ASTEROIDS, COMETS, AND TRANS-NEPTUNIAN OBJECTS:
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1 ASTEROIDS, COMETS, AND TRANS-NEPTUNIAN OBJECTS: SMALL BODIES IN THE SOLAR SYSTEM Rosemary E. Pike ASIAA TIARA Summer School 2018 On the Origins of the Solar System
2 SMALL BODIES IN THE SOLAR SYSTEM Formation in a Disk Evolved ~4Gyr Small bodies Today Size Distribution Composition Dynamics Shape What do we see today and what can we learn about Solar System formation from small body characteristics?
3 SMALL BODIES
4 Asteroids e.g. Ceres SMALL BODIES
5 SMALL BODIES Trans-Neptunian Objects e.g. Pluto
6 SMALL BODIES Comets e.g. C/67P
7 SMALL BODY COMPOSITION Simple Picture: Small objects condense out of the protoplanetary disk, composition depends on distance from the sun (ice lines) Actually more complex: Disk has temperature gradients in 3D, there is radial drift of gas and particles, effects of planets, mass-dependent long-term stability, etc. Morbidelli et al. 2016
8 SMALL BODY COMPOSITION: ASTEROIDS Many astroid surface types We know a lot about asteroid chemical composition from Meteorite falls, but matching meteorites to asteroids has been challenging Differentiated and Undifferentiated
9 SMALL BODY COMPOSITION: ASTEROIDS Many astroid surface types We know a lot about asteroid chemical composition from Meteorite falls, but matching meteorites to asteroids has been challenging Differentiated and Undifferentiated wikipedia
10 SMALL BODY COMPOSITION: ASTEROIDS Many astroid surface types We know a lot about asteroid chemical composition from Meteorite falls, but matching meteorites to asteroids has been challenging Differentiated and Undifferentiated wikipedia
11 SMALL BODY COMPOSITION: ASTEROIDS Asteroids can be classified by surface reflectivity With high quality spectroscopy, Asteroid and Meteorite reflectance have been linked This connects the measured lab composition of meteorites to the orbital distribution of Asteroids on sky
12 SMALL BODY COMPOSITION: ASTEROIDS Asteroid surface type distribution on sky.
13 SMALL BODY COMPOSITION: COMETS AND TNOS Large TNOs have volatile surface ices: Water, Methane, Nitrogen, CO, Ammonia Volatile retention depends on surface gravity and distance Small TNOs typically show only a (varying) red slope in the visible (similar to Tholins), with the exception of the Haumea family.
14 SMALL BODY COMPOSITION: COMETS AND TNOS Small TNOs can only be studied using photometry, they are too faint for spectroscopy. They can be classified into different surface types based on optical-nir colors. One classification example is g, r, and z band colors: These colors separate dynamically excited TNOs from the cold classical objects in the Kuiper belt. Pike et al Open questions: How many TNO surface types exist? What is the surface composition? Silicates and ice?
15 Meech et al SMALL BODY COMPOSITION: OORT CLOUD OBJECTS Very little is known about Oort cloud objects in situ Some Oort cloud objects are measured as comets, Manx (tailless comets) give the best view of the objects surfaces The majority resemble TNOs (Dtype), but 1 C-Type Manx comet has been identified
16 SMALL BODY DYNAMICS Orbit distribution Behavior over time: stable or evolving? Implications for primordial orbits Inner Solar System Minor Planet Center Outer Solar System
17 SMALL BODY DYNAMICS: ASTEROIDS Chamberlain/JPL/Caltech
18 SMALL BODY DYNAMICS: ASTEROIDS Parker et al Combining Color and orbital information is the key to determining family membership in the asteroid belt!
19 SMALL BODY DYNAMICS: ASTEROIDS Families! Parker et al Combining Color and orbital information is the key to determining family membership in the asteroid belt!
20 Alex Parker:
21 SMALL BODY DYNAMICS: COMETS AND TNOS
22 SMALL BODY DYNAMICS: OORT CLOUD OBJECTS Galactic Tides raise the inclinations and perihelia of objects with a<1000 AU Initial inclination on ecliptic (63 degrees) After 5 Gyr This results in the spherical cloud shape Galactic Tides and stellar flybys result in the delivery of Oort cloud objects into the solar system Galactic tides and stellar flybys can also result in objects lost to interstellar space. Higuchi et al. 2007
23 SHAPES OF SMALL BODIES Shapes can tell us about formation and evolution Large bodies are round (and possibly differentiated) Small bodies may be collisional remnants, or partially re-assembled post-collision Greyscale photograph of Comet 67P Churyumov Gerasimenko taken by the Rosetta spacecraft Objects may be binary or contact binaries
24 SHAPES OF ASTEROIDS Shapes Measured by direct imagining, radar, occultations, and light curve analysis Surfaces typically cratered Many are likely collisional remnants The large fraction of asteroids in families is consistent with collisional remnants Adapted from the picture by Emily Lakdawalla (Planetary Society)
25 Surface properties (mountains, surface texture) measurable by phase curves New Horizons, NASA SHAPES OF TNOS Measured by direct imaging, occultation, light curve analysis (spacecraft) Some Centaurs have been found to have jets and/ or rings Large objects are round, small TNOs are typically not round The majority of objects surface structure can only be inferred by light curve measurement (changing brightness over time)
26 BINARY SMALL BODIES TNOs: The binary fraction of TNOs is high Estimates are that the vast majority of cold classical TNOs (~100%) must have formed as binaries Many contact binaries among the TNOs, estimated ~40% in the Plutinos Thirouin & Sheppard 2018 One known Jupiter trojan binary, 6-10% estimated to be contact binaries Small main belt asteroids ~15% binary Constraints from Binary Objects: Formation and Stability! Fraser et al. 2017
