Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: Maria Teresa Capria
MINOR BODIESMINOR BODIESBack in time to the Origin of Solar SystemBack in time to the Origin of Solar System
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: Maria Teresa Capria
Why do we study Why do we study cometscometsCometary material has been submitted to
the lowest level of processing: it contains information on the physical and chemical processings prevailing during the early stages of the Solar System
Comets probably played an important role in the evolution of Earth, bringing water and organic matter
Physical and chemical processes taking place in the coma are still poorly understood
We have only few images of the a nucleus surface
The interior of the nucleus is completely unknown
And then we have now Kuiper Belt Objects completing the inventory of Solar System bodies…
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: Maria Teresa Capria
Why do we study asteroidsWhy do we study asteroids
There are surprising differences between them:
Asteroids range from small rocky fragments to big differentiated bodies like 4 Vesta; they can be binary and can have satellites…
There is a continuous change in composition going from the inner to the outer Solar System.
We have samples of their matter (meteorites), but the link between some types of meteorites and the bodies from which they originated (parent body) is not clear.
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: Maria Teresa Capria
How do we study minor bodiesHow do we study minor bodies
From all the points of view…
Theoretical Observational Space mission participation
Comet nucleus modelingStatistical analysis (classification)
Mineralogical characterization of asteroids through near infrared spectroscopyComa composition through high resolution spectroscopy in the visible range Rosetta to comet
67P/Churyumov-Gerasimenko…DAWN to 4 Vesta …
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: Maria Teresa Capria
Theoretical models of the thermal evolution and differentiation of a nucleus must be used to link coma observations with real nuclei characteristics and properties. At the IASF a nucleus model has been developed; many real comets have been simulated, as well as Kuiper Belt Objects.We participated in an international team, located at ISSI in Bern, that defined a standard model.Our model is also used as a help in the planning of the instrument operations of VIRTIS, our imaging spectrometer on Rosetta mission.
The theoretical point of view: nucleus The theoretical point of view: nucleus modelingmodeling
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: Maria Teresa Capria
Space missions: theSpace missions: the Rosetta journeyRosetta journeyThe ESA cornerstone mission Rosetta is set to a rendezvous with Comet 67P/Churyumov-Gerasimenko, orbiting around it and making observations as it journeys towards the Sun. A lander will be deposited on the surface of the comet.The mission is aimed to study the origin of comets, the relationship between cometary and interstellar material and its implications with regard to the origin of the Solar System. It carries instruments for remote sensing, composition analysis, nucleus large-scale structure, dust flux and mass distribution, comet plasma environment and solar wind interaction, radio science.
Launch date: 26 Feb 2004Perihelion passage: 2015
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: Maria Teresa Capria
VIRTIS (Visible and Infrared Thermal Imaging Spectrometer) combines a double capability: moderate-resolution visible and infrared imaging in the 0.25-5 m range (VIRTIS-M channel) high-resolution spectroscopy in the 2-5 m range (VIRTIS-H channel).VIRTIS maps and studies the nature of the solids and the temperature on the surface of the nucleus. Also identifies comet gases, characterises the physical conditions of the coma and helps to identify the best landing sites.
Radiator
Baseplate (S/C Interface)
VIRTIS-HVIRTIS-M
Cold box
VIRTIS on ROSETTAVIRTIS on ROSETTA
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: Maria Teresa Capria
INAF IASF, IFSI Padua, Lecce and
Perugia Universities Capodimonte and
Arcetri Observatories
VIRTIS on ROSETTAVIRTIS on ROSETTA
Spectral resolutionSpectral sampling
100-380 70-360 1300-3000 1.89nm 9.44nm 0.6nm
-M visible –M IR -H
VIRTIS international consortium
The instrument has been successfully integrated and tested and is ready for the launch
P.I. Angioletta Coradini
Paris-Meudon Observatory
IAS, Orsay
DLR Berlin Galileo Avionics, Florence (prime contractor)
TecnoSystem, NeaplesLaben, MilanKayser Trade, Munich
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: Maria Teresa Capria
La missione Dawn: •cos’e’ •Scienza
Space missions: theSpace missions: the DAWN journeyDAWN journey
The NASA Discovery mission DAWN will be launched in 2006 and will orbit Vesta for one year, in 2010; it brings a framing camera, a mapping spectrometer and a gamma ray/neutron spectrometer. The spectrometer is VIR, a re-build (a twin) of the mapper channel of VIRTIS. VIRTIS-M
VIR
A. Coradini is mission Co.I. and instrument P.I.
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: Maria Teresa Capria
Vesta is:one of only four bodies for which we have samples (HED meteorites).perhaps the only surviving member of the class of planetesimals that accreted to form the terrestrial planets.Vesta…differentiated 4.5 billion years ago under conditions distinct from Earth, Moon, Marshas a heterogeneous surface of various crustal rocks and possibly excavated mantle rocks.
Why Vesta?Why Vesta?
Thin section of HED meteorite
On Vesta we could:better constrain planet formation by understanding their protoplanetary building blocks test our ideas about the thermal, physical, chemical and mineralogical evolution of planetesimals, presently crafted from the incompletely sampled rubble of disrupted asteroids (meteorites)
Vesta, Space Telescope
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