5. Excesos IR F  

7. Discos “flared ”

10. 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 << 1 00

11. Dust absorption/emission different  ** dd Dust opacity abs emiss star + shock disk

16. Properties of disk structure D’Alessio et al 1999 zszs  1/R “flared” hasta R ~ 100 AU TcTc T fot T vis T0T0 T c ~ T fot  1/R 1/2 T c > T fot

17. T profiles T0T0 T fot TcTc Disk optical depth

20. SEDs D’Alessio et al 1999 SED @ IR similar for low dM/dt – dominated by irradiation F mm increases with  dM/dt / 

21. Dependence of SED on inclination to line of sight D’Alessio et al 1999 At high inclinations disk self-absorbs scattered light inclination

22. Imagenes D’Alessio et al 1999 Dark lane: optically thick disk layers near mid-plane

23. Optical/mm Optical/near IR scattered light (upper layers) mm emission (midplane, most mass)

24. Gas T different from dust T Glassgold et al 2004 X-ray heating of gas in upper less dense layers