT’S LITERALLY A

MICRO-METEORITE!

WE SURE GOT LUCKY...

HOUSTON, WE’RE LOSING

PRESSURE IN HERE!

Darn those dust

devils!

Okay, you two set up the shelter, I’ll be

inspecting the damage.

WHAT IS

?

THE VEHICLE (SEV)

FUNCTIONAL REQUIREMENTS• PASSENGER CAPACITY: Crew of 2, up to 4 in emergencies• MOBILITY: Up to 10km/ hour, mobility chassis wheel able to pivot 360º, allowing it to drive in any direction

SPECIFICATIONS:Weight: 3,000 kg Payload: 997 kgLength: 4.48 m Wheelbase: 3.9 mHeight: 3.048 m feet Wheels: 4.7x 1 m in diameter, 0.3 m wide

On planetary surfaces, astronauts will need surface mobility to ex-plore multiple sites across the lunar and Martian surfaces. The SEV surface concept has the small, pressurized cabin mounted on a wheeled chassis that would enable a mobile form of exploration. These two components could be delivered to the planetary surface together, or as separate elements. The SEV can provide the astro-nauts’ main mode of transportation, and – unlike the unpressurized Apollo lunar rover – also allow them to go on long excursions with-out the restrictions imposed by spacesuits. The pressurized cabin has a suitport that allows the crew to get into their spacesuits and out of the vehicle faster than before, enabling multiple, short spacewalks as an alternative to one long spacewalk.

The Space Exploration Vehicle Characteristics (Surface Concept)

ounded by 2.5 cm

y

Ice-shielded Lock / Fusible Heat Sink: Lock surrof frozen water provides radiation protection. Same ice is used as a fusible heat sink, rejecting heat energby melting ice instead of evaporating water to vacuum.

1

3

47

96

5 8

2

6

5

8

9

Docking Hatch: Allows crew members to move fr om the rover to a habitat, an ascent module or another rover.

Suit PortableLife SupportSystemReduces mass, cost, volume and complexity.

Suitports: Allow suit donning and vehicle egress in less than 10 minutes with minimal gas loss.

Pressurized Rover: Low-mass, low-volume design makes it possible to have two vehicles on a planetary lunar surface, greatly extending the range of safe exploration.

Chariot Style Aft Driving Station: Enables crew to drive rover while conduct-ing moonwalks.

Pivoting Wheels:

Enables crab-style driving for docking and maneuvering on steep terrain.

Work Package Interface: Allows attachment of modular work packages (e.g. winch, cable, backhoe or crane).

Modular Design: Pressurized Rover and chassis may be deliveron separate landers or pre-integrated on one lander.

SEVTYPE A

DIM: (WxLxH)4 x 8 x 3m


SEVTYPE A

DIM: (WxLxH)4 x 4.5 x 3m


HOW TO USE YOUR DRASH SHELTER

FOLDING PATTERN

BASE GRID (1m x 1m): 20 x 14

PACKINGDEPLOYMENT PROCESS: SET-UP

PLAN 1:100 FLOOR PLAN 1:100

FUNCTIONAL PLAN

ROOF PLAN 1:100

<core>life-support

20%

<ancillary>adaptive functions

75%

4500 500 500 500 500

2000

800

thickness

curtain track and storage for airbag sub-assembly

wheels positioned at maximum width

A

B

PACKING

DEPLOYMENT PROCESSFUNCTIONAL PLAN

<core>life-support

20%

<ancillary>adaptive functions

75%

4500 500 500 500 500

2000

800

thickness

FOLDING PATTERN

BASE GRID (1m x 1m): 20 x 14 PLAN 1:100 FLOOR PLAN 1:100 ROOF PLAN 1:100

AIR LOCK / ACCESSAirlocks are required at entrances to prevent loss of internal air-pressure. Eg. revolving door, airlock portals, zippers, Velcro. When using a double wall construction; one doesn't need a proper door.

