|Major contractors||Orbital Sciences · JPL · UCLA|
|Mission type||Flyby / Orbiter|
|Launch date||September 27, 2007, 11:34:00 UTC
( 7 years, 83 days ago)
|Launch vehicle||Delta II 7925H|
|Launch site||Space Launch Complex 17B
Cape Canaveral Air Force Station, Florida, United States
|Mission duration||through July 2015|
|Flyby of||Mars (February 4, 2009)|
|Satellite of||Vesta (July 2011 – September 2012)
|Orbital insertion date||Vesta: July 16, 2011, 04:47 UTC
(3 years, 5 months and 3 days ago)
Ceres: April 2015 (projected)
|Mass||1,240 kg (2,730 lb) (wet)|
|Power||1300 W (Solar array) at 3 AU|
Dawn is a space probe launched by NASA on September 27, 2007, to study two of the most massive objects of the asteroid belt – the protoplanet Vesta and the dwarf planet Ceres. Currently en route to Ceres, it is expected to arrive in April 2015. Dawn was the first spacecraft to visit Vesta, entering orbit on July 16, 2011, and successfully completing its fourteen month survey mission of Vesta in late 2012. Should its entire mission succeed, it will also be the first spacecraft to visit Ceres and to orbit two separate extraterrestrial bodies.
The mission is managed by NASA's Jet Propulsion Laboratory, with major components contributed by European partners from the Netherlands, Italy and Germany. It is the first NASA exploratory mission to use ion propulsion to enter orbits; previous multi-target missions using conventional drives, such as the Voyager program, were restricted to flybys.
- 1 Project history
- 2 Scientific background
- 3 Objectives
- 4 Specifications
- 5 Mission summary
- 6 See also
- 7 References
- 8 External links
The status of the Dawn mission changed several times. The project was cancelled in December 2003, and then reinstated in February 2004. In October 2005, work on Dawn was placed in "stand down" mode, and in January 2006, the mission was discussed in the press as "indefinitely postponed", even though NASA had made no new announcements regarding its status. On March 2, 2006, Dawn was again cancelled by NASA.
The spacecraft's manufacturer, Orbital Sciences Corporation, appealed NASA's decision, offering to build the spacecraft at cost, forgoing any profit in order to gain experience in a new market field. NASA then put the cancellation under review, and on March 27, 2006, it was announced that the mission would not be cancelled after all. In the last week of September 2006, the Dawn mission's instrument payload integration reached full functionality. Although originally projected to cost US$373 million, cost overruns inflated the final cost of the mission to US$446 million in 2007. The Dawn mission team is led by Christopher T. Russell.
The Dawn mission was designed to study two large bodies in the asteroid belt in order to answer questions about the formation of the Solar System, as well as to test the feasibility of its ion drive. Ceres and Vesta were chosen as two contrasting protoplanets, the first one apparently "wet" (i.e. icy and cold) and the other "dry" (i.e. rocky), whose accretion was terminated by the formation of Jupiter. The two bodies provide a bridge in scientific understanding between the formation of rocky planets and the icy bodies of the Solar System, and under what conditions a rocky planet can hold water.
The IAU adopted a new definition of planet on August 24, 2006, which introduced the term "dwarf planet" for ellipsoidal worlds that were too small to qualify for planetary status by "clearing their orbital neighborhood" of other orbiting matter. If the IAU's definition stands and the spacecraft experiences no delays, Dawn will be the first mission to study a dwarf planet, arriving at Ceres a few months before the arrival of the New Horizons probe at Pluto in July 2015.
Ceres is a dwarf planet whose mass comprises about one-third of the total mass of the bodies in the asteroid belt, and whose spectral characteristics suggest a composition similar to that of a water-rich carbonaceous chondrite. Vesta, a smaller, water-poor achondritic asteroid, has experienced significant heating and differentiation. It shows signs of a metallic core, a Mars-like density and lunar-like basaltic flows.
Available evidence indicates that both bodies formed very early in the history of the Solar System, thereby retaining a record of events and processes from the time of the formation of the terrestrial planets. Radionuclide dating of pieces of meteorites thought to come from Vesta suggests that Vesta differentiated quickly, in three million years or less. Thermal evolution studies suggest that Ceres must have formed some time later, more than three million years after the formation of CAIs (the oldest known objects of Solar System origin).
