DEPARTMENT “ASTEROIDS COMETS” IX. Annual Report 2005...2.5 Asteroid search and follow-up...

Deutsches Zentrum für Luft- und Raumfahrt e.V. German Aerospace Center Institut für Planetenforschung Institute of Planetary Research

ASTEROIDS

Comets

SPACE MISSIONS MODELS

DDEEPPAARRTTMMEENNTT:: ““AASSTTEERROOIIDDSS AANNDD CCOOMMEETTSS”” IX. Annual Report

2005

http://solarsystem.dlr.de/KK

From left to right Dr. Jörg Knollenberg [email protected] Scientific staff member Dr. Gerhard Hahn [email protected] Scientific staff member Dr. Ekkehard Kührt [email protected] Section leader Prof. Uwe Motschmann [email protected] Guest scientist Laura Brumm [email protected] Secretary Detlef de Niem [email protected] Scientific staff member Dr. Carmen Tornow [email protected] Scientific staff member Michael Müller [email protected] PhD student Dr. Alan W. Harris [email protected] Deputy section leader Not appearing in the photo: Dr. Stefano Mottola [email protected] Scientific staff member

Thermal-infrared image (8 – 14 μm), changed order

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mailto:[email protected]










Contents 1. Introduction (EK)

2. Asteroid science

2.1 Investigations of the physical properties of asteroids with the NASA Infrared Telescope Facility (Harris, Müller)

2.2 Observations of asteroids with the Spitzer Space Telescope (Harris, Mueller)

2.3 Asteroid thermal modelling (Müller, Harris)

2.4 Photometric observations of main-belt and near-Earth asteroids (Mottola, Hahn, Harris, Müller)

2.5 Asteroid search and follow-up programmes (Hahn)

2.6 Orbital evolution studies of Saturn family comets (Hahn)

3. Comet science

3.1 Hydrodynamical influence on formation of HCN molecules in hot cores (Tornow, Kührt, Motschmann)

3.2 Modelling the solar wind interaction with weakly outgassing comets by a hybrid model (Motschmann, Kührt)

4. Impact phenomena

4.1 Meteorite ejecta range after terrestrial impacts (de Niem, Kührt, Motschmann)

4.2. Physical limits of solar collectors in deflecting Earth-threatening asteroids (Kahle, Kührt, Hahn, Knollenberg)

5. Contributions to space missions

5.1 Rosetta-Mupus (Knollenberg, Kührt, Spohn, Schrödter)

5.2 Rosetta-Rolis (S. Mottola, H. Michaelis)

5.3 DAWN (S. Mottola, R. Jaumann)

5.4 Don Quijote: Study of a hazardous asteroid mitigation pre-cursor mission (Harris)

5.5 Deep Impact measurements and simulations (Knollenberg, de Niem, Kührt)

6. Technology projects

6.1 HP3 (Knollenberg, Nadalini)

6.2 FIREWATCH (Kührt, Knollenberg, Behnke, Mertens)

7. Appendix

7.1 Scientific publications in refereed journals and books (submitted or published in 2004)

7.2 Scientific publications in other journals and proceedings (published in 2004)

7.3. Minor Planet Circulars/Electronic Circulars

7.4 Publications in the popular literature and public outreach

7.5 Observing campaigns 2004

7.6 Space mission responsibilities

7.7 Other events and activities

7.8 Funding

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1. Introduction (E. Kührt)

This report describes the work of the “Asteroids and Comets” Department of the Institute of Planetary Research of the DLR (German Aerospace Center) during the year 2005. The Department consisted of 7 scientists and 1 PhD student; two guest scientists, one from the Assam University, India, and one from the Technical University Braunschweig, worked in the Department during the year. Our scientific goal is to investigate small bodies by observing them in the visible, infrared, and other wavelength ranges, contributing to relevant space missions and modelling physical processes associated with this class of object. Other fields of interest are risk evaluation of impacts of Near Earth Objects (NEOs) on our home planet, the origin of life and the transfer of space technology to solve environmental problems on Earth.

Scientific interest in the minor bodies of the Solar System stems mainly from the crucial role they appear to have played in the formation of the planets and the development of life. Asteroids and comets are thought to be remnant material from the process of formation and the initial development of planets. Due to their peculiar dynamical and physical properties, such as small size, lack of a permanent atmosphere, and relatively little thermal processing, these objects have remained largely unaltered since the time of Solar System formation. Consequently, comets and asteroids should contain a wealth of information on conditions in the protoplanetary nebula. Many scientists believe that comets and asteroids have significantly influenced the evolution of the terrestrial planets and life on Earth. In particular, scientific and public interest in near-Earth asteroids has risen in recent years. Activities in these fields are a part of our DLR-project “Comets and asteroids”. They are summarized in Sections 2, 3, and 4.

Contributions to several space missions are described in Section 5. We are involved in Rosetta to comet Churyumov-Gerasimenko with 1 Principal Investigator, 1 Project Manager and 8 Coinvestgator-ships and in the Science Team of the DAWN mission to asteroids Ceres and Vesta. The progress in our technology transfer projects is discussed in Section 6.

The Appendix summarises publications, project contributions, observation campaigns, public outreach activities, and our funding.

2. Asteroid Science

2.1. Investigations of the physical properties of asteroids with the NASA Infrared Telescope Facility (Harris, Müller)

The NASA Infrared Telescope Facility (IRTF) is a 3-m telescope situated on Mauna Kea, Hawaii. Our project has been awarded observing time on the IRTF regularly over the past 5 years. It has recently become possible to carry out observations remotely from Berlin, which means that, without heavy travel costs, observing time can be scheduled at intervals of a few days over a total period of weeks to study the variation of infrared emission from asteroids as their observing geometry changes. The resulting data can reveal important information on the surface characteristics of asteroids, especially thermal inertia. A major focus of our work with the IRTF is near-Earth asteroids (NEAs). This year saw the publication in Icarus of our work on (1580) Betulia, in which revised values of size and albedo and a thermal inertia of 180 J m-2s-0.5 K-1 were obtained for this unusual C-type NEA. This is amongst the first determinations of thermal inertia for NEAs; it is some three times higher than the lunar value but an order of magnitude less than that expected for a bare rock surface. Our result for Betulia is consistent with recently obtained values for other NEAs discussed in Section 2.3.

