circumstellar disks - a primer ast622 the interstellar medium partially based on les houches lecture...
TRANSCRIPT
Circumstellar disks - a primer
Ast622
The Interstellar Medium
Partially based on Les Houches lecture by Michiel Hogeheijde
(http://www-laog.obs.ujf-grenoble.fr/heberges/Houches08/index.htm)
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Motivation
• The last step in the transport of the ISM to stellar scales
• The first step in the formation of planetary systems
Disks are an inevitable ( ubiquitous?) consequence of angular momentum conservation
Indirect evidence for disks
• Emission line (H) stars above the main sequence accretion
• Infrared-millimeter excess emission reprocessing of starlight by a non-spherical geometry
• Ultraviolet excess and X-ray emission accretion hot spots and star-disk interface
Direct evidence for disks(i.e. imaging)
Smith & Terrile 1984
Direct evidence for disks(i.e. imaging)
SED classification
αIR = -dlog(νFν)/dlog(ν)
= log(25F25/2F2)/log(2/25)
(Lada 1987)
Fig from Andre
SED theory
• Chiang & Goldreich (1997) following pioneering work by Adams, Lada & Shu (1987), Kenyon & Hartmann (1987)
• Also see reviews by Beckwith (1999) and Dullemond et al. (2006)
Flat blackbody disk
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Flat blackbody disk
Observe
d
Fig. 1.— SED for the flat blackbody disk, with contributions from star and disk identified. The n = 4/3 law is evident between 30 μm and 1 mm. The turnover near 1 mm is due to our truncation of the disk at ao ≈ 270 AU. Chiang & Goldreich 1997
Flared blackbody diskThe vertical component of gravity will decrease with radius along with the surface density. Hydrostatic equilibrium then implies the disk scale height increases with radius: the disk is flared.
The outer regions of the disk of a flared disk intercept more starlight than a flat disk and the mid-to-far infrared emission is stronger.
Flared blackbody disk
Fig. 2.— SED for the flared blackbody disk. At mid-IR wavelengths, Lν ∝ ν−2/3. At longer wavelengths, Lν ∝ ν3.
Radiative equilibrium disk
Fig. 3.— Radiative transfer in the passive disk. Stellar radiation strikes the surface at an angle α and is absorbed within visible optical depth unity. Dust particles in this first absorption layer are superheated to a temperature Tds. About half of the emission from the superheated layer emerges as dilute blackbody radiation. The remaining half heats the interior to a temperature Ti.
Radiative equilibrium disk
Radiative equilibrium disk
Radiative equilibrium flared disk
Fig. 6.— SED for the hydrostatic, radiative equilibrium disk. At mid-IR wavelengths, the superheated surface radiates approximately 2–3 times more power than the interior. Longward of 300 μm, n gradually steepens from about 3 to 3 + β as the disk becomes increasingly optically thin.
Radiative equilibrium flared disk
Adding in solid state features
Fig. 10.— SED for the hydrostatic, radiative equilibrium disk using a grain emissivity profile motivated by data from Mathis (1990). For wavelengths shorter than 0.3 μm, our assumed emissivity is unity; longward of 0.3 μm, it obeys a (single) power-law relation ∊λ = (0.3 μm/λ)1.4, on which are superposed two Gaussians centered on 10 and 20 μm, having amplitudes that are 3 times their local continuum emissivity and FWHM equal to 3 and 9 μm, respectively.
Flaring + hot inner rim
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Dullemond et al. 2006, PPV review
Dependence of SED on disk geometry
Dependence of SED on disk geometry
Dependence of SED on disk geometry
Dependence of SED on disk geometry
Dependence of SED on disk geometry
SED + spatial modeling
disk mass, radius and temperature and surface density profiles, T ~ R-q, ~ R-p
Andrews & Williams 2007
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Accretion disk theory
Same temperature profile (and hence SED) as as passive flat blackbody disk, T R-3/4
Flared disk SEDs dominated by stellar irradiation.
Accretion critical for understanding disk evolution
L = GMMdot/R
Annual Reviews 1981
Viscous evolution
accretion shocks
magnetospheric accretion
spreading
Muzerolle et al. (1998, 2001)
Gullbring et al. (1997)
As disk accretes to star, conservation of momentum implies disk spreads out; mass, accretion, decrease with time, radius increases with time.
