Planets Building Blocks#
Introduction
Intro paragraph
Notes
To Do
Think about coherent plan
Implement
Colaboration
Star formation is not my expertise so if you want to help, feel free to comment the contribution you could make
Note
Speak about snowline
Grain shape, grain properties SED !
ISM Dust#
Note
Link to BT Draine website with Dust properties
[Hensley and Draine, 2023]: Unified model Dust+PAH
From molecular clouds to PPD#
[Hirashita and Li, 2013]: Numerical modelling (formation of ÎĽm-sized grains in dense cores of molecular clouds), results: coreshine (mid-IR emission due to scattering from ÎĽm-sized grains in dense cores) must come from long-lived entities rather than dynamically transient objects (based on free-fall time for typical hydrogen densities around 105 cm-3)
Water in the ISM#
Review: [Dishoeck et al., 2011]: observations (80 sources), molecules: H2O/H218O/CO/13CO/C18O/OH+/H2O+/dust continuum, lack of water in cold gas, strong water emission from shocks, UV radiational heating of gas in outflow, H2O generally not the dominant coolant in warm dense gas around protostars.
Note
To (print) read !!
Dust observation in PPD#
[Min et al., 2012]:modelling (understand effects of dust particle structure/size-dependent grain settling/instrumental properties), different dust particle models and disk structures, particle size and shape have strong effect on brightness/detectability of disk, realistic models give very different results than homogeneous sphere model, need to also simulate telescope effects before interpretation of results
Interstellar Dust#
Warning
Dustpy - Python package to model dust in PPD Check in more detail
Grain shape#
[Mutschke et al., 2009]: Lab and calculated dust extinction spectra often not in good agreement, modelling with distribution of form factors (DFF) to match lab results -> later grain shapes can be derived from model fits independently.
Ice#
Is the ice amorphous, crystaline, something else ...
[Ehrenfreund et al., 2003]: cold ISM: dust particles covered in ultrathin icy layers, drive rich chemistry in star-forming regions, polar caps of terrestrial planets and outer solar system satellites covered in ice, earth atmosphere, weather etc., are lab ices good analogues?, bulk structure, surface catalytic properties, ice + dust experiments (1 + 0 g) + models, proposed experiments for ISS.
Processing#
![../../_images/Dust-grains-ice-process.png](../../_images/Dust-grains-ice-process.png)
Fig. 33 [Boogert et al., 2015]#
Surface#
[Fraser et al., 2002]: experiment designed to study surface ice chemistry in the lab (solid-gas interactions), 7 – 500 K, pressures 103 larger than in protoplanetary disks, gas composition H2 & CO, mass-spec/RAIRS/quartz crystal microbalance all in one chamber.
Crystaline#
[Schegerer and Wolf, 2010]: spectroscopic detection of crystalline water ice in young stellar object, predominantly small grains (0.1 – 0.3 μm), few large grains, evidence for grain growth, crystallinity increases in upper layers of circumstellar disk, only amorphous grains exist in bipolar envelope, crystallization close to disk atmosphere, where water ice is shielded from hard radiation.
Ferroelectric Ice#
Note
Definition + link toward physic course on ferroelectrecity
[Fukazawa et al., 2015]: Characterisation (neutron diffraction, D2O with impurities (KOD, NaOD, LiOD, DCl, ND3, Ca(OD)2), atmospheric pressure) of “ferroelectric ice” (= ice XI, can generate giant electric fields), stable @ 57 – 74 K, can be important for planet formation, results: ferroelectric ice forms with dopants that produce L-defects (KOD, NaOD), no ferroelectricity observed for samples with D-defect.
[Iedema et al., 1998]: Characterisation experiments (partially proton-ordered ice Ic (vapour deposited on Pt(111) substrate), 40 – 150 K, Kelvin probe), result: slight preference for O aiming away from surface, 0.2 % net dipole per H2O molecule (@ 40 K) = -3 mV/monolayer, decreases with deposition T (exp(-T/27K)), when ice changes from amorphous to crystalline (130, 140, 150 K), dielectric properties become active, vapour-deposited ice in space may develop large electric fields.
Dust Light Interaction#
Processing#
Up to protostar - [Ă–berg et al., 2011]
Dust evolution#
Grain-Grain collisions#
foundation for theoratical models of dust evolution in disks
cf next chapters
Interplanetary Dust Particles#
How can we catch those grains ? Well this has been achieved by the Stardust mission that we will describe below
StarDust mission#
First sample return mission, launched by NASA in 1999
StarDust website
Properties#
Chemical evolution#
Comets#
[Weidenschilling, 1997]: Modelling (numerical simulation (growth of cometesimals), beginning with uniform mixture of microscopic grains in nebular gas, coagulation, settling => small aggregates in central plane, gas drag, radial motion, velocity dispersion prevents gravitational instability to grow bodies > 10 m), results: size-distribution of cometesimals shows narrow peak @ 10’s – 100’s m, resulting bodies have low mechanical strength, macroscopic voids, small scale porosity.
Cometesimals#
Cometary Dust#
Review: Arxiv link
Ice in space#
[Gundlach et al., 2011]: Characterisation of ice aggregates, built of μm-sized H2O ice particles (formed by spraying water into liquid N2), porosity of aggregates depends on production method: 0.11 – 0.72 volume filing factor, critical rolling friction force ice: 114.8 x 10-10 N (silica: 12.1 x 10-10 N), adhesive bonding for ice stronger than for SiO2, specific surface energy ice: 0.19 J/m2
Circumplanetary Disk#
Disks that formed around planets and from which Icy Satellites forms
Composition#
[Oberg et al., 2023] : Model (code ProDiMo)
Note
Check the model
Kuiper Belt Objects#
Formation from relatively unaltered material, may be at the origin of comets