Our programme was awarded a total of 8 x 0.5 nights of observing time with the NASA IRTF in the 2005 observing schedule. However, the quality of thermal-infrared data, especially in the case of weak targets, is very dependent on atmospheric conditions and on several occasions in 2005 we were forced to turn to a back-up programme of observations of relatively bright main-belt M-type asteroids because of unfavourable conditions.

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Fig. 2.1 Thermal-infrared flux measurements of the M-type asteroid (16) Psyche, with model thermal continua for different values of thermal inertia overlaid. The flux measurements in the case of Psyche are indicative of relatively high thermal inertia. The data set shown was taken in 2004. Similar data sets were obtained in 2005 for all the M-type asteroids mentioned in the text.

Very low thermal inertia

Higher thermal inertia

One of the major current questions concerning asteroid mineralogy is the nature of M-type asteroids. Are M-type asteroids really metallic or not? We were able to obtain useful multi-filter thermal-infrared flux measurements of the main-belt M-type asteroids (16) Psyche, (21) Lutetia, (129) Antigone, (135) Hertha, (201) Penelope, (216) Kleopatra, and (785) Zwetana. Preliminary results indicate that (16) Psyche and (216) Kleopatra have relatively high values of thermal inertia. Furthermore, Psyche and Kleopatra also have very high radar albedos and therefore presumably have metallic surfaces. On the other hand, Lutetia appears to have normal values of thermal inertia and radar reflectivity. In the cases of Lutetia, Antigone, Hertha, and Penelope, for which our observations indicate normal thermal inertia, near-infrared reflectance spectroscopy provides evidence for hydrated surfaces, indicating that these objects are not metallic. To summarize: there may be a correlation between thermal inertia and radar reflectivity, which would indicate that thermal inertia is a useful indicator of metallic surfaces, and our results are consistent with recent findings that many M-type asteroids appear to be of non-metallic composition.

Our study of the physical characteristics of (21) Lutetia was completed with the acceptance of the work for publication in Astronomy and Astrophysics. Our derived albedo of 0.21, typical for an M-type object, agrees well with the IRAS albedo and rules out the possibility, suggested on the basis of spectroscopic observations, that Lutetia may actually have a carbonaceous composition.

2.2. Observations of asteroids with the Spitzer Space Telescope (Harris, Mueller)

Two proposals submitted for observing time with Spitzer (Figure 2.2) in 2005 were awarded a total of 24 hr. observing time. The programmes are led by Harris and Mueller, respectively, and include a total of 7 co-investigators from Europe and the USA:

1. The Karin cluster asteroids in the main belt display very similar proper orbital elements and are therefore assumed to be dynamically related. The cluster, named after its largest member, (832) Karin, is believed to have been formed 5.8 ± 0.2 Myr ago in a catastrophic collision and thus to be significantly younger than most known asteroid families. The cluster is of great interest due to the

fact that the physical properties of its members may preserve unique information about asteroid fragmentation and surface processes on small asteroids, which include regolith formation and modification of albedo and spectral properties via space weathering. Our Spitzer observations of 17 Karin cluster members should allow us to determine their sizes, albedos and information on thermal inertia. The questions that can be addressed with these observations include: Are the distributions of sizes and albedos compatible with the Karin cluster being the result of a single catastrophic collision

Fig. 2.2 Spitzer Space Telescope

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5.8±0.2 Myr ago? Are the sizes and thermal properties of the Karin cluster members compatible with the claim that the Yarkovsky effect is responsible for an apparent non-gravitational drift of their orbital motion?

2. Observations of 2000 PH5, a very small (D ≈ 150 m), rapidly rotating NEA have been completed. Data reduction and analysis are currently in progress. This object presents a unique opportunity to gain insight into the thermal inertia of what, according to current understanding, should be a regolith-free surface. NEAs studied to date with sizes down to several 100 m do not display the very high thermal-inertia values expected for regolith-free surfaces. A clearer knowledge of the thermal properties of small NEAs, such as thermal inertia and conductivity, is vital to improve calculations of the gradual orbital drift of small asteroids due to the reactive force resulting from the anisotropic emission of thermal photons (the “Yarkovsky effect”). For example, the orbital evolution of potentially hazardous asteroids depends on the Yarkovsky effect.

2.3. Asteroid thermal modelling (Müller, Harris)

We have continued to develop and test a sophisticated thermophysical model that takes account of an object’s size, shape, rotation vector, thermal inertia, emissivity, albedo, and surface roughness. The application of the model to thermal-IR spectrophotometric data of asteroids leads to more robust estimates of asteroid diameters, albedos and surface thermal inertia, compared to simpler thermal models. Thermal inertia is a measure of a material’s resistance to temperature changes, from which conclusions on the physical nature of the material can be drawn.

A new method to determine the average surface thermal inertia of a sample of asteroids, when insufficient data is available for thermal modelling of individual objects, has been developed in collaboration with M. Delbo (Turin Observatory). Using a large database of thermal-IR observations of km-sized asteroids, the average thermal inertia was found to be about four times larger than that of lunar regolith and about ten times larger than the value commonly adopted for regolith-covered main-belt asteroids. These results have potentially important implications for calculations of orbital drift due to the Yarkovsky effect. Furthermore, we have identified a trend of increasing thermal inertia with decreasing asteroid diameter down to ~1km. These results are reported in a paper submitted to Nature in Dec. 2005 (Delbo, dell’Oro, Harris, Mottola, Müller).

In preparation for a Spitzer program, which we plan to propose in 2006, we have enhanced our thermophysical model by incorporating the treatment of mutual shadowing of facets on a globally non-convex shape. This is particularly important for binary asteroid systems, in which one component can eclipse the other. We plan to add the treatment of the mutual heating of surface elements on an arbitrary non-convex shape. Together with the shadowing already implemented, this will enable more realistic modelling of asteroid surfaces taking into account, for example, ridges or boulders as seen on spacecraft imagery of the NEAs Eros and Itokawa.

