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Status Report DAWN DISCOVERY MISSION: STATUS REPORT C. T. Russell 1, C. A. Raymond 2, T. C. Fraschetti 2, M. D. Rayman 2, J. McCarthy 3, A. C. Grandfield 3 1 IGPP & ESS, UCLA, Los Angeles, CA 90095, USA; E-mail: [email protected] 2 JPL, 4800 Oak Grove Dr., Pasad ena, CA 91109 ,USA 3Orbital Sciences Corporation, Dulles, VA 20166 , USA ABSTRACT temperature in the interior of planets is sufficiently high that they evolve thermally and differentiate over The Dawn mission is the ninth spacecraft in the the age of the sola r system. In order to understand the Discovery series, selected for study in January 2001 planet -forming process we wish to be able to resolve and approved for development in December 2001. It is the heliocentric gradient in the solar nebula. The now being readied for launch in late June 2006 to asteroid belt is the best region in which to explore this rendezvous with and orbit the two largest minor planets gradient, because shortly after the formation of the be lt, 4 Vesta and 1 Ceres. Dawn is the first purely science Jupiter condensed and began to stir the asteroids mission to use ion propulsion as an enabling gravitationally . This stirring was sufficient to stop technology and the first to orbit two planetary bodies accretion and to begin the collisional disruption of the other than E arth. This mission is well into its assembly protoplanets in the belt. The resultant, rather small test and launch operations phase. This paper gives an sizes of the asteroids kept thei r thermal evolution to a overview of the science objectives and payload, reports minimum. The largest of these bodies, especially 1 on the status of the mission, and provides pointers to Ceres and 4 Vesta, survived the collisions and seem the literature describing the Dawn mission in greater not to have moved greatly from their point of detail. formation. Dawn’s objective is to place constraints on the nature of the ea rly solar nebulae by learning as 1. INTRODUCTION much as we can about the two very different bodies. Planetary systems arise in cold clouds of dust and gas, Vesta, the closer to the Sun, lies at 2.34 Astronomical called nebulae. The dust forms from minerals that Units (AU). Telescopic observations show it to be precipitate as the gas cools. The dust then accretes into roughly a triaxial ellipsoid of dimensions 289 x 280 x ever larger bodies, or planetary embryos, eventuall y 229 km, with a large southern crater. Its surface has forming protoplanets, and then planets. Hot stars may the reflectance spectrum of basalt. This spectrum is also form in the nebula through gravitational very similar to the reflected spectrum of light from the instabilities, shine brightly, dissipate the gas, and leave Howardite -Eucrite -Diogenite class of meteorite only the orbiting bodies. The history of this process is (HEDs). Most asteroid researchers believe that the largely hidden from view by the d istance of these HED meteorites derive from the disruption of larger planet -forming regions, and in the case of our own bodies or v estoids, ejected from Vesta during the solar system, the thermal and dynamical evolution of southern cratering event. Some of this material now the system. resides near orbital resonances with Jupiter at which point they can be perturbed onto impact traj ectories The solar system consists of several distinct classes of with Earth, producing 5% of observed meteorite falls. bodies: the terrestrial planets that are largely silicate These HED meteorites, in turn, allow us to paint a mantle s surrounding iron cores; the gas giants that are picture of Vesta that is very consistent with the hydrogen -helium balls around rocky cores, some with inferences from the reflectance spectra. Vesta is a dry, thick water mantles between these two layers. There rocky body with an iron core. It has extensively are several belts of smaller bodies, the main asteroid melted, recrystallized, and formed a differentiated body belt between Mars and Jupiter, the Kuiper b elt beyond [1]. Neptune, closely related to Pluto, and the Oort cloud beyond that. It is difficult to learn much about the Ceres, the larger body, lies at 2.77 AU. Recent Hubble early solar nebula from the present -day planets. The observations show that Ceres is rotationally symmetric planets are well separated. The composition of each and oblate with dimensions 487 x 487 x 455 km [2]. planet is expected to be an av erage over the material The shape is not consistent with a homogeneous originally in a broad region of the solar nebula in the density but rather with a two -layer structure, a rocky approximate neighborhood of the planet. The core covered with a 100 -km ice mantle. Because ice is Fig. 1 Two assembled framing cameras, covered by thermal blankets, after