Moreover, Vesta appears to be the source of many smaller objects in the Solar System. Most (but not all) V-type near-Earth asteroids, and some outer main-belt asteroids, have spectra similar to Vesta, and are thus known as vestoids. Five percent of the meteoritic samples found on Earth, the howardite–eucrite–diogenite (HED) meteorites, are thought to be the result of a collision or collisions with Vesta.
In 2005, Peter Thomas of Cornell University proposed that Ceres has a differentiated interior; its oblateness appears too small for an undifferentiated body, which indicates that it consists of a rocky core overlain with an icy mantle. There is a large collection of potential samples from Vesta accessible to scientists, in the form of over 1,400 HED meteorites, giving insight into Vestan geologic history and structure. Vesta is thought to consist of a metallic iron–nickel core, an overlying rocky olivine mantle and crust.
The Dawn mission's goal is to characterize the conditions and processes of the Solar System's earliest eon by investigating in detail two of the largest protoplanets remaining intact since their formation. The primary question that the mission addresses is the role of size and water in determining the evolution of the planets. Ceres and Vesta are highly suitable bodies with which to address this question, as they are two of the most massive of the protoplanets. Ceres is geologically very primitive and icy, while Vesta is evolved and rocky. Their contrasting characteristics are thought to have resulted from them forming in two different regions of the early Solar System.
There are three principal scientific drivers for the mission. First, the Dawn mission can capture the earliest moments in the origin of the Solar System, enabling us to understand the conditions under which these objects formed. Second, Dawn determines the nature of the building blocks from which the terrestrial planets formed, improving our understanding of this formation. Finally, it contrasts the formation and evolution of two small planets that followed very different evolutionary paths, so that we can understand what controls that evolution.
With its solar array in the retracted launch position, the Dawn spacecraft is 2.36 meters (7.7 ft) long. With its solar arrays fully extended, Dawn is 19.7 meters (65 ft) long. Total area of solar arrays is 36.4 square metres (392 sq ft).
The Dawn spacecraft is propelled by three xenon ion thrusters that inherited NSTAR engineering technology from the Deep Space 1 spacecraft. They have a specific impulse of 3,100 s and produce a thrust of 90 mN. The whole spacecraft, including the ion propulsion thrusters, is powered by a 10 kW (at 1 AU) triple-junction gallium arsenide photovoltaic solar array manufactured by Dutch Space. To get to Vesta, Dawn is allocated 275 kg (606 lb) of xenon, with another 110 kg (243 lb) to reach Ceres, out of a total capacity of 425 kg (937 pounds) of on-board propellant. With the propellant it carries, Dawn can perform a velocity change of more than 10 km/s over the course of its mission, far more than any previous spacecraft achieved with onboard propellant after separation from its launch rocket. Dawn is NASA's first purely exploratory mission to use ion propulsion engines.
Dawn carries a memory chip bearing the names of more than 360,000 space enthusiasts. The names were submitted online as part of a public outreach effort between September 2005 and November 4, 2006. The microchip (about the size of a United States nickel coin) was installed on May 17, 2007 above the forward ion thruster, underneath the spacecraft's high-gain antenna. More than one microchip was made, with a back-up copy put on display at the 2007 Open House event at the Jet Propulsion Laboratory in Pasadena, California.
NASA's Jet Propulsion Laboratory provided overall planning and management of the mission, the flight system and scientific payload development, and provided the Ion Propulsion System. Orbital Sciences Corporation provided the spacecraft, which constituted the company's first interplanetary mission. The Max Planck Institute for Solar System Research and the German Aerospace Center (DLR) provided the framing cameras, the Italian Space Agency provided the mapping spectrometer, and the Los Alamos National Laboratory provided the gamma ray and neutron spectrometer.