2.4. Photometric observations of main-belt and near-Earth asteroids (Mottola, Hahn, Harris, Müller)

Photometric studies, carried out as part of international campaigns from several astronomical observatories with the goal of determining the rotational and physical properties of asteroids, have led to the discovery of several binary Near Earth Asteroids (Pravec et al. 2006, Icarus, in press), super-fast monolithic rotators, and tumbling asteroids (Pravec et al. 2005, Icarus, 173, 108). An interesting result from photometry was the discovery of the chaotic rotation state of 2000 WL107, a NEA (Figure 2.3) with a principal rotation period just under 10 minutes. Although very complex, the developed model is capable of accurately reproducing the rotational behavior of the bodies. The fast rotation of this 40 m sized object implies that it is monolithic, and is held together mainly by its tensile strength, rather than gravity, with its surface being exposed rock with an insignificant amount of regolith. Also in the course of this program, methods have been developed for the inversion of disk-integrated photometric data, which allow the modeling of the binary systems and the retrieval of the convex shape of planetary objects. These studies have enabled us to derive the three-dimensional shape of 15 Eunomia (Figure 2.4), one of the largest asteroids in the Main Belt, and to detect the compositional diversity across its surface (Nathues, Mottola et al. 2005).

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In cooperation with Dr. A.K. Sen, Assam University, Silchar, India, we have performed photometric observations of members of the Karin asteroid family, in support of observations with the Spitzer IR Satellite Observatory. The collaboration was established with the aim to use the Himalaya Chandra Telescope, the highest astronomical observatory in the world.

2.5. Asteroid search and follow-up programmes (Hahn)

ODAS – OCA-DLR Asteroid Survey

Fig. 2.3 The chaotic rotation of asteroid 2000 WL107 results in non-periodic lightcurves.

Fig. 2.4 Our photometric studies have enabled us to derive the three-dimensional shape of 15 Eunomia, one of the largest asteroids in the Main Belt, and to detect the compositional diversity across its surface.

Although the observing programme at the Schmidt telescope of the OCA at Calern was cancelled in 1999, the database of astrometric observations (more than 44000 were obtained) is still maintained. These observations are continuously checked at the Minor Planet Center, and used for orbit determination and/or improvements. By the end of 2005 more than 39150 of these observations were linked to known asteroids or comets. The survey resulted in 954 orbits of new discovered asteroids, of which currently 677 are numbered. Further details are available at http://earn.dlr.de/odas/ .

UDAS – Uppsala-DLR Asteroid Survey

Observation at the Kvistaberg Station has continued, resulting in more than 38000 astrometric observations of asteroids and comets by the end of 2005. Details and current observing statistics can be found at http://earn.dlr.de/udas/ .

ADAS – Asiago-DLR Asteroid survey

Due to lack of further funding, this observing programme has been stopped. The available database of astrometric positions and the derived orbital data are maintained and updated via the latest data from the Minor Planet Center. The observing programme resulted in astrometry for more than 3500 asteroids, yielding some 17200 individual positions. 184 new asteroids were discovered of which 45 had been numbered by the end of 2005. Further details can be found at http://dipastro.pd.astro.it/planets/adas/ .

NGSPB project

In cooperation with the Nordic Group for Small Planetary Bodies (NGSPB) the Nordic Optical Telescope (NOT) on La Palma was used to perform astrometric follow-up and recovery observations of NEOs. Our group has been participating in the reduction of these data. Further information can be found at http://www.astro.helsinki.fi/~psr/NEO/not_obs.html .

Databases

Physical properties and discovery circumstances of NEOs are available at http://earn.dlr.de/nea/ . A constantly updated database of all known NEOs (as announced and published by the Minor Planet Center - MPC) is maintained, providing a “home-page” for each asteroid. These pages contain the discovery circumstances, and all published data on the physical properties, including references. It contains an update to the table of physical properties of NEOs published in the Asteroids III book (Univ. Arizona Press), and is further updated on a regular basis.

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http://earn.dlr.de/odas/

http://earn.dlr.de/udas/

http://dipastro.pd.astro.it/planets/adas/

http://www.astro.helsinki.fi/%7Epsr/NEO/not_obs.html

http://earn.dlr.de/nea/

−15 −10 −5 0 5 10 15−15

−10

−5

0

5

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2.6. Orbital evolution studies of Saturn family comets (Hahn)

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X

Y

In cooperation with C.-I. Lagerkvist, Astronomical Observatory, Uppsala, Sweden, a study of the dynamical evolution of comets currently under the influence of Saturn was started. The recently discovered comet P/2004 A1 (LONEOS) was investigated and the interesting fact revealed that this comet is in transition from the influence of the planet Saturn to that of Jupiter (Figure 2.5).

A

B

S

J

Fig. 2.5 The orbits of Jupiter, Saturn and P/2004 A1. Axes units are in astronomical units. A: Position at the epoch of 2005 January 30, shortly after the comet’s discovery. B: Position of closest approach to Saturn in 1992.

3. Comet science

3.1. Hydrodynamical influence on formation of HCN molecules in hot cores (Tornow, Kührt, Motschmann)

HCN, an important prebiotic compound, was detected in a number of comets but not in interstellar ice. To analyse whether it was formed in pre-cometary ice the chemical processes around hot cores have been studied. First, we modelled the chemical composition of hydrostatic hot cores. However, the amount of HCN produced in the gas phase in this case was too low compared to observations.

We modelled the formation of the HCN molecules using the kinetic equations that combine the relevant chemical reactions in the gas phase with the sublimation and accretion activity in the gas and ice phases. Figure 3.1 presents the results for different gas pockets and a standard cosmic ray ionization rate ξCR = 1.3 ⋅10

-17 s-1 in the absence of an initial amount of HCN ejected from the ice phase. The influence of the variation of ξCR and the amount of HCN containing ice is illustrated in the two plots of Figure 3.2 for the inner gas pocket.

We find that HCN abundance in hot cores is strongly influenced by the cosmic ray ionization rate and that N-bearing molecules must be contained in the ice phase to fit HCN line intensity measurements for the studied types of protostars.

Fig. 3.1 Time dependency of the HCN abundance calculated for different gas pockets moving to the hot core centre (solid line: inner gas pocket at 0.0001 pc).

Fig. 3.2 The upper left plot shows the influence of the cosmic ray ionization rate ξCR (solid line ξCR

= 1.3 ⋅10-18

s-1, dotted line ξCR = 1.3 ⋅10

-17

s-1

and dashed line ξCR = 1.3 ⋅10-16 s-1). The upper right plot presents the

influence of different HCN abundances x*0(HCN) ejected from the ice phase (solid line x*0(HCN) = 6.6 ⋅10

-9, dotted line x*0(HCN) = 6.6 ⋅10-8,

dashed line x*0(HCN) = 6.6 ⋅10-7).

