Debris Disks and the Formation and Evolution of Planetary Systems… Christine Chen October 14, 2010

Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations

Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations

Our Solar System Terrestrial Planets Asteroid Belt Jovian Planets Kuiper Belt Ice Dwarf Planets Oort Cloud

The Zodiacal Light Mdust = 21020 g = 10-10 Mplanets = 10-4 MMAB LIR(dust) = 100 LIR(planets)

Asteroid Families Distribution of the proper sine of inclination vs. semi-major axis for the first 1500 numbered asteroids. The Hirayama families Themis (T), Eos (E), and Koronis (K) are marked. Kirkwood gaps are visible. The detached Phocaea region is at upper left. Chapman et al. (1989) In 1918 Hirayama discovered concentrations of asteroids in a-e-i space (osculatory orbital semi-major axis, eccentricity and inclination) he named “families”. It is widely believed that these families resulted from the break up of larger parent bodies.

Origin of Dust Bands in the Zodiacal Light The a, b, g dust bands in the Zodiacal Light are believed to have been generated by mutual collisions within the Themis, Koronis, and Eos families. Other dust bands are not found in association with other major asteroid families with the possible exception of the Io family. The Koronis family has a greater dust population than the larger Themis family. The majority of dust bands were probably produced by large random collisions among individual asteroids.

The Kuiper Belt More than one thousand km-sized KBOs have now been discovered. Although, no dusty disk has yet been detected, one is believed to exist.

Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations

The Vega Phenomenon Routine calibration observations of Vega revealed 60 and 100 μm fluxes 10 times brighter than expected from the stellar photosphere alone. Subsequent coronagraphic images of b Pic revealed an edge-on disk which extends beyond 1000 AU in radius. Infrared excess is well described by thermal emission from grains. Backman & Paresce 1993

A Circumstellar Disk Around  Pictoris! Spectral Type: A5V Distance: 19.3 pc Tdust: 85 K LIR/L*: 3  10-3 Mdust: 0.094 M Rdust: 1400 AU Inclination: 2-4º Age: 20 ± 10 Myr Mouillet et al. (1997)

Radiation Effects Poynting-Robertson Drag Dust particles slowly spiral into the orbit center due to the Poynting-Robertson effect. The lifetime of grains in a circular orbit is given by (Burns et al. 1979). Radiation Pressure If Frad > Fgrav (or  > 1), then small grain will be radiatively driven from the system Artymowicz (1988)

Solar Wind Drag The solar wind is a stream of protons, electrons, and heavier ions that are produced in the solar corona and stream off the sun at 400 km/sec Typically, Fsw << Fgrav; therefore, stellar wind does not effectively drive dust out of the system radially. However, they do produce a drag force completely analogous to the Poynting-Robertson effect (Plavchan et al. 2005)

Debris Disks are dusty disks around main sequence stars Debris Disks are dusty disks around main sequence stars. Unseen planets are believed to gravitationally perturb asteroids and comets, causing them to collide with one another generating fine dust grains. Astronomical telescopes detect the starlight scattered by these dust grains and the heat emitted from the grains.

Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations

A Possible Planet in the b Pic Disk Observed Dwarp = 70 AU 48 MJup brown dwarf at <3 AU Or 17.4 MJup – 0.17 MJup planet at 5 – 150 AU STIS/CCD coronagraphic images of the b Pic disk. The half-width of the occulted region is 15 AU. At the top is the disk at a logarithmic stretch. At bottom is the disk normalized to the maximum flux, with the vertical scale expanded by a factor of 4 (Heap et al. 2000)

Direct Detection of  Pic b Standard Star HR 2435  Pic Target - Standard Target/ Standard Lagrange et al. 2008

A Planet Around Fomalhaut… The Fomalhaut disk’s brightness asymmetry which may be caused by secular perturbations of dust grain orbits by a planet with a = 40 AU and e = 0.15 Distance between planet and disk and thickness of disk suggest planet mass < 3MJup Kalas et al. (2008) (Stapelfeldt et al. 2005)

or a circumplanetary dust disk? Kalas et al. 2008 “Planet” is significantly brighter than expected at visual wavelengths “Planet” possesses same color as center star “Planet light” could be light scattered from circumplanetary dust grains that are forming a moon

An Orbiting Planetary System Around HR 8799? Marois et al. 2008 (see APOD: http://apod.nasa.gov/apod/ap081117.html): Gemini North near-infrared (1.1 - 4.2 m) images Reveal 3 objects with projected separations 24, 38, and 60 AU in nearly face-on orbit Around HR 8799, an 160 Myr old, nearby (39.4 pc), main sequence A5V star

An Asteroid Belt and a Kuiper Belt? The SED of HR 8799 is best fit using two single temperature black bodies with temperatures, Tgr = 160 K and 40 K These temperatures correspond to distances of 8 AU and 110 AU, respectively.

Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations

Outstanding Science Questions Do terrestrial planets form via the same mechanisms in other solar systems? Are planetary embryos built up on the same timescales and via the same processes? Do large collisions occur, indicating possible moon forming events or water delivery? Do the giant planets in other solar systems migrate, creating periods like the Late Heavy Bombardment? Is the Solar System’s composition and architecture (configuration of terrestrial planets, asteroid belt, Jovian planets, and Kuiper Belt) common?