- Framing camera (FC) — The framing camera uses 20 mm aperture, f/7.9 refractive optical system with a focal length of 150 mm. A frame-transfer charge-coupled device (CCD), a Thomson TH7888A, at the focal plane has 1024 × 1024 sensitive 93-μrad pixels, yielding a 5.5° x 5.5° field of view. An 8-position filter wheel permits panchromatic (clear filter) and spectrally selective imaging (7 narrow band filters). The broadest filter allows imaging from about 400 to 1050 nm. In addition, the framing camera will acquire images for optical navigation in the vicinities of Vesta and Ceres. The FC computer is a custom radiation-hardened Xilinx system with a LEON2 core and 8 GiB of memory. The camera will offer resolutions of 17 m/pixel for Vesta and 66 m/pixel for Ceres. Because the framing camera is vital for both science and navigation, the payload has two identical and physically separate cameras (FC1 & FC2) for redundancy, each with its own optics, electronics, and structure.
- Visible and infrared spectrometer (VIR) — This instrument is a modification of the visible and infrared thermal-imaging spectrometer used on the Rosetta and Venus Express spacecraft. It also draws its heritage from the Saturn orbiter Cassini's visible and infrared mapping spectrometer. The spectrometer's VIR spectral frames are 256 (spatial) × 432 (spectral), and the slit length is 64 mrad. The mapping spectrometer incorporates two channels, both fed by a single grating. A CCD yields frames from 0.25 to 1.0 μm, while an array of HgCdTe photodiodes cooled to about 70K spans the spectrum from 0.95 to 5.0 μm.
- Gamma Ray and Neutron Detector (GRaND) — This instrument is based on similar instruments flown on the Lunar Prospector and Mars Odyssey space missions. This instrument includes 21 sensors with a very wide field of view. It will be used to measure the abundances of the major rock-forming elements (oxygen, magnesium, aluminium, silicon, calcium, titanium, and iron) on Vesta and Ceres, as well as potassium, thorium, uranium, and water (inferred from hydrogen content).
On April 10, 2007, the spacecraft arrived at the Astrotech Space Operations subsidiary of SPACEHAB, Inc. in Titusville, Florida, where it was prepared for launch. The launch was originally scheduled for June 20, but was delayed until June 30 due to delays with part deliveries. A broken crane at the launch pad, used to raise the solid rocket boosters, further delayed the launch for a week, until July 7; prior to this, on June 15, the second stage was successfully hoisted into position. A mishap at the Astrotech Space Operations facility, involving slight damage to one of the solar arrays, did not have an effect on the launch date; however, bad weather caused the launch to slip to July 8. Range tracking problems then delayed the launch to July 9, and then July 15. Launch planning was then suspended in order to avoid conflicts with the Phoenix mission to Mars, which was successfully launched on August 4.
A discussion of Dawn’s launch is included in the first chapter of "The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres". The launch of Dawn was rescheduled for September 26, 2007, then September 27, due to bad weather delaying fueling of the second stage, the same problem that delayed the July 7 launch attempt. The launch window extended from 07:20–07:49 EDT (11:20–11:49 GMT). During the final built-in hold at T−4 minutes, a ship entered the exclusion area offshore, the strip of ocean where the rocket boosters were likely to fall after separation. After commanding the ship to leave the area, the launch was required to wait for the end of a collision avoidance window with the International Space Station. Dawn finally launched from pad 17-B at the Cape Canaveral Air Force Station on a Delta 7925-H rocket at 07:34 EDT, reaching escape velocity with the help of a spin-stabilized solid-fueled third stage. Thereafter, Dawn's ion thrusters took over.
After initial checkout, during which the ion thrusters accumulated more than 11 days of thrust, Dawn began long-term cruise propulsion on December 17, 2007. On October 31, 2008, Dawn completed its first thrusting phase to send it on to Mars for a gravity assist flyby in February 2009. During this first interplanetary cruise phase, Dawn spent 270 days, or 85% of this phase, using its thrusters. It expended less than 72 kilograms of xenon propellant for a total change in velocity of 1.81 kilometers per second. On November 20, 2008, Dawn performed its first trajectory correction maneuver (TCM1), firing its number 1 thruster for 2 hours, 11 minutes.
Dawn made its closest approach (549 km) to Mars on February 17, 2009 during a successful gravity assist. On this day, the spacecraft placed itself in safe mode, resulting in some data acquisition loss. The spacecraft was reported to be back in full operation two days later, with no impact on the subsequent mission identified. The root cause of the event was reported to be a software programming error.
