lecture 9: the spectral energy distributions of dusty...
TRANSCRIPT
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Herschel/Spitzer Image of Protostars in L1641
4.5 μm70 μm
160 μm
Lecture 9: The Spectral Energy Distributions of Dusty Young Stellar
Objects
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2
Review: From Cores to Stars
Remember:
Pressure supported isothermal core bounded by Pressure and Gravity
Bonnor-Ebert sphere:Solution for hydrostatic equilibrium
Figure pirated from K. Dullemond
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Why Cores Collapse
3
Gravitationally bound isothermal cores are intrinsically unstable:
As compressed, kinetic energy is constant (K = 3/2 M k T), but gravitational potential energy decreases (U = - GM2/R).
In contrast, a pressure bound core is not unstable. Instability in Bonner-Ebert sphere depends on whether core is primarily pressure confined or gravitationally bound.
Thus, collapse is a natural consequence of the isothermality.
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Inside-out collapse model of Shu (1977)
Singular isothermal sphere: r-2
Free-fall region: r-3/2
Transition region: matter starts to fall
Expansion wave front
Slide pirated from K. Dullemond
Note: free fall time shorter for dense gas, hence centrally condense core leads to inside-out collapse
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Angular Momentum leads to Disk
cst
Increasing angular momentum
Axis of rotation
Disk Shocks
Parabolic Orbits
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The Luminosity of Protostars
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Observable Consequences in SEDs
• Protostars:–central protostar–disk surrounding protostar– infalling envelope–envelope flattened by rotation (lower optical depth along
rotaton axis)–outflows clear cavities along rotation axis
• Pre-main sequence stars–central star–disk surrounding star
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Spectral Energy Distributions (SEDs)Plotting normal flux makes it look as if the source emits much more infrared radiation than optical radiation:
This is because energy is:
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Fν dν = Fν ΔνSlide pirated from K. DullemondSlide pirated from K. Dullemond
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Spectral Energy Distributions (SEDs)Typically one can say: and one takes a constant (independent of ν).
€
Δν = ν Δ(logν)
€
Δ(logν )
€
νFνIn that case is the relevant quantity to denote energy per interval in logν. NOTE:
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νFν ≡ λFλ
Slid
e pi
rate
d fr
om K
. Dul
lem
ond
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Temperature of a dust grain
Heating:
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Q+ = π a2 Fν εν∫ dν
a = radius of grainεν= absorption efficiency (=1 for perfect black sphere)
Cooling:
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Q− = 4π a2 πBν (T)εν∫ dν
€
κν =π a2ενm
Thermal balance:
€
4π a2 πBν (T)εν∫ dν = π a2 Fν εν∫ dν
€
Bν (T)κν∫ dν =14π
Fν κν∫ dν
Optically thin case:
Slide pirated from K. Dullemond
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€
σπT 4 =
14π
F
Temperature of a dust grain
Assume grey opacity:€
Bν (T)κν∫ dν =14π
Fν κν∫ dν
€
σπT 4 =
14π
L*4π r2
€
T 4 =14σ
L*4π r2
€
T 4 =14σ
4π r*2σT*
4
4π r2
€
T 4 =r*2T*
4
4r2
€
T =r*2r
T*
Slide pirated from K. Dullemond
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Reprocessing of Starlight and Dust Photospheres
Thus, the shell will appear as a cool blackbody
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In reality, we don’t have one temperature
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The SEDs of Protostars (from Hartmann)
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Dust Absorption in the IR
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From Hartmann
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SED of Protostars
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Herschel Orion Protostar Survey
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Real Protostars (Will Fischer)
• Modeled SEDs with B. Whitney’s RT code
• Key parameters• Luminosity• Envelope density
• With stellar parameters, derive• Envelope infall rate• Accretion luminosity
• HOPS 168, 203: dMdisk/dt = dMenv/dt implies Mstar ~ 0.1 Msun• Episodic accretion would allow larger masses
λ (µm)
λFλ (
erg
s-1 c
m-2
)
(Fischer et al. 2010, A&A special issue)
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HOPS 68 - a flattened protostar with external heating
envelope
attenuateddisk
attenuatedstar
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The Protostars HOPS 68
From Poteet, submitted. Using the inner envelope density and assumed stellar mass, we get:
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HOPS 68 - a protostar with external heating
envelope
attenuateddisk
attenuatedstar
Peak of internally heated envelope
Peak of externally heated envelope
total
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The Contribution from Scattering
ScatteringTotal
RV = 3.1 dust modelBruce Draine’s website
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Spectra of collapsing cloud + star + diskWhitney et al. 2003
Class ISlide pirated from K. Dullemond
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Spectra of collapsing cloud + star + diskWhitney et al. 2003
Class 0Slide pirated from K. Dullemond
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HOPS 136: A Case Study of an Edge-on Protostar
Fischer et al. in prep.