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3.2. Modelling the solar wind interaction with weakly outgassing comets by a hybrid model (Motschmann, Kührt)

To support the measurements of the plasma package onboard Rosetta the interaction of the solar wind with weakly outgassing comets has been modeled. In this case the interaction exhibits kinetic features thus hybrid models are an adequate description. Results for 67P/Churyumov-Gerasimenko (CG) were derived (Figure 3.3). Beyond 3.5 AU CG’s activity is extremely weak and the cometary ions behave mainly as test particles. For decreasing heliocentric distances the ion production goes up and thus the reaction of the cometary plasma to the solar wind becomes significant. Plasma structures like cometopause, bow shock and precursors of a magnetic cavity appear. A paper on this subject is to be published in Space Science Reviews (2006).

Fig. 3.3 The hybrid simulation of the interaction of a weakly outgassing comet with the solar wind shows the colour coded magnetic field in nT. The units of the coordinate axes are normalized to ion inertia length.

4. Impact phenomena

4.1. Meteorite ejecta range after terrestrial impacts (de Niem, Kührt, Motschmann)

A sophisticated and robust 2D multi-material hydro code which is stable for up to 800 characteristic times has been used to analyze high-energy Chicxulub-type impacts and impacts into the ocean. The focus of the investigations was the distribution of meteoritic material on the Earth after such events. The impact of a large 10 km diameter asteroid with a velocity of 20 km/s on the continental crust has been modelled for the case of a one-layered target and a crust with a 3 km thick sedimentary cover of limestone on top of a granite basement, appropriate for the Chicxulub crater. The proportion of meteorite material in high-speed ejecta is a function of velocity, time, and consequently, of distance to the crater. Global ballistic distribution of mass comparable to that of the impactor seems to be excluded, at least for the assumed value of the impact velocity. It was

found that the diameter of the transient crater of the K/T impact was 90 km and that the fraction of the impactor material in the ejecta close to the crater is relatively low but increases outwards. Most of the high-speed ballistic ejecta originating during the first 30 seconds would come from the sedimentary layer, not deeper, in the case of a 3 km thick layer of limestone. After an oceanic impact of a 1 km sized stony asteroid (Figure 4.1) 80% of the extraterrestrial material is not mixed with the ocean floor, thus enhancing the signature of meteorite material compared to impacts onto continents. The ejection of meteorite material is a late time effect (timescale of the collapse of the water cavity) and the material is distributed over an area of only several 100 km extent, which is much less than in the case of continental impacts.

Fig. 4.1 Density of oceanic water, 20 seconds after the impact of a 1 km diameter asteroid into 5.5 km deep ocean at (0;0) gives an impression of the extent of the transient water cavity and the mushroom-like chaotic structure containing the debris of the asteroid (dark blue). Units on the coordinate axes are kilometers.

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4.2. Physical limits of solar collectors for the deflection of Earth-threatening asteroids (Kahle, Kührt, Hahn, Knollenberg)

Solar collector lifetime, t

100200300400500600700800900

1000

0.0001 0.0010 0.0100

Velocity change, Δv [m/s]

NEA

size

, DN

EA

[m]

10 min30 min1 h

10 h1 d

5 d10 d

50 d

100 d

10-4 10-3 10-2

5 h

We have investigated the physical limits of a solar collector for orbit deflection of near-Earth asteroids (NEAs) on a collision course with Earth (Kahle et al., Aerospace Science and Technology, in press). Given decades of warning time, a small change of NEA orbital velocity Δv by a few mm/s might suffice to turn a collision into an Earth fly-by and consequently avert a local or even global catastrophe. In principle this can be achieved by means of a large solar collector that focuses sunlight onto the NEA surface in order to vaporize surface material, hence transferring a continuous momentum to the NEA. We have modelled the evaporation process and vapour expansion to investigate the feasibility of the technique. From an analysis of focussing misalignments and collector degradation we found that a considerable operational effort is required to maintain operating conditions. The most important result was that a maximum solar collector lifetime of only 10 to 30 minutes is estimated, based on approximations for the modelling of the evaporation process and vapour expansion. If the focusing mismatch could be controlled adequately by collector shape adjustment, we estimate that a 200 m diameter NEA could be deflected by 0.1 mm/s whereas for a 100 m NEA a Δv of about 1 mm/s is feasible (Figure 4.2). The results apply to a 630 m diameter collector.

Various approaches for collector lifetime prolongation have been studied. The application of removable protecting foils or operation with replaceable secondary mirrors could increase the lifetime by an order of magnitude, albeit at the cost of increased system complexity.

Fig. 4.2 Required collector lifetime as a function of NEA size and NEA orbital velocity change.

5. Contributions to space missions

5.1. Rosetta-MUPUS (Knollenberg, Kührt, Spohn, Schrödter)

During 2005 the MUPUS Ground Reference Model was build-up at the MUPUS/HP3 laboratory and brought into service. The analysis of the NCR’s raised during commissioning and the associated revision of the currently implemented flight software (written by SRC Warsaw) was finalized, and, as a consequence, the decision to completely rewrite the flight software was made. The rewrite was completed to about 75%. MUPUS participated in 2 passive payload checkouts which demonstrated the general health of the hardware but also revealed the possible problem of an apparent loss of sensitivity of the infrared detectors of MUPUS-TM. The actual status of MUPUS was presented to the PHILAE team at the relevant meetings of the Lander Operational Working Group and the Science Working Team.

5.2. Rosetta-Rolis (Mottola, Michaelis)

ROLIS is a miniature CCD imager developed and built at DLR, Berlin. It is located on the balcony of the Rosetta Philae Lander and oriented in a downward-looking direction. From this position ROLIS can observe a region of about 30x30 cm of the nucleus surface located below the lander with a spatial sampling of 0.3 mm/pixel. In order to illuminate the field to be imaged, ROLIS incorporates four independent arrays of light emitting diodes (LEDs) irradiating through the visible and near IR, in spectral bands centered at about 470, 530, 640 and 870 nm, respectively, and with a FWHM of

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about 100 nm. ROLIS will also operate during the descent phase, acquiring images of the landing site and its vicinity shortly before touch-down. During 2005 we participated in several checkout test campaigns, during which the health of the instrument was thoroughly checked. In addition to preparing the instrument for the observations at the comet, such tests give a unique opportunity to monitor the status of Rolis.