MEMBRANE/ MATERIALITYThe skin of pneumatic system determines much spatial quality of the construct. In responding to environmental demands, and by integrating material technologies, one can look for qualities like scales in translucency or elasticity. Materials can be highfrequency sealed, glued or just stitched. Other qualities are; non static, lightweight, strong, resistant to tearing, self-repairing. Considerations are made to use microfibers, non-wovens, woven vecram (used in the space industry), metallic foils, plastic films.

MYLAR

ANCHORING> Ballast > Earth/Water Ballast Anchorage Syste > Sandbags> Ground Anchorage System > Surface Ground Anchors > Underground Anchors1_Architects of air’s anchorage by pins 800mm x 25mm diameter. 2_Ballast anchorage usually takes the form of sandbags or concrete blocks in units of 125k, to come to a total weight from 5 - 12 tons

INFLATABLES IN SPACERadar RelfectiveSpheres [5]These radar calibration reflector spheres have been manufactured since the very earliest days of Raven Indus-tries and Aerostar International still manufactures them today.

Mars Pathfinder [8]The Mars Pathfinder airbag system was designed to protect the lander regardless of its orientation upon impact with the surface of the planet. The system also was designed to handle lateral movement as well as vertical descent. The huge, multi-lobed air bags, which will envelope and protect the Mars Pathfinder spacecraft before it impacts the surface of Mars. The air bags are composed of four large bags with six smaller, interconnected spheres within each bag. The bags measure 5 m tall and about 5 m in diameter. As Pathfinder is descending to the Martian surface on a parachute, an onboard altimeter inside the lander will monitor its distance from the ground. The computer will inflate these large air bags about 100 meters above the surface of Mars.

Inflatable Antenna [7]Credit: STS-77 Crew, Space Shuttle Endeavor, NASA, 1996The Inflatable Antenna Experiment was as part of a Spartan satellite. The antenna is roughly the size of a tennis court and is even visible from Earth. The function of an antenna is to broadcast radio messages, and the large dish at the end helps focus radio waves into a narrow beam which can be detected over long distances.

TransHab/ Space Hotel [6]Bigelow Aerospace’s inflatable Space Station continues the work on expandable space habitation of the TransHab Successfully verifying Bigelow Aerospace’s proprietary folding and packing techniques.

STRUCTURAL BEHAVIOUR [10]Cables and nets divide the membrane into a number of small elements, with small radii of curvature (when pres-surised, thus reducing membrane stresses. A major portion of the stresses is transferred to the netting when the membrane presses against the net under the influence of the internal pressure. Large spans can be achieved with thin transparent membranes.

`

FOLDING/PACKING [11]

Air Bag TechnologyIn asembling the airbag/cover, the airbag is initially prefolded to a predetermined configuration outside the cover. The prefolded air bag is then inserted as a unit into the cavity defined within the cover.

Origami

HEMPLANET INFLATED RIB STRUCTURE A framework of pressurised tubes which supports a weatherproof membrane in tension.[Thermosplastic polyurethane TPU bladder to keep the air inside and a polyester-laminated fabric outer jacker for protection and stability].

Pressurised Construction

Pneumatic Constr.

Air Controlled

Air Stabilised

Air Inflated

Air Supported

Hybrid Struc-

Dual Walled

Rib Structures

Total Pneumatic Hybrid

Partial Pneumatic Hybrid

OTHER STRUCTURAL FORMS

INFLATED SPACES - Spaces measuring the physical body as a co-structure in its inflated surrounding

1 2

43

5 6 8

7

Reinf. cable w/thimble & swaged sleeve end

anchor shackle

bent strap or rod in concrete

membrane

membrane liner

steel angle

removable expansion anchor (for temporaryinstallation)h9 Typical anchor

detail

DESIGN CONSIDERATIONS FOR INFLATED / PRESSURISED SPACES

10

11

Studio AAD, 2012NASA, Mars Habitat

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Transcript of Studio AAD, 2012NASA, Mars Habitat