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0-APOLLO 15-launch_wide.jpgThe Launch of Apollo 15227 visiteThe "ORIGINAL" Apollo Time-Table (from Apollo 13)
APOLLO 13. March, 1970. Land in Fra Mauro formation of flat highlands, stay about 22 hours. Collect soil and rock from an old area relatively untouched by what many believed were ancient floods or volcanoes.
APOLLO 14. July, 1970. Land in Censorinus Crater area for a stay of about 22 hours. Investigate craters, possibly carved in Moon's surface by meteors.
APOLLO 15. November, 1970. Land in Littrow area of volcano-like projections, remain about 22 hours. Attempt a pinpoint landing on an exact, pre-selected target.
APOLLO 16. March, 1971. Descend to Crater Copernicus, remaining for about 70 hours. Extract from crater and high-rising column within formation rocks believed to be from far below the lunar surface.
APOLLO 17. Late in 1971. Land near rugged highland crater Tycho for stay of about 70 hours. Test first moon "rover" vehicle.
APOLLO 18. Early 1972. Land in Marius Hills, remain about 70 hours. Collect soil and rock samples from volcanic-like domes and valleys between.
APOLLO 19. Middle or late 1972. Land deep in Schroeter's Valley, with about 70 hours on the surface. Attempt a descent into a deep crater to determine cause of mysterious "red flashes" seen there by astronomers.
APOLLO 20. Late 1972 or early 1973. Land near the Hyginus Rill, a long, major canyon, for stay of about 70 hours. Investigate canyon for possible lunar core material.
This timeline had been altered slightly even before the Apollo 13 mission, when in January, 1970, Apollo 20 was cancelled in order to reserve the last production Saturn V for use in launching the planned Skylab orbiting laboratory a few years later. This change shifted the planned Apollo 18 and 19 lunar missions to 1974 to follow Skylab, but further budget-cutting in late 1970 also resulted in the cancellation of Apollo 18 and 19.
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0-Saturn and Friends.jpgSaturn and His Moons190 visiteThe dozens of moons orbiting Saturn vary drastically in shape, size, age and origin. Some of these moons have rocky surfaces, while others are porous, icy bodies. Many have craters, ridges and valleys and some show evidence of tectonic activity. Some appear to have formed billions of years ago, while others appear to be pieces of a bigger, fragmented body. The most interesting one is Titan, the biggest of them all. Larger than Earth's Moon, Titan even has its own thick atmosphere - the only natural satellite in the Solar System with such a luxury. During its 4-year mission in this immense region, the Cassini spacecraft will extensively photograph many of these moons and collect data that will increase our understanding of their composition.
To date, 34 moons have been officially named. In alphabetic order, they are: Albiorix, Atlas, Calypso, Dione , Enceladus, Epimetheus, Erriapo, Helene, Hyperion, Iapetus, Ijiraq, Janus, Kiviuq, Methone, Mimas, Mundilfari, Narvi, Paaliaq, Pallene, Pan, Pandora, Phoebe, Polydeuces, Prometheus, Rhea, Siarnaq, Skadi, Suttung, Tarvos, Telesto, Tethys, Thrym, Titan and Ymir.
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0-Venus.jpgVenus from Mariner 10170 visiteVenus Data and Statistics
Mass (kg) = 4.869e+24
Mass (Earth = 1) = 81476
Equatorial radius = 6.051,8 Km
Equatorial radius (Earth = 1) = 0,94886
Mean density (gm/cm^3) = 5,25
Mean distance from the Sun = 108.200.000 Km
Mean distance from the Sun (Earth = 1) = 0,7233
Rotational period (days) = 243,0187
Orbital period (days) = 224,701
Mean orbital velocity = 35,02 Km per second
Tilt of axis = 177,36
Orbital inclination = 3,394
Equatorial surface gravity (m/sec^2) = 8,87
Equatorial escape velocity = 10,36 Km per second
Magnitude (Vo) = - 4,4
Mean surface temperature = + 482C
Atmospheric pressure (bars) = 92
Atmospheric composition: Carbon dioxide 96%, Nitrogen 3% and trace amounts of: Sulfur dioxide, water vapor, carbon monoxide, argon, helium, neon, hydrogen chloride and hydrogen fluoride.