5.3. DAWN (Mottola, Jaumann)

Dawn is a NASA Discovery mission whose goal is to achieve an understanding of the conditions and processes at the solar system's earliest epoch. Dawn will investigate the internal structure, density and homogeneity of two complementary protoplanets: 1Ceres and 4 Vesta that have remained intact since their formation, by measuring their mass, shape, volume and spin rate with imagery and gravity. It will record their elemental and mineral compositions and will provide context for the meteorites that have come from these bodies. Dawn will determine their bombardment and tectonic history and uses gravity and spin-state data to limit the size of any metallic core, and infrared and gamma ray spectrometry to search for water-bearing minerals.

The mission uses solar-powered ion engines to deliver the spacecraft first to Vesta, to descend to the high-resolution mapping orbit, and, after a stay of about 7 months, to leave for Ceres, where it stays for 5 months. The spacecraft carries a redundant framing camera, a visible-NIR mapping spectrometer and a gamma ray/neutron spectrometer. DLR contributes to the mission by providing the CCD and front-end electronics of the framing camera. Furthermore, it is represented in the mission Science Team by two co-investigators. During 2005 DLR Berlin has progressed in the construction of the framing camera, by readying two flight units and two flight spares, and by carrying out the respective test programs. Further, DLR has continued in the scientific support of the mission by participating in the activities of the Dawn Science Team.

5.4. Don Quijote: A hazardous asteroid mitigation pre-cursor mission (Harris: Chairman ESA Near-Earth Asteroid Mission Advisory Panel - NEOMAP)

Don Quijote, a European initiative, is conceived as a test of a mitigation pre-cursor mission. In the event of a hazardous asteroid being identified, and assuming the availability of sufficient time before the impact on the Earth, a mission like Don Quijote could be launched to gather the physical information on the threatening asteroid required for the design of an effective mitigation mission. The Don Quijote concept involves two spacecraft launched into separate interplanetary trajectories. One spacecraft, called Hidalgo, will impact on the ~ 500 m diameter target asteroid at a relative speed of at least 10 km/s. The other spacecraft, Sancho, arrives at the same asteroid several months earlier via a different route. A major goal of the mission is to measure the orbital deflection and change in the rotation state of the asteroid as a result of the impact of Hidalgo. Don Quijote would be the first mission to provide direct observations of the effects of a kinetic impact on an asteroid. Changes in the dynamic state of the asteroid will be measured by means of long-term observations from Sancho and ground-based facilities. Imaging by Sancho of the impact process will provide the volume and speeds of ejecta to aid in the determination of the momentum change of the asteroid.

Fig. 5.1 Don Quijote: artist’s impression of Sancho observing the impact of Hidalgo onto the target asteroid.

During 2005 the NEOMAP issued a report entitled “Target Selection for the Don Quijote Mission” which discusses the requirements and preferences for the target asteroids. This work was presented by Harris at the ESA CDF NEO study final presentation, ESA/ESTEC, 8.2.05, and at the Industry Briefing of ESA Activities on Near Earth Objects, ESA/ESTEC, 30.9.05. The latter served as a kick-off meeting for phase-A activities related to Don Quijote. An ESA Invitation to Tender for

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contracts to carry out phase-A studies of the Don Quijote concept was issued shortly before the ESTEC briefing. Two phase-A studies will be carried out during 2006 by two independent consortia of European companies and scientific research institutes. For further information see:

http://www.esa.int/gsp/NEO/objectives/mission_completed.htm.

5.5. Deep impact measurements and simulations (Knollenberg, de Niem, Kührt)

On July 4th the impactor of the NASA mission “Deep Impact” hit the nucleus of comet Tempel-1 at a velocity of 10.2 km s-1 and ejected a prominent cloud of gas and dust. The OSIRIS camera (P.I. H.U. Keller, MPS Lindau) onboard ESA’s Rosetta spacecraft participated in the observational campaign and produced a unique data set comprising of about 2 weeks continuous observations in different gas (OH, CN, OI, Na) and continuum filters. From the observations an impact-induced mass of H2O of about 5000 t was determined as well as a total dust cross section of 330 km2 (assuming an albedo of 0.1), which was moving outward at an average speed of 150-200 m s-1. These results were interpreted as indicative of a dust-to-gas ratio larger than one, and a dust cloud dominated by relatively small particles (several micron radius) which was accelerated further after the impact by gas released in an extended source from ejected icy grains. The observation planning, data reduction and interpretation was supported by members of our Department.

6. Technology projects

6.1. HP3 (Knollenberg, Nadalini)

During 2005 the laboratory build-up was continued and preliminary experiments showing the feasibility of the chosen approach for TEM (the thermal measurements part of HP3) were executed. The main task of TEM is to measure the subsurface temperature profile and the thermal properties of the surrounding medium by use of a tether attached to a mole as carrier. These experiments proved that thermal sensors integrated on a flat Kapton foil (the tether) are well suited for the measurement of low thermal conductivity granular materials. A developed nonlinear inversion technique for the extraction of the thermal conductivity from the self-heating curve of a sensor showed promising results. Compared to the standard linear technique the time of a thermal conductivity measurement could be reduced by a factor of 3-10, a result which is especially important for landers with limited lifetimes in low thermal conductivity environments (e.g. hermean or lunar regolith). Furthermore, the first pieces of specially designed TEM Copper RTD’s were delivered by our subcontractor for the tether manufacturing (Oxford University) and tested in our MUPUS/HP3 laboratory in a temperature range between -150°C and +50°C. The conclusion was that the sensors satisfied the success criteria defined by the HP3 project.

6.2. FIREWATCH (Kührt, Knollenberg, Behnke, Mertens)

Our knowledge of camera development and image processing has been applied to a successful long-term technology transfer project to develop a prototype of an Autonomous Forest Fire Detection System FIREWATCH (Figure 6.1). The aim of the is to detect smoke clouds arising from forest fires up to a distance of 10 km within 8 minutes from outlook towers. The complex system consists of advanced hardware and sophisticated image processing software based on IDL. The operating camera was originally developed for space applications.

In 2005 the 100th system was sold in Germany on the basis of a license agreement with an external company. Trial systems have been tested in France, Chile, Poland and Greece.

Fig. 6.1 Firewatch System

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http://www.esa.int/gsp/NEO/objectives/mission_completed.htm

7. Appendix

7.1. Scientific publications in refereed journals and books (submitted or published in 2005)

Delbó, M., dell’Oro, A., Harris, A. W., Mottola, S., and Mueller, M. 2005. Thermal inertia of near-Earth asteroids and magnitude of the Yarkovsky effect. Nature, submitted.