To cruise from Earth to its targets, Dawn traveled in an elongated outward spiral trajectory. NASA posts and continually updates the current location and status of Dawn online. The actual Vesta chronology and estimated Ceres chronology is as follows:
- September 27, 2007: launch
- February 17, 2009: Mars gravity assist
- July 16, 2011: Vesta arrival and capture
- August 11, 2011 - August 31, 2011: Vesta survey orbit
- September 29, 2011 - November 2, 2011: Vesta first high altitude orbit
- December 12, 2011 - May 1, 2012: Vesta low altitude orbit
- June 15, 2012 - July 25, 2012: Vesta second high altitude orbit
- September 5, 2012: Vesta departure
- March–April 2015 : Ceres arrival
- Early 2016: End of primary Ceres operations
On May 3, 2011, Dawn acquired its first targeting image, 1,200,000 km from Vesta, and began its approach phase to the asteroid. On June 12, Dawn's speed relative to Vesta was slowed in preparation for its orbital insertion 34 days later.
Dawn was scheduled to be inserted into orbit at 05:00 UTC on July 16 after a period of thrusting with its ion engines. Because its antenna was pointed away from the Earth during thrusting, scientists were not able to immediately confirm whether or not Dawn successfully made the maneuver. The spacecraft would then reorient itself, and was scheduled to check in at 06:30 UTC on July 17. NASA later confirmed that it received telemetry from Dawn indicating that the spacecraft successfully entered orbit around Vesta. The exact time of insertion could not be confirmed, since it depended on Vesta's mass distribution, which has only been estimated.
After being captured by Vesta's gravity and entering its orbit on July 16, 2011. Dawn moved to a lower, closer orbit by running its xenon-ion engine using solar power. On August 2, it paused its spiralling approach to enter a 69-hour survey orbit at an altitude of 2,750 km. It assumed a 12.3-hour high-altitude mapping orbit at 680 km on September 27, and finally entered a 4.3-hour low-altitude mapping orbit at 210 km on December 8, 2011.
In May 2012, NASA released the preliminary results of Dawn's study of Vesta, including estimates of the size of Vesta's metal-rich core, which is theorized to be 220 km across. NASA scientists furthermore stated that they believed Vesta to be the "last of its kind" – the only remaining example of the large planetoids that came together to form the rocky planets during the formation of the Solar System. In October 2012, NASA stated that data from Dawn had revealed the origin of anomalous dark spots and streaks on Vesta's surface, which were likely deposited by ancient asteroid impacts. In December 2012, it was reported that Dawn had observed gullies on the surface of Vesta that were interpreted to have been eroded by transiently flowing liquid water. More details about the Dawn mission’s scientific discoveries at Vesta are included on the Vesta page.
Dawn was originally scheduled to depart Vesta and begin its journey to Ceres on August 26, 2012. However, a problem with one of the spacecraft's reaction wheels forced Dawn to delay its departure from Vesta's gravity until September 5, 2012. Dawn successfully departed Vesta on this date. It is scheduled to arrive at Ceres in late March or early April 2015, three to four months prior to the arrival of New Horizons at Pluto; Dawn will thus be the first mission to study a dwarf planet at close range. Images taken from Dawn of Ceres will exceed the resolution of the Hubble Space Telescope by January 26, 2015, while images taken from New Horizon of Pluto will exceed the resolution of the Hubble Space Telescope by approximately May 5, 2015. Dawn's mission profile calls for it to enter orbit around Ceres at an initial altitude of 13,500 km for a first full characterization. Dawn will then spiral down to a survey orbit at an altitude of 4,430 km. This phase will last for 22 days, and is designed to obtain a global view of Ceres with Dawn's framing camera, and global maps with the visible and infrared mapping spectrometer (VIR). Dawn will then spiral down to an altitude of 1,480 km, where in August 2015 it will begin a two-month phase known as the high-altitude mapping orbit. During this phase, Dawn will continue to acquire near-global maps with the VIR and framing camera at higher resolution than in the survey phase. It will also image in stereo to resolve the surface in 3D. After spiralling down for another two months, Dawn will begin its closest orbit around Ceres in late November 2015, at a distance of about 375 km. This orbit is designed to acquire data (for 3 months) with Dawn's gamma-ray and neutron detector (GRaND) and gravity investigation.