Luminosity = 1.8 solar lum.Mass infall = 3x10-6 solar masses per yearRc = 500 AUInclination = 90o (opposed to 81o from Robitaille fitter)
Thermal Emission from envelope and disk
Light from inner disk and photosphere scattered by envelope and dust in outflow cavity.
Shadow
outfl
ow
cavity
Disk
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Plus we have a disk, seen in absorbed scattered light: Models of HOPS 136
W. Fischer
Note: this example is not a particularly good fit
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Disks
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Spectra of collapsing cloud + star + diskWhitney et al. 2003
Class IISlide pirated from K. Dullemond
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Spectra of collapsing cloud + star + diskWhitney et al. 2003
Class IIISlide pirated from K. Dullemond
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Calculating the SED from a flat disk
€
Iν (r) = Bν (T(r))
Assume here for simplicity that disk is vertically isothermal: the disk emits therefore locally as a black radiator.
Now take an annulus of radius r and width dr. On the sky of the observer it covers:
€
dΩ =2π rdrd2
cosi
€
Fν = Iν dΩand flux is:
Total flux observed is then:
€
Fν =2π cosid2
Bν (T(r)) rdrrin
rout∫Slide pirated from K. Dullemond
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Multi-color blackbody disk SED
Wien region
multi-color region
Rayleigh-Jeans region
λ
νFν
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Heating and Coolings of Disks
Disk
StarlightThermal emission from disk
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Flat irradiated disks
α
€
α ≅0.4 r*r
Irradiation flux:
€
Firr =αL*4π r2
Cooling flux:
€
Fcool =σT 4
€
T =0.4 r*L*4πσ r3
⎛
⎝ ⎜
⎞
⎠ ⎟
1/ 4
€
T ∝ r−3 / 4
Similar to active accretion disk, but flux is fixed.Similar problem with at least a large fraction of HAe and T Tauri star SEDs.
Slide pirated from K. Dullemond
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Flared disks
flaring
irradiation
heating vs cooling
verticalstructure
● Kenyon & Hartmann 1987● Calvet et al. 1991; Malbet & Bertout 1991● Bell et al. 1997; ● D'Alessio et al. 1998, 1999● Chiang & Goldreich 1997, 1999; Lachaume et al. 2003
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Summary
36
Spectral Energy Distributions: distribution of power over large portion of the electromagnetic spectrum. Usually constructed from a mixture of photometry and spectroscopy from many different instruments.
SEDs are a major source of information on protostars and stars with disks.
Dust temperature for a grain being heated directly by a star decreases T = k r-1/2
An optically thick shell (were the primary form of opacity is dust) can reprocess radiation to a lower wavelength, creating an effective low temperature dust photosphere. Tshell = k Rshell-1/2
The radius of the dust photosphere depends on the wavelength and opacity - this pushes thepeak of the protostellar SED into the far-IR
Scattering of light from the inner star and disk by the envelope may also fill in protostellar SEDs atwavelengths < 10 μm.
Disks can be modeled as a series of concentric annuli each heated to a different temperature.
For a passively heated flat disk, the temperature goes as T = k r-3/4