Hahn, G., Lagerkvist, C.-I., Karlsson, O., Oja, T., Stoss, R. M. 2005. P/2004 A1 (LONEOS) - a comet under transition from Saturn to Jupiter. Astronomische Nachrichten, in press.

Harris, A. W. 2005. The surface properties of small asteroids from thermal-infrared observations. Proc. Asteroids, Comets, Meteors 2005, IAU Symposium No. 229, Cambridge University Press, UK, in press (invited review).

Harris, A. W., Mueller, M., Delbó, M., and Bus, S. J. 2005. The surface properties of small asteroids: Peculiar Betulia—A case study. Icarus, 179, 95 – 108.

Kahle, R., Hahn, G., Kührt, E. 2005. Optimal Deflection of NEOs en Route of Collision with the Earth. Icarus, in press.

Kahle, R., Kührt, E., Hahn, G., Knollenberg, J. 2005. Physical limits of solar collectors in deflecting Earth-threatening asteroids. Aerospace Science and Technology, in press.

Keller, H.U., Jorda, L., Küppers, M., Gutierrez, P., Hviid, Stubbe, F., Knollenberg, J., Lara, L.-M., Sierks, H., Barbieri, C., Lamy, P., Rickman, H., Rodrigo, R. 2005. Deep Impact Observations by OSIRIS Onboard the Rosetta Spacecraft. Science, 310, 281 – 283.

Küppers, M., Bertini, I., Fornasier, S., Gutierrez, P., Hviid, Stubbe, F., Jorda, L., Keller, H.U., Knollenberg, J., Koschny, D., Kramm, R., Lara, L.-M., Sierks, H., Thomas, N., Barbieri, C., Lamy, P., Rickman, H., Rodrigo, R. 2005. Evidence for a Large Dust/Ice Ratio in the Nucleus of Comet 9P/Tempel 1. Nature, 437, 987 – 990.

Motschmann, U., Kührt, E. 2005. Interaction of the solar wind with weak obstacles: hybrid simulations for comets and Mars. Space Science Reviews, in press.

Mueller, M., Harris, A. W., Bus, S. J., Hora, J. L., Kassis, M., and Adams, J. D. 2005. The size and albedo of Rosetta fly-by target 21 Lutetia from new IRTF measurements and thermal modelling. Astronomy and Astrophysics, in press.

Nathues, A., Mottola, S., Kaasalainen, M., Neukum, G. 2005. Spectral Study of the Eunomia Asteroid Family. I. Eunomia. Icarus, 175, 452 – 463.

Pravec, P., Harris, A. W., Scheirich, P., Kušnirák, P., Šarounová, L., Hergenrother, C.W., Mottola, S., Hicks, M., Masi, G., Krugly, Y.N., Shevchenko, V.G., Nolan, M.C., Howell, E.S., Kaasalainen, M., Galád, A., Brown, P., DeGraff, D. R., Lambert, J. V., Cooney Jr., V. R., Foglia, S. 2005. Tumbling asteroids. Icarus, 173, 108 – 131.

Pravec, P., Scheirich, P., Kusnirak, P., Sarounova, L., Mottola, S., Hahn, G., and other 52 authors 2005. Photometric Survey of Binary Near-Earth Asteroids. Icarus, submitted.

Torppa, J., Virtanen, J., Muinonen, K., Laakso, T., Niemelä, J., Näränen, J., Aksnes, K., Dai, Z., Lagerkvist, C.-I., Rickman, H., Hahn, G., Michelsen, R., Grav, T., Jörgensen, U-G. 2005. Physical and dynamical properties of near-Earth objects: First results from Nordic NEON. Icarus, submitted.

Tornow, C., Kührt, E., Motschmann, U. 2005. Pre-Cometary Ice Composition from Hot Core Chemistry. Astrobiology, 5 (5), 632 – 650.

7.2. Scientific publications in other journals and proceedings (published in 2005)

de Niem, D., Motschmann, U., Kührt, E., Knollenberg, J. 2005. Analytical solution for the expansion of the Deep Impact vapor plume. In: Bulletin of the American Astronomical Society, S. 43.30, DPS 2005, 37. Meeting, Cambridge, UK, 2005-09-04 - 2005-09-09, ISSN 0002-7537.

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http://elib.dlr.de/21417/
















De Niem 2005. Hochgeschwindigkeitseinschläge von Asteroiden, Kometen und Meteoriten. Thesis, TU Braunschweig.

Harris, A. W., Benz, W., Fitzsimmons, A., Green, S. F., Michel, P., and Valsecchi, G. B. 2005. Target selection for the Don Quijote mission. NEOMAP report to ESA, 23.2.05.

Harris, A. W., Mueller, M., Delbó, M., and Bus, S. J. 2005. Peculiar Betulia Re-visited: A Near-Earth Asteroid with a Bare-Rock Surface? In: Bulletin of the American Astronomical Society, S. 43.30, DPS 2005, 37. Meeting, Cambridge, UK, 2005-09-04 - 2005-09-09, ISSN 0002-7537.

Helbert, J., Jessberger, E., Benkhoff, J., Arnold, G.,,Banaszkiewicz, M., Bischoff, A., Blecka, M., Calcutt, S., Coangeli, L., Coradini, A., Erard, S., Fonti, S., Killen, R., Knollenberg, J., Kührt, E., Mann, I., Mall, U., Moroz, L., Peter, G., Rataj, M., Robinson, M. S., Spohn, T., Sprague, A., Stöffler, D., Taylor, F., Warrell, J. 2005. In: Lunar and Planetary Science XXXVI, LPI Contribution.

Keller, H. U., Christensen, U., Nathues, A., Sierks, H., Jaumann, R., Mottola, S., Russell, C., DAWN Science Team 2005. Scientific investigation of 4 Vesta and 1 Ceres with the DAWN Framing Cameras. ACM meeting, Buzios, Brazil.

Kahle, R. 2005. Modelle und Methoden zur Abwendung von Kollisionen von Asteroiden und Kometen mit der Erde. Thesis, TU Berlin.

Knollenberg, J., de Niem, D. 2005. Numerical Modelling of the Deep Impact Vapour Plume. 37th Meeting of the Division of Planetary Sciences of the AAS, Cambridge (UK), 2005-09-04 - 2005-09-09.

Kührt, E., Kahle, R., Hahn, G. 2005. Optimal Deflection of NEOs on Collision Course with the Earth. In: Bulletin of the American Astronomical Society, S. 43.30, DPS 2005, 37. Meeting, Cambridge, UK, 2005-09-04 - 2005-09-09, ISSN 0002-7537.

