1. New results on the giant dark silhouette disk dd114-426 in the Orion Nebula. Anna Miotello Massimo Robberto miotello@stsci.edu August 12 th, 2011 Physics Graduated in Physics at University of Milan, Italy (2011) Astrophysics Doing Master’s degree in Astrophysics at University of Milan, Italy Anna Miotello

2. Anno accademico 2009-2010 Anna Miotello 114-426 NASA, ESA, M. Robberto (STScI/ESA), HST Orion Treasury Project Team.

3. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto (Ricci et al. 2008) The presence of disks with and without evidence of photoevaporation in the same cluster provides a unique opportunity of understanding how environmental factors may affect the path to planet formation.

4. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto HST images WFPC2 ACS F435WF555W F775WF658N F820LP F336W 1000AU N W U Hα V Bz I

5. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto i.Disk Structure Multiple asymmetry  Lobe dimensions  Lobe positions  Stretched disk’s top ACS F820LP ~44° (Atanassiu L. F. D.)

6. N W 210 AU 746 AU1117.8 AU ★ Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto i.Disk Structure F658N – F850LP

7. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto ii.114-426 in its Environment ~ 0.01 pc ~ 0.03 pc 117-421 121-434 EUV flux from θ 1 C

8. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto ii.114-426 in its Environment (Bally et al. 2000)

9. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto Photoevaporation EUV photons ( hν ≥ 13.6 eV ) FUV photons ( 6 eV ≤ hν ≤ 13.6 eV ) o Create a PDR at the disk surface with T ~ 100 ÷ 1000 K o Are absorbed early on at a IF in the photoevaporated wind that escapes radially, being ionized and heated to T ~ 10 000 K o Are not absorbed by atomic hydrogen and easily penetrate to the disk surface FUV Even in the core of the Trapezium Cluster, disk photoevaporation is normally supported by FUV photons (Johnstone et al. 1998 )

10. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto Mass loss (Adams et al. 2004) o Chemical composition o FUV flux coming from the Trapezium and scattered by the nebular wall Observations ~ 1

11. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto 49 X pixel 80 85 84 83 82 81 86 88 87 89 93 92 91 90 Y pixel

12. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto 49 X pixel 80 85 84 83