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00-MRO-front-view_br~0.jpgHere is the "Mars Reconnaisance Orbiter"104 visiteThis artist's concept of the Mars Reconnaissance Orbiter features the spacecraft's main bus facing down, toward the red planet. The large silver circular feature above the spacecraft bus is the high-gain antenna, the spacecraft's main means of communicating with both Earth and other spacecraft. The long, thin pole behind the bus is the SHARAD antenna. Seeking liquid or frozen water, SHARAD will probe the subsurface using radar waves at a 15-25 MHz frequency band, "seeing" in the first few hundreds of feet (up to 1 kilometer) of Mars' crust. The large instrument (covered in black thermal blanketing) in the center is the HiRISE camera. This powerful camera will provide the highest-resolution images from orbit to date.
The other easily visible instruments are: the Electra telecommunications package which is the gold-colored instrument directly left of the HiRISE camera. It will act as a communications relay and navigation aid for Mars spacecraft. To the right of the HiRISE camera is the Context Imager (CTX).
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00-PhoenixLiftoff.jpgThe beginning...76 visiteCaption NASA:"Can Mars sustain life? To help answer this question, last week NASA launched the Phoenix Mission to Mars. In May 2008, Phoenix is expected to land in an unexplored North Polar Region of Mars that is rich in water-ice. Although Phoenix cannot move, it can deploy its cameras, robotic arm, and a small chemistry laboratory to inspect, dig, and chemically analyze its landing area. One hope is that Phoenix will be able to discern telling clues to the history of ice and water on Mars. Phoenix is also poised to explore the boundary between ice and soil in hopes of finding clues of a habitable zone there that could support microbial life.
Phoenix has a planned lifetime of 3 months on the Martian surface".MareKromium
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00-SMART1.jpgSMART-1 and the Moon77 visiteSMART-1's science payload, with a total mass of some 15 Kg, features many innovative instruments and advanced technologies. These are:
- AMIE, a miniaturised HR camera for Lunar Surface imaging;
- SIR, a Near-Infrared Point-Spectrometer for Lunar mineralogy investigation;
- D-CIXS, a very compact X-ray Spectrometer with a new type of detector and micro-collimator which will provide fluorescence spectroscopy and imagery of the Moon's surface elemental composition;
- XSM, an X-ray monitor to support D-CIXS by providing measurements of solar X-ray emission for calibration:
- KaTE, an experiment aimed at demonstrating deep-space telemetry and telecommand communications in the X and Ka-bands;
- RSIS, a Radio-Science Experiment relying on KaTE. It monitors the electric propulsion by means of tracking techniques. In lunar orbit it will, with AMIE, also study the Moon's libration.