Mueller, M., Harris, A. W., Delbó, M., and the MIRSI Team. 2005. 21 Lutetia and other M-types: Their sizes, albedos, and thermal properties from new IRTF measurements. In: Bulletin of the American Astronomical Society, S. 43.30, DPS 2005, 37. Meeting, Cambridge, UK, 2005-09-04 - 2005-09-09, ISSN 0002-7537.

Mueller, M., Harris, A. W. 2005. Thermische Modellierung erdnaher Asteroiden. Verhandlungen der Deutschen Physikalischen Gesellschaft 4/2005.

Michaelis, H., Jaumann, R., Mottola, S., Oberst, J., Kramm, R., Roll, R., Boenhardt, H., Michalik, H., Neukum, G. 2005. CMOS-APS sensor with TDI for high resolution Planetary Remote Sensing. IEEE workshop on Charge-Coupled Devices and Advanced Image Sensors, Nagano, Japan.

Nathues, A., Mottola, S., Kaasalainen, M., Neukum, G. 2005. Color Variations of 15 Eunomia. IAU Symposium 229, ACM meeting, Buzios, Brazil.

Tornow, C., Kührt, E. and Motschmann, U. 2005. Hydrodynamical influence on the formation of HCN molecules in hot cores. IAU Symposium 231, Monterey, USA.

Torppa, J. and 11 co-authors, including G. Hahn 2005. Spins and shapes of potentially hazardous asteroids. In: Bulletin of the American Astronomical Society, S. 43.30, DPS 2005, 37. Meeting, Cambridge, UK, 2005-09-04 - 2005-09-09, ISSN 0002-7537.

7.3. Minor Planet Circulars/Electronic Circulars

Barbieri, C. and 6 co-authors, including G. Hahn and S. Mottola: Minor Planet Observations [209 Asiago Observatory, Cima Ekar-ADAS], Minor Planet Circular 53632, 2 (2005).



Davidsson, B.; Karlsson, O.; Hahn, G. Comet Observations [049 Uppsala-Kvistaberg], Minor Planet Circular 53409, 3 (2005).

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Gnädig, A. and 10 co-authors, including G. Hahn: Minor Planet Observations [260 Siding Spring-DSS], Minor Planet Circular 54347, 14 (2005).

Karlsson, O., and 5 co-authors, including G. Hahn and S. Mottola: Comet Observations [049 Uppsala-Kvistaberg], Minor Planet Circular 53595, 1 (2005).


Karlsson, O., and 5 co-authors, including G. Hahn and S. Mottola: Comet Observations [A49 Uppsala-Angstrom], Minor Planet Circular 53902, 43 (2005).


Karlsson, O., and 5 co-authors, including G. Hahn and S. Mottola: Comet Observations [A49 Uppsala-Angstrom], Minor Planet Circular 54524, 49 (2005).


Lagerkvist, C.-I., and 5 co-authors, including G. Hahn and S. Mottola: Minor Planet Observations [049 Uppsala-Kvistaberg], Minor Planet Circular 53629, 7 (2005).

Lagerkvist, C.-I., and 6 co-authors, including G. Hahn and S. Mottola: Minor Planet Observations [A49 Uppsala-Angstrom], Minor Planet Circular 53644, 2 (2005).





Maury, A. and 3 co-authors, including G. Hahn: Minor Planet Observations [910 Caussols-ODAS], Minor Planet Circular 53641, 10 (2005).



Muinonen, K, and 7 co-authors, including G. Hahn. Minor Planet Observations [J50 La Palma-NEON], Minor Planet Circular 54984, 10 (2005).

Antonini, P., and 78 co-authors, including G. Hahn and S. Mottola: Observations of Comets, Minor Planet Electronic Circ., 2005-E43 (2005).

Karlsson, O., and 88 co-authors, including G. Hahn and S. Mottola: Observations of Comets, Minor Planet Electronic Circ., 2005-A55 (2005).

Karlsson, O., and 67 co-authors, including G. Hahn and S. Mottola: Observations of Comets, Minor Planet Electronic Circ., 2005-C37 (2005).

Karlsson, O., and 72 co-authors, including G. Hahn and S. Mottola: Observations of Comets, Minor Planet Electronic Circ., 2005-H14 (2005).

Karlsson, O., and 75 co-authors, including G. Hahn and S. Mottola: Observations of Comets, Minor Planet Electronic Circ., 2005-H33 (2005).

Karlsson, O., and 33 co-authors, including G. Hahn and S. Mottola: Comet C/2005 B1 = 2004 FS101 (christensen), Minor Planet Electronic Circ., 2005-J06 (2005).

Karlsson, O., and 88 co-authors, including G. Hahn and S. Mottola: Observations of Comets, Minor Planet Electronic Circ., 2005-K10 (2005).

Tichy, M., and 76 co-authors, including G. Hahn and S. Mottola: Observations of Comets, Minor Planet Electronic Circ., 2005-G34 (2005).

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7.4. Publications in the popular literature and public outreach

A. W. Harris

Review of the book "Mitigation of Hazardous Comets and Asteroids", Cambridge University Press, UK, 2004, in Sterne und Weltraum, 7/2005, pp. 97-98.

Press releases:

ESA press release, N° 41-2005, 26.9.05: ESA selects targets for asteroid-deflecting mission Don Quijote: http://www.esa.int/esaCP/Pr_41_2005_p_EN.html

Consultant for articles on asteroids and planetary phenomena:

The Washington Post, 9.4.05:

(http://www.washingtonpost.com/wp-dyn/articles/A38306-2005Apr8_2.html).

Astronomy Now (UK popular astronomy magazine), July 2005 issue.

Stuttgarter Zeitung, 5.8.05:

(http://www.stuttgarter-zeitung.de/stz/page/detail.php/967611).

Der Tagesspiegel, 19.8.05:

(http://www.tagesspiegel.de/wissen-forschen/index.asp?ran=on&url=http://

archiv.tagesspiegel.de/archiv/19.08.2005/1998366.asp).

Leipziger Volkszeitung, 20/21.8. 2005.

Neue Zürcher Zeitung, 2.11.05:

(http://www.nzz.ch/2005/11/02/ft/articleDA5SW.html).

Invited lectures:

Max-Planck-Institut für Sonnensystemforschung, 1.06.05.