- Comparable missions
- Galileo probe – 951 Gaspra and 243 Ida flybys
- Hayabusa – 25143 Itokawa rendezvous and sample return
- Near Earth Asteroid Rendezvous (NEAR) – 253 Mathilde flyby, orbited 433 Eros from 2000-2001
- Rosetta – 2867 Šteins and 21 Lutetia flyby, is orbiting 67P/Churyumov–Gerasimenko
- Other related articles
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- "Dawn probe spies possible water-cut gullies on Vesta". BBC. 6 December 2012. Retrieved 8 December 2012.
- Staff, Space.com. "NASA's Dawn Spacecraft Says Goodbye to Giant Asteroid Vesta". Yahoo.com. Retrieved 6 September 2012.
- "'Dawn has departed the giant asteroid Vesta'". NASA/JPL. 2012-09-05.
- Williams, D. A.; Yingst, R. A.; Garry, W. B. (December 2014). "Introduction: The geologic mapping of Vesta". Icarus 244: 1–12. doi:10.1016/j.icarus.2014.03.001.
- Scully, J. E. C.; Yin, A.; Russell, C. T.; Buczkowski, D. L.; Williams, D. A.; Blewett, D. T.; Ruesch, O.; Hiesinger, H.; Le Corre, L.; Mercer, C.; Yingst, R. A.; Garry, W. B.; Jaumann, R.; Roatsch, T.; Preusker, F.; Gaskell, R. W.; Schröder, S. E.; Ammannito, E.; Pieters, C. M.; Raymond, C. A. (December 2014). "Geomorphology and structural geology of Saturnalia Fossae and adjacent structures in the northern hemisphere of Vesta". Icarus 244: 23–40. doi:10.1016/j.icarus.2014.01.013.
- Schäfer, M.; Nathues, A.; Williams, D. A.; Mittlefehldt, D. W.; Le Corre, L.; Buczkowski, D. L.; Kneissl, T.; Thangjam, G. S.; Hoffmann, M.; Schmedemann, N.; Schäfer, T.; Scully, J. E. C.; Li, J. Y.; Reddy, V.; Garry, W. B.; Krohn, K.; Yingst, R. A.; Gaskell, R. W.; Russell, C. T. (December 2014). "Imprint of the Rheasilvia impact on Vesta – Geologic mapping of quadrangles Gegania and Lucaria". Icarus 244: 60–73. doi:10.1016/j.icarus.2014.06.026.
- Kneissl, T.; Schmedemann, N.; Reddy, V.; Williams, D. A.; Walter, S. H. G.; Neesemann, A.; Michael, G. G.; Jaumann, R.; Krohn, K.; Preusker, F.; Roatsch, T.; Le Corre, L.; Nathues, A.; Hoffmann, M.; Schäfer, M.; Buczkowski, D.; Garry, W. B.; Yingst, R. A.; Mest, S. C.; Russell, C. T.; Raymond, C. A. (December 2014). "Morphology and formation ages of mid-sized post-Rheasilvia craters – Geology of quadrangle Tuccia, Vesta". Icarus 244: 133–157. doi:10.1016/j.icarus.2014.02.012.
- "'Dawn Engineers Assess Reaction Wheel'". 2012-08-18.
- "NASA's Dawn Fills out its Ceres Dance Card". NASA. 2013-12-03. Retrieved 2013-12-08.
- McCord, Thomas B.; Castillo-Rogez, Julie; Rivkin, Andy (2011). "The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres". p. 63. doi:10.1007/978-1-4614-4903-4_5. ISBN 978-1-4614-4902-7.
Media related to Dawn (spacecraft) at Wikimedia Commons
- Dawn mission home page at JPL
- Dawn mission home page at NASA
- Visible and Infrared Spectrometer Instrument at INAF (Istituto Nazionale di Astrofisica)
- Dawn Framing Camera at Max Planck Institute for Solar System Research
- Gamma Ray and Neutron Spectrometer for Dawn, short paper on the instrument, from 37th Lunar and Planetary Science Conference
- http://dawndata.igpp.ucla.edu Download Dawn data here