The Solar System at ~10 mas perspectives for a Fresnel imager Paolo Tanga Marco Delbò Laboratoire...
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![Page 1: The Solar System at ~10 mas perspectives for a Fresnel imager Paolo Tanga Marco Delbò Laboratoire Cassiopée, OCA.](https://reader035.fdocuments.us/reader035/viewer/2022062518/56649e4d5503460f94b42ee3/html5/thumbnails/1.jpg)
The Solar System at The Solar System at ~10 mas ~10 mas
perspectives for a Fresnel perspectives for a Fresnel
imagerimager Paolo TangaPaolo Tanga
Marco DelbòMarco Delbò
Laboratoire Cassiopée, OCALaboratoire Cassiopée, OCA
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Observational challengesObservational challenges Hi-res atmospheric activity & aurorae (UV) on Hi-res atmospheric activity & aurorae (UV) on
Jupiter, SaturnJupiter, Saturn Atmospheric activity on the remote planetsAtmospheric activity on the remote planets Evolution of fine structures in Saturn’s ringsEvolution of fine structures in Saturn’s rings …… Trans-Neptunian Object population:Trans-Neptunian Object population:
InventoryInventory Size (albedo)Size (albedo) Anomalous orbitsAnomalous orbits
Asteroids:Asteroids: Inventory at small sizesInventory at small sizes Internal structure (mass, size, shape)Internal structure (mass, size, shape) Cometary activityCometary activity
CometsComets Evolution of chemicals after sublimationEvolution of chemicals after sublimation
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Giant planetsGiant planets UV features:UV features:
AuroraeAurorae Upper atmospheric Upper atmospheric
features (40-100 mb)features (40-100 mb)
InterestInterest Connection to Connection to
magnetospheremagnetosphere Coupling to other Coupling to other
wavelengthswavelengths Our nearby Our nearby
prototype of prototype of extrasolar planets!extrasolar planets!
HST, H2 emission (160 nm)
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The importance of The importance of asteroids…asteroids…
The great issues:The great issues:
Origin: collisional life, related physics
Dynamical processes: transport, mixing in the primitive nebula, origin of meteorites
Impact risks and mitigation strategy
The problem…The problem…Very limited knowledge of basic properties: density, porosity… Spectral types and connection to composition Shapes, satellites Size distribution
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Itokawa as seen by Itokawa as seen by HayabusaHayabusaIs this a cohesionless « gravitational aggregate »?Is this a cohesionless « gravitational aggregate »?
540 m
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How much is/will be knownHow much is/will be known
PropertyProperty todaytoday after Gaiaafter Gaiashapes, poles 100 ~100,000
rotation periods 1000 10,000
satellites ~ 20 (MBA) ? New
constraints!
surface properties ~ 1000 ~200,000
astrometry ~ 0"5 0"005
masses, < 50% ~ 50 150
size / albedos ~2000 3000
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Angular size as a function of distance for objects of 10 and 100 km. The two « p » curves represent the limit size at V=20 (at opposition) for two extreme albedo values.
Jup
iter
Nep
tun
e
Mar
s
Ceres
~200 asteroids
1 x 106 (?)1 x 106 (?)
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Areas open to a Fresnel Areas open to a Fresnel imagerimager
Size inventory/improvement 10-100 Size inventory/improvement 10-100 kmkm
Macroscopic shapes 10-100 kmMacroscopic shapes 10-100 km Cometary activity (OH at 308 nm)Cometary activity (OH at 308 nm)
Binary asteroidsBinary asteroids DiscoveryDiscovery OrbitsOrbits
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Binary asteroidsBinary asteroids Importance:Importance:
Linked to the collisional physics Linked to the collisional physics past history of the belt past history of the belt Period + separation Period + separation mass mass If size is known If size is known density (internal properties) density (internal properties)
Properties:Properties: Wide range of separations Wide range of separations
and size ratios!and size ratios! 16% of objects at D<30 km?16% of objects at D<30 km?
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Binary asteroids – the Fresnel Binary asteroids – the Fresnel imager domainimager domain
radar/lightcurves Imaging (AO)
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How many asteroids at How many asteroids at V=20 ?V=20 ?
Evolution of the number of entries H < HEvolution of the number of entries H < Hlimlim
old files retrieved by D. Hestroffer in the IMCCE archivesold files retrieved by D. Hestroffer in the IMCCE archives
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45°
Geometric observability of Geometric observability of orbitsorbits
L2
Sun
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Velocity distributionVelocity distribution
simulation on 5,000 objectssimulation on 5,000 objectsmain-belt, NEOsmain-belt, NEOs
Possible problems related Possible problems related to motionto motion
~ 12 mas/s
mas/s
%
-40 -30 -20 -10 0 10 20 30 400
1
2
3
4
5
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Possible strategies:Possible strategies:
Priority given to Solar System objectsPriority given to Solar System objects Exceptional events (comets, storms on Exceptional events (comets, storms on
the main planets…)the main planets…) Specific long-term monitoring programsSpecific long-term monitoring programs
« Opportunity » targets« Opportunity » targets ~50 asteroids V<20 in 1 sq. degree~50 asteroids V<20 in 1 sq. degree Few requirements on pointingFew requirements on pointing
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ConclusionsConclusions Asteroids offer a wide variety of Asteroids offer a wide variety of
targetstargets Binary objectsBinary objects Cometary activityCometary activity
Giant planetsGiant planets Interesting features at all Interesting features at all
wavelengthswavelengths Can help in modeling extrasolar Can help in modeling extrasolar
planet observationsplanet observations
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Configuration space period-diameterConfiguration space period-diameter no very fast rotator due to centrifugal forceno very fast rotator due to centrifugal force lack of global cohesionlack of global cohesion
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The occultation revivalThe occultation revival TodayToday poor predictability for objects <50 kmpoor predictability for objects <50 km bright Hipparcos/Tycho stars favouredbright Hipparcos/Tycho stars favoured ~0.1 events/objects/year~0.1 events/objects/year Current practical limit: 100 km at 10% Current practical limit: 100 km at 10%
accuracyaccuracy
After Gaia (100 X orbit improvement):After Gaia (100 X orbit improvement): Uncertainty smaller than the asteroid at Uncertainty smaller than the asteroid at
>20 km>20 km 1-m automated telescope(s):1-m automated telescope(s):
Single site: 20-40 events/yr for an object Single site: 20-40 events/yr for an object of ~20 kmof ~20 km Network: completeness of diameters Network: completeness of diameters > 20 km in a few yr> 20 km in a few yr
Projected shape knownProjected shape known
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Light curvesLight curves Asteroid’s magnitude function of:Asteroid’s magnitude function of:
shape, rotation period, direction of shape, rotation period, direction of
spin axisspin axis
Direct problem: Direct problem: model of light curves for different model of light curves for different
shapes and rotationshapes and rotation
Inverse problem: Inverse problem: find the rotation parameters from find the rotation parameters from
photometric dataphotometric data
strongly non linearstrongly non linear
not well conditioned if period not well conditioned if period
unknownunknown
Animation: M. Delbo