excesos ir f discos “flared ”
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Excesos IR
F
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Discos “flared”
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•Radiation enters at angle to local normal: deposits at o ~1, o= cos o,,, , o, , 0 << 1
(*) > (disk), because dust opacity decreases with => * > disk => energy is deposited at disk = 0 /q, with q = */disk >> 1
•Stellar energy is deposited in upper levels
Upper layers are hotter than regions where the continuum form
N
Continuum disk ~ 1
disk =0/q << 10
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Dust absorption/emission different
* d
Dust opacity
abs emiss
star + shockdisk
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Properties of disk structure
D’Alessio et al 1999
zs
1/R
“flared” hasta R ~ 100 AU
Tc
Tfot
Tvis
T0
Tc ~ Tfot 1/R1/2
Tc > Tfot
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T profiles
T0
TfotTc
Disk optical depth
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SEDs
D’Alessio et al 1999
SED @ IR similar for low dM/dt – dominated by irradiationFmm increases with dM/dt /
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Dependence of SED on inclination to line of sight
D’Alessio et al 1999
At high inclinations disk self-absorbs
scattered light
inclination
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Imagenes
D’Alessio et al 1999
Dark lane: optically thick disk layers near mid-plane
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Optical/mm
Optical/nearIR scattered light (upper layers)
mm emission(midplane, most mass)
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Gas T different from dust T
Glassgold et al 2004
X-ray heating of gas in upper less dense layers