Inst. Raumfahrtsysteme, Univ. Stuttgart, 16.6.05.

Technical University of Dresden, 23.6.05.

Verein Deutscher Ingenieure, Ingolstadt, 27.9.05.

Technical University of Braunschweig, 29.11.05.

Inst. Raumfahrtsysteme, Univ. Stuttgart, 18.12.05.

Technical University of Dresden, 19.12.05.

TV appearances:

“W wie Wissen”, ARD, 12.1.05:

(http://www.daserste.de/wwiewissen/thema_dyn~id,ectyg7c6rtfp5tzi~cm.asp) “Nano”, 3Sat, 28.1.05:

(http://www.3sat.de/3sat.php?http://3sat.de/nano/bstuecke/75264/index.html)

Vox Nachrichten, 28.6.05

Radio interviews:

Die Hayabusa Mission, Raumfahrt Journal, Radio F.R.E.I., Nov., 2005

Hayabusa: Update, Raumfahrt Journal, Radio F.R.E.I., Dec., 2005

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http://www.esa.int/esaCP/Pr_41_2005_p_EN.html

http://www.washingtonpost.com/wp-dyn/articles/A38306-2005Apr8_2.html

http://www.stuttgarter-zeitung.de/stz/page/detail.php/967611

http://www.tagesspiegel.de/wissen-forschen/index.asp?ran=on&url=http://archiv.tagesspiegel.de/archiv/19.08.2005/1998366.asp).

http://www.nzz.ch/2005/11/02/ft/articleDA5SW.html

http://www.daserste.de/wwiewissen/thema_dyn%7Eid,ectyg7c6rtfp5tzi%7Ecm.asp

http://www.3sat.de/3sat.php?http://3sat.de/nano/bstuecke/75264/index.html

E. Kührt

Interview for New Scientist to Impact Hazard, Sept. 2005

(http://www.newscientistspace.com/article.ns?id=mg18725174.900)

Interview Bildzeitung to Deep Impact, July 4, 2005

Interview MDR to Deep Impact, July 3 and July 6, 2005

Interview Radio 1 to Deep Impact, July 10, 2005

Consultant of mission Prometheus in the scientific game Scienox

(http://www.scienox.de/)

Lecturer "Lange Nacht der Wissenschaften", 11.06.2005

M. Müller

TV appearance “Hallo Berlin”, FAB, 4.7.05

7.5. Observing Campaigns 2005

Date Telescope Targets ______________________________________________________________________

(UT)

30 Apr. IRTF NEAs (6611) 1993 VW, 2004 QT24;

M-type asteroid (201) Penelope. 1 May IRTF NEAs (6611) 1993 VW, 2004 QT24;

M-types (216) Kleopatra, (129) Antigone;

8, 9 May IRTF NEAs (6611) 1993 VW, 1999 HF1

M-types (785) Zwetana, (129) Antigone.

11 Nov. IRTF NEA (1862) Apollo; M-type (16) Psyche

14 Nov. IRTF Bad weather, optical data only taken.

19 Nov. IRTF NEAs (1862) Apollo, 2005 JE46;

M-type (135) Hertha

29 Nov. IRTF M-types (16) Psyche, (135) Hertha, (21) Lutetia

2005 Spitzer Space Telescope NEA (54509) 2000 PH5

(total of 0.8 hrs. observing time allocated).

2005-2006 Spitzer Space Telescope 17 Karin cluster main-belt asteroids

(total of 23.5 hrs. observing time allocated).

______________________________________________________________________

Harris and Mueller are responsible for the IRTF and Spitzer observing programmes. The IRTF is the 3.0-m NASA Infrared Telescope on Mauna Kea, Hawaii.

7.6. Space mission responsibilities

A. W. Harris

• Chairman, ESA Near-Earth Object Mission Advisory Panel

• Member of the study team for the CNES/ASI/DLR proposal for a rendezvous/lander mission to a near-Earth asteroid

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http://www.newscientistspace.com/article.ns?id=mg18725174.900

http://www.scienox.de/

J. Knollenberg

• Rosetta: Project Manager MUPUS

• Co-Investigator ROSETTA-experiments: MUPUS, OSIRIS

• Co-Investigator BepiColombo-Mertis

E. Kührt

• Co-Investigator ROSETTA-experiments: MUPUS, OSIRIS, RPC, VIRTIS and ROMA

• Team member framing camera DAWN

• Co-Investigator BepiColombo-Mertis

S. Mottola

• PI of the ROLIS experiment on the Lander of the ESA Rosetta mission

• Co-I of the NASA DAWN mission

• Co-I of the VIRTIS experiment on the ESA Rosetta mission

• Associated Scientist of the OSIRIS experiment on the ESA Rosetta mission

7.7. Other events and activities

A. W. Harris

• Presentation of the ESA NEO Mission Advisory Panel Report “Target Selection for the DonQuijote Mission” at the ESA CDF NEO study final presentation, ESTEC, Noordwijk, 8.2.05.

• Speaker at the Presentation to Industry of ESA Activities on Near Earth Objects, ESA/ESTEC, Noordwijk, 30.9.05.

• Member, Scientific Advisory Board, Asteroids, Comets, Meteors Conference, Brazil, 2005.

• Member, Scientific Advisory Board, Symposium on Near-Earth Objects, IAU XXVI General Assembly, Prague, 2006.

• Invited speaker: Asteroids, Comets, Meteors Conference, Brazil, 2005.

• Referee for the journals Advances in Space Research, The Aeronautical Journal, and the Proceedings of the The First Hayabusa Symposium, 2004, Sagamihara, Japan.

• Member, Organizing Committee of Commission 15, "Physical Studies of Asteroids and Comets", of the International Astronomical Union.

E. Kührt

• Coordinator of the network of Leopoldina Academy fellowship holders.

• Invited lecture, Rosetta Philae workshop, Teistungen, March 2005.

• Invited lecture, Forest Fire workshop, Marseille, Nov. 2005.

S. Mottola

• Referee in 2005 of 2 articles for Icarus and 1 article for Earth, Moon and Planets.

7.8. Funding

• Programmatics at DLR (projects: Rosetta, Dawn, Asteroids and Comets)

• ESA (project HP3)

• ESOC (contract 15836/01/D/HK(SC))

• Industrial funding for AWFS technology project

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DEPARTMENT “ASTEROIDS COMETS” IX. Annual Report 2005...2.5 Asteroid search and follow-up...

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