successfully completing Fig. 2 The visible and infrared spectrometer (VIR) environmen tal testing mounted to the vibration test table with GSE fixturing not visible on the surface it must be covered by a thick Rosetta mission. The detector and readout electronics layer of dust. This surface is dark but has discernible are copies of the units implemented in the downward - features. Some of these features are circular but at this looking imager (ROLIS) from Rosetta. The camera is time we cannot be certain as to the source of these provided by the Max -Planck -Institut fur features [3]. Th ese observations are consistent with the Sonnensystemforschung (MPS) in Lindau Germany earlier modeling predictions [4]. under the leadership of H. Uwe Keller with assist ance from the Institut fur Plane tenforsch ung of the Improvement in our understanding of Vesta and Ceres Deutsches Zentrum fur Luft -und Raumfahrt (DLR) in has paralleled the development of the flight system. Berlin. The DPU is fabricated by the Institut fur This evolution has proceeded not just through the Datentechnik und Kommunikationsnetze of the efforts of the Dawn sci ence team, but as a concerted Technische Universitat Braunschweig. The two effort of the members of the science community, both redundant framing cameras have been delivered to the inside and outside the Dawn family. It occurs both in spacecraft. collaborations with Dawn team members and in independent studies. The existence of a mission to The mapping spectrometer, illustrated in Figure 2, targets such as Ve sta and Ceres does much to focus combines two data channels in one compact instrument attention, and provide direction to the efforts of the with a visible channel from 0.25 to 1.0 microns and an scientific community [5]. infrared channel from 1 to 5 microns. The instantaneous field of view is 500 m/pix el at 200 km 2. SCIENTIFIC PAYLOAD with a full field of view of 64 mrad. The spectrometer is a modification of the Rosetta mapping spectrometer The spacecraft carries three scientific instruments: a (VIRTIS) that in turn derives much heritage from the framing camera, a visible and infrared spectrometer, Cassini VIMS spectrometer. The spectrometer is and a gamma ray and neutron spectrometer. In provided to Dawn by the Agenzia Spaziale Italiana addition gravity measurements will be obtained (ASI) under the direction of Angioletta Coradini of the through analysis of the radio transmissions and other Instituto Nazionale Di Astrofisica (INAF). The navigational measurements. The camera, illustrated in spectrometer was designed, built and tested at Galileo Figure 1, has two identical (and redundant) units and Avionica. At this writing the main electronics has been obtai ns images on a frame transfer CCD with 1024 x delivered to Orbital a nd returned to Galileo Avionica 1024 sensitive pixels. The camera samples the surface for refurbishment. It is expected to be returned to of the bodies with a resolution of 18.6 m/pixel a Orbital and installed by the end of the ICLCPM distance of 200 km. The camera serves to provide conference. optical navigation data as well as scientific data. Th e camera includes a filter wheel with one clear filter and The gamma ray and neutron spectrometer (GRaND), 7 spectral filters. The heritage of the camera is based illustrated in Figure 3, maps the abundance of rock on several previous missions, including a data forming el ements (O, Si, Fe, Ti, Mg, Al, and Ca) as processing unit from the Venus Monitoring Camera on well as radioactive elements (K, U, Th) and elements the Venus Express Mission, with an oper ating system such as H, C and N that are major constituents of ices. developed for the science imager (OSIRIS) from the The instrument draws on decades of experience in 2 The solar array is 19.7 m tip -to -tip and prov ides approximately 10 kW of power at 1 AU. During launch the two five -paneled solar array wings are folded against the sides of the spacecraft, and are deployed after successful injection into the launch trajectory. The solar array is Dawn’s only deploy able appendage. Figure 5 shows one wing of Dawn’s solar array, deployed at the manufacturer’s facility. Other mechanical systems include gimbals for the thrusters and covers for the optical instruments. The core of the spacecraft is a central thrust tu be inside of which are the two fuel tanks, one for hydrazine used by the reaction control system and one for the ion propulsion system’s xenon. The external panels are Fig. 3 The gamma ray neutron spectrometer prior t o mounted to the thrust tube forming the bus structure. thermal blanket installation The thrust tube also supports the solar array that rotates around its longitudinal axis so that the solar panels can measuring neutrons and energetic photons.
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