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00-The Moon.jpgThe Moon66 visiteMoon Facts and Data
Mass (kg) = 7.349e+22
Mass (Earth = 1) = 1.2298e-02
Equatorial radius = 1.737,4 Km
Equatorial radius (Earth = 1) = 2.7241e-01
Mean density (gm/cm^3) = 3.34
Mean distance from Earth = 384.400 Km
Rotational period (days) = 27,32166
Orbital period (days) = 27,32166
Average length of lunar day (days) = 29,53059
Mean orbital velocity (km/sec) = 1,03
Tilt of axis = 1,5424
Orbital inclination = 5,1454
Equatorial surface gravity (m/sec^2) = 1,62
Equatorial escape velocity (km/sec) = 2,38
Magnitude (Vo) = -12,74
Mean surface temperature (day) = 107C
Mean surface temperature (night) = -153C
Maximum surface temperature = 123C
Minimum surface temperature = -233C
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000-Clementine.gif000 - Clementine55 visiteDescription
Clementine was a joint project between the Ballistic Missile Defense Organization (BMDO, nee the Strategic Defense Initiative Organization, or SDIO) and NASA. The objective of the mission was to test sensors and spacecraft components under extended exposure to the space environment and to make scientific observations of the Moon and the near-Earth asteroid 1620 Geographos. The Geographos observations were not made due to a malfunction in the spacecraft. The lunar observations made included imaging at various wavelengths in the visible as well as in ultraviolet and infrared, laser ranging altimetry, gravimetry, and charged particle measurements. These observations were for the purposes of obtaining multi-spectral imaging the entire lunar surface, assessing the surface mineralogy of the Moon and obtaining altimetry from 60N to 60S latitude and gravity data for the near side. There were also plans to image and determine the size, shape, rotational characteristics, surface properties, and cratering statistics of Geographos. Clementine carried 7 distinct experiments on-board: a UV/Visible Camera, a Near Infrared Camera, a Long Wavelength Infrared Camera, a High Resolution Camera, two Star Tracker Cameras, a Laser Altimeter, and a Charged Particle Telescope. The S-band transmitter was used for communications, tracking, and the gravimetry experiment.
Spacecraft and Subsystems
The spacecraft was an octagonal prism 1.88 meters high and 1.14 m across with two solar panels protruding on opposite sides parallel to the axis of the prism. A high-gain fixed dish antenna was at one end of the prism, and the 489 N thruster at the other end. The sensor openings were all located together on one of the eight panels, 90 degrees from the solar panels, and protected in flight by a single sensor cover. The spacecraft propulsion system consisted of a nonpropellant hydrazine system for attitude control and a bipropellant nitrogen tetraoxide and monomethyl hydrazine system for the maneuvers in space. The bipropellant system had a total capability of about 1900 m/s with about 550 m/s required for lunar insertion and 540 m/s for lunar departure. Attitude control was achieved with 12 small attitude control jets, two star tracker cameras, and two inertial measurement units. The spacecraft was three-axis stabilized in lunar orbit via reaction wheels with a precision of 0.05 Deg. in control and 0.03 Deg. in knowledge. Power was provided by gimbaled, single axis, GaAs/Ge solar panels which charged a 15 amp-hour, 47-w hr/Kg Nihau (Ni-H) common pressure vessel battery. Spacecraft data processing was performed using a MIL-STD-1750A computer (1.7 million instructions per second) for savemode, attitude control, and housekeeping operations, a RISC 32-bit processor (18 million ips) for image processing and autonomous operations, and an image compression system provided by the French Space Agency CNES. A data handling unit sequenced the cameras, operated the image compression system, and directed the data flow. Data was stored in a 2 Gbit dynamic solid state data recorder.
Mission Profile
The mission had two phases. After two Earth flybys, lunar insertion was achieved approximately one month after launch. Lunar mapping took place over approximately two months, in two parts. The first part consisted of a five hour elliptical polar orbit with a periapsis of about 400 Km at 30 degrees south latitude and an apoapsis of 8300 Km. Each orbit consisted of an 80 minute lunar mapping phase near periapsis and 139 minutes of downlink at apoapsis. After one month of mapping the orbit was rotated to a periapsis at 30 degrees north latitude, where it remained for one more month. This allowed global imaging and altimetry coverage from 60 degrees south to 60 degrees north, over a total of 300 orbits. After a lunar/Earth transfer and two more Earth flybys, the spacecraft was to head for Geographos, arriving three months later for a flyby, with a nominal approach closer than 100 Km. Unfortunately, on May 7, 1994, after the first Earth transfer orbit, a malfunction aboard the craft caused one of the attitude control thrusters to fire for 11 minutes, using up its fuel supply and causing Clementine to spin at 80 rpm. Under these conditions, the asteroid flyby could not yield useful results, so the spacecraft was put into a geocentric orbit passing through the Van Allen radiation belts to test the various components on board. The mission ended in June 1994 when the power level onboard dropped to a point where the telemetry from the spacecraft was no longer intelligible.