Planet Formation in Our Solar System Terrestrial Planet Formation Giant Impacts including Moon Formation and Late Patina Formation of km-sized bodies Oligarchic Growth ~few Myr 30-100 Myr time 1-3 Myr 10-30 Myr Core Formation Envelope Accretion Giant Planet Formation Once gas has dissipated, km-sized bodies agglomerate into oligarchs that stir small bodies Infrared observations of dust can help constrain disk properties during the period of oligarchic growth to determine average properties and magnitude of variation

Oligarchic Growth Simulations Coagulation N-body simulations (Kenyon & Bromley 2004, 2005, 2008) Gas dissipates on a timescale ~10 Myr Parent bodies with sizes 1m-1km at 30-150 AU in the disk Pluto-sized (1000 km) objects grow via collisions until gas dissipates They stir leftover planetesimals, which generates debris

MIPS 24 m Excess Evolution Our MIPS 24 m observations of F0-F5 stars are broadly consistent with the Kenyon & Bromley (2008) models, but do not indicate a peak in the upper envelope of 24 m excess at 15-30 Myr The Carpenter et al. (2009) observation of US show that models must be updated to include dust within 30 AU around the late-type stars Chen et al. 2011

A Hypervelocity Collision Around HD 172555 Silica (Tektite and Obsidian) and possible SiO gas detected Fine dust mass 1020 kg; gas mass 1022 kg, if gas is fluorescent If gas is dense then it must be transient High spectral resolution observations are needed to confirm SiO, measure gas properties and infer excitation mechanism Lisse et al. 2009

The Main Asteroid Belt as a Function of Time Grogan et al. 2001 Simulations of the Main Asteroid Belt suggest that individual collisions between parent asteroids may have been detectable to outside observers Are debris disks observed today bright because they have undergone a recent collision?

The Period of Late Heavy Bombardment in Our Solar System The moon and terrestrial planets were resurfaced during a short period (20-200 Myr) of intense impact cratering 3.85 Ga called the Late Heavy Bombardment (LHB) Apollo collected lunar impact melts suggest that the planetary impactors had a composition similar to asteroids Size distribution of main belt asteroids is virtually identical to that inferred for lunar highlands Formation and subsequent migration of giant planets may have caused orbital instabilities of asteroids as gravitational resonances swept through the asteroid belt, scattering asteroids into the terrestrial planets. Strom et al. (2005)

Is  Crv Experiencing a Period of Late Heavy Bombardment? Wyatt et al. 2004 Lisse et al. 2011 The SED shows warm (~300 K) and cool components (~30 K) The mid-infrared spectrum of the warm component is well modeled using primitive materials such as amorphous silicates and carbon, metal sufides, and water ice

Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations

JWST MIRI 6.5 m primary mirror Direct imaging: 5.6-25.5 m Coronagraphic Imaging: 4QPM 10.65, 12.3, 15.5 m Lyot 23 m Low Resolution Spectrograph (R~100): 5-10 (14) m Medium Resolution Spectrograph (R~3000): 5-27 m

Mid-Infrared Imaging of the Vega Disk Su et al. 2005 Spitzer MIPS 24 and 70 m imaging has revealed a large extended disk at distances > 85 away from the central star The dust geometry and the low apparent vsini of the star suggests that the star-disk system is face-on Mid-infrared imaging is sensitive to smallest grains that are either gravitationally unbound or on eccentric orbits

Millimeter Imaging of the Vega Disk Wilner et al. 2002 IRAM Plateau de Bure inteferometric observations at 1.3 mm detected dust in two lobes around Vega, at distances 9.5 and 8.0 from the central star The observations can be explain using large dust grains that are trapped into principal mean motion resonances of a 3 MJup planet

High Resolution Multi-wavelength Imaging Wyatt 2006 Sub-blow out sized dust grains will be subject to radiation pressure (infrared imaging) Largest grains may be trapped in resonances (submm/mm imaging) Intermediate-sized grains may be at similar distances as larger grains but not physically trapped in resonances (far-infrared imaging)

Processed Grains in the Outer Solar System Infrared spectroscopy of comets and analysis of comet dust grains from STARDUST suggest that comets possess crystalline silicates How does material processed at high temperatures near the sun mix in a proto-planetary disk become incorporated into cold bodies such as comets?

Spatially Resolved Spectroscopy Gradients in grain size as a function of position in debris disks may suggest the presence of planetesimal belts (e.g. Okamoto et al. 2004 - Pic) Gradients in grain composition as a function of position may allow use to test theories for the origin of atomic gas Okamoto et al. 2004

Conclusions Our Solar System possesses second generation dust generated by sublimation of comets and collisions between asteroids and KBOs There are exoplanetary systems that possess similar dust In these systems, collisions between asteroids and comets is believed to generate dust Whenever disks are observed at high angular resolution, structures, suggesting the presence of planets are discovered Observations of these systems can help us place constraints on terrestrial planet formation and solar system evolution JWST is expected to make important contributions to our understanding of debris disks