Andrews & Williams 2007
Dust mineralogy
van Boekel et al. (2004)
observed
olivine
pyroxene
hydrosilicate
ISM silicate
Grain growth
submillimeter emission “efficiency” ~ 2 ~ 0
ISM grains pebbles/snowballs
related to size of largest solids in diske.g. Pollack et al. (1994), Draine (2006)
Grain growth
Isella et al. 2007
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disk ~ 1ISM ~ 2
Grain growth
Andrews PhD thesis 2007
Dust settling
Dullemond et al. 2004
The gaseous disk
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Molecular Hydrogen
H2 is difficult to detect• no permanent dipole -> no dipole rotational transitions; only weak quadrupole transition in mid-IR that require hundred K or more to excite• conflicting reports about detection• fluorescent H2 emission in UV (electronic transitions) and near-infrared (vibrational) has been detected but is difficult to analyze quantitatively
Molecular Hydrogen
Lahuis et al. (2007)
Near infrared disk ro-vibrational lines
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Boogert et al. 2002
Recent Spitzer IRS results
Watson et al. 2007 Carr & Najita 2008
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Atomic fine structure lines in disks:probes of the giant planet forming region
Herschel GASPS Key Program
Atomic fine structure lines in disks:probes of the giant planet forming region
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Herschel GASPS Key Program
Millimeter observations:the cold outer reservoir
Simon et al. (2000)
• <1% by mass of gas consists of CO, and smaller quantities of other molecules and atoms
• CO easily detected in mm rotational transitions• shows rotation patterns• inferred masses 10-100 times smaller than from dust:
depletion• CO freezes out on dust grains for T<20 K
Qi PhD thesis 2000
Millimeter observations:the cold outer reservoir
Disk chemistry
• most molecules now understood to be present only in a warm layer at intermediate height and close to the star• frozen out in mid-plane• photo-dissociated in the disk surface
Semenov et al. (2008)
Disk chemistry:resolving the D/H ratio
Qi et al. (2008)
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Disk lifetimes
Haisch et al. 2001 Hillenbrand 2005fdisk > 80% at ~1 Myrfdisk ~ 50% at ~3 Myr
fdisk ~ few% at >10 Myr
Disk lifetimes
Andrews & Williams 2005
NIR excess outer diskInner and outer disks have
similar dissipation timescales
sub-mm emission(disk masses)decreases with IR SED evolution
sub-mm SEDchanges with
IR SED evolution(particle growth)
Class I disks
Class II disks
Class III disks
Disk evolution (at mm)
Sean Andrews PhD 2007
Transitional disksViscous evolution is expected to be quicker at small radii but transitional disks, with mid-infrared dips in their SED and cold outer rings of dust and gas are rare (and possibly only seen around binaries?)
Brown et al. 2008
Disk clearing through photoevaporation
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Alexander et al. 2006
Alexander “UV-switch” model where stellar wind very rapidly erodes disk (from inside out but in only ~105yr) as accretion rate drops below photoevaporation rate
External photoevaporation
O’Dell, McCaughrean, Bally Williams et al. 2005
Rapid mass loss, 10-5 M☉/yr, at center, but massive disks survive at large distances (Rita Mann PhD)
Debris disks
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astro-ph/0511083
Debris disks
Williams et al. 2004
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Isella et al. 2007
Debris disks have double peaked SEDs with a stellar photosphere plus generally a single temperature dust component. They have very low (if any) gas and have a much simpler geometry than protostellar disks.
Debris disks
See http://astro.berkeley.edu/~kalas/disksite/
As for protostellar disks, images are rare (but critically important); many properties inferred from infrared excesses and SED studies alone.
Summary• Disks are ubiquitous
– but generally only indirectly inferred from infrared excesses
• Masses range from 0.001–0.3 M☉
• Radii range from tens to hundreds of AU• Grains in disks grow to cm sizes• Gas shows Keplerian motion
– Many molecules (but not H2) frozen out in cold interior
• The fraction of stars with disks decreases with time– from >80% at <1 Myr to <10% at 10 Myr– ‘half-life’ of disks ~3 Myr– inner and outer disk dissappear almost simultaneously
• Debris disks from planetesimal collisions may be visible for >>100 Myr after star formation