27 SMALL BODY SIZE DISTRIBUTIONS How we measure the Mass in the Belt!
28 SMALL BODY SIZE DISTRIBUTIONS: ASTEROIDS The asteroid population is significantly collisional evolved The family members are depleted of large objects and enhanced in small objects as expected D < 70km: primordial slope was much shallower than the current one The asteroids identified as non-family members here are likely relatively unmodified Tsirvoulis et al. 2017
29 SMALL BODY SIZE DISTRIBUTIONS: TNOS The largest TNOs have a steeper slope (Dwarf Planets) Above ~100km diameter, TNOs have a steep slope (alpha ~0.8) The size distribution transitions at H~8.5. Additional transitions in the size distribution are measured in the New Horizons cratering record
30 SMALL BODY SIZE DISTRIBUTIONS: OORT CLOUD OBJECTS LPCs with H<~12 are extremely rare, so they are likely less active/disrupted Larger LPCs have a size distribution slope of alpha= (shallow) Fernandez & Sousa 2012
31 OBSERVING THE SOLAR SYSTEM In the Solar System, we are sensitive to small bodies and relatively insensitive to dust Small body discovery searches have progressed from small scale searches to major campaigns The main belt asteroid sample is essentially complete to H=14.8 TNO surveys have entered the large-scale characterized discovery phase in the last ~15 years. TNO distribution is well measured to H~9. - km - Minor Planet Center
32 ASTEROID DISCOVERIES Scott Manley
33 TNO DISCOVERIES Video: Michele Bannister, OSSOS
34 PUTTING IT ALL TOGETHER: WHAT DOES IT MEAN? Solar system had a violent history The vast majority of small bodies have been modified by surface processing, orbital disruption, and scattering Disentangling the formation location of different small bodies is extremely challenging However, large samples of asteroids and scale surveys of TNOs and provide a sample which can be compared to theoretical models and simulations of the solar system s initial conditions and evolution
35 THE GRAND TACK Constraints: Size of Mars, Asteroid belt structure Occurs during the Gas phase of the disk Jupiter, then Saturn, move inward in Type 2 migration When Jupiter and Saturn become locked in 3:2 MMR, drift outward instead of inward
36 THE GRAND TACK Philip Carter et al. 2015
37 THE NICE MODEL Jupiter Saturn Uranus Neptune Levison et. al 2004
38 PLANETARY MIGRATION SCULPTS THE SMALL BODY POPULATION DISTRIBUTIONS Different migration specifics result in different planetesimal signatures High-eccentricity Neptune which circularizes after/while moving outward produces significant resonant drop-off populations and asymmetric resonance occupation Grainy migration results in reduced resonance population sizes and sunward drop-off of particles Smooth migration is more efficient at resonance trapping and generating low-eccentricity TNOs Fast migration (faster than Kozai cycling timescales) results in the production of few low-eccentricity particles
39 SIGNATURES OF MIGRATION The Astronomical Journal, 152:133 (15pp), 2016 November Kaib & Sheppard Kaib & Sheppard 2016 Figure 2. Plots of our particles final eccentricities vs. semimajor axes for our (A) SmS, (B) SmF, (C) GS, and (D) GF simulations. Red dashed lines mark q = 30 au and q = 40 au orbits. Blue dotted lines mark major MMRs with Neptune.
40 SIGNATURES OF MIGRATION Figure 6. ± ( ) ( ) Kaib & Sheppard 2016
41 CONSTRAINTS ON PLANETESIMAL FORMATION High binary formation fraction for TNOs Binary preservation fraction (limits collisional grinding and violent scattering events): up to 100% of cold classical TNOs with H<6 may be binary (Noll et al. 2014), ~30% or larger for smaller objects Dynamically excited TNOs are estimated to contain ~10% binary pairs One identified TNO collisional family: little collisional evolution occurred in their current locations
42 CONSTRAINTS ON PLANETESIMAL EVOLUTION The Grand Tack, the Nice Model, STIP instability, Grand Smack, Must preserve the terrestrial planets Produce high-density Mercury/Inner edge of disk Low-mass Mars Produce the proper density in the Asteroid belt region Limited collisional evolution for TNOs Replicate the detailed structure of the Asteroid and Kuiper belts
43 FUTURE PROSPECTS: DISCOVERY & OBSERVATION New Horizons flyby of a cold classical TNO! LSST: full sky TNO and asteroid discovery survey TAOS2: Serendipitous Occultation survey to discover small TNOs passing in front of stars Lucy: Spacecraft Mission to Neptunian Trojans JWST: NIR characterization of small body surfaces
44 ASTEROIDS, COMETS, AND TRANS-NEPTUNIAN OBJECTS: SMALL BODIES IN THE SOLAR SYSTEM Rosemary E. Pike ASIAA TIARA Summer School 2018 On the Origins of the Solar System
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