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000-Kaguya.jpgThe Kaguya (SELENE) Probe64 visiteThe SELenological and ENgineering Explorer "KAGUYA"(SELENE), Japans 1st large Lunar Explorer, was launched by the H-IIA rocket on September 14, 2007 (JST). The mission, which is the largest Lunar Mission since the Apollo Program, is being keenly anticipated by many countries.
The major objectives of the Mission are to understand the Moons origin and evolution and to observe the Moon in various ways in order to utilize it in the future. The Lunar Missions that have been conducted so far have gathered a large amount of information on the Moon, but the mysteries of its origin and evolution have been left unsolved.
KAGUYA will investigate the entire Moon in order to obtain information on its elemental and mineralogical composition, geography, surface and sub-surface structure, the remnant of its magnetic field and its gravity field.
The results are expected to lead to a better overall understanding of the Moons evolution. At the same time, the observation equipment installed on the orbiting satellite will observe plasma, the electromagnetic field and high-energy particles. The data obtained in this way will be of great scientific importance for exploring the possibility of using the moon for human endeavors.MareKromium
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000-Mars.jpgMars: the Red Planet with "Blue Limbs"...252 visiteMars Data and Statistics
Mass (kg) = 6.421e+23
Mass (Earth = 1) = 1.0745e-01
Equatorial radius = 3.397,2 Km
Equatorial radius (Earth = 1) = 5.3264e-01
Mean density (gm/cm^3) = 3,94
Mean distance from the Sun = 227.940.000 Km
Mean distance from the Sun (Earth = 1) = 1,5237
Rotational period (hours) = 24,6229
Rotational period (days) = 1,025957
Orbital period (days) = 686,98
Mean orbital velocity = 24,13 Km per second
Tilt of axis = 25,19
Orbital inclination = 1,850
Equatorial surface gravity (m/sec^2) = 3,72
Equatorial escape velocity = 5,02 Km per second
Magnitude (Vo) = - 2.01
Minimum surface temperature = - 140C
Mean surface temperature = - 63C
Maximum surface temperature = + 35C
Atmospheric pressure (bars) = 0,007
Atmospheric composition: Carbon Dioxide (C02) 95,2%; Nitrogen 2,7%; Argon 1,6%; Oxygen 0,13%; Carbon Monoxide 0,07%; Water 0,03%; Neon 0,00025%; Krypton 0,00003%
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000-Phobos-Global_Map-ESA.jpgPhobos: Global Map (False Colors)55 visiteCaption ESA:"This mosaic image is composed by 53 pictures obtained by the Super Resolution Channel (or SRC, a part of the High Resolution Stereo Camera experiment) on board ESAs Mars Express.
The SRC images covered 70% of the moon's surface. The remaining area is filled with 16 images previously obtained by NASAs Viking mission.
The mean resolution is 12 mt/pixel". MareKromium
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0000b.jpgThe Dawn of "X-Mars": the Dam (edm - High-Def-3D; credits: Dr M. Faccin & Lunar Explorer Italia)238 visiteIn questo extra-detail mgnf (sempre realizzato dal Dr Faccin), la struttura a doppio arco del rilievo si pu cogliere in tutta la sua bellezza.
Si tratta di un double-crater ormai in rovina? Secondo noi no. Certo, da qui a dire che si tratta di un rilievo artificiale ci passa la stessa distanza che separa la Terra da Marte, ma un dato a noi pare certo: questa Surface Feature NON E' rappresentativa n di un cratere "tradizionale" (e cio "da impatto"), n di un pozzo da collasso (e cio il risultato finale di una subsidenza ---> cedimento di una struttura a causa del suo stesso peso).
E' una "Planetary Oddity": una "Stranezza Planetaria", che va osservata e studiata. Tutto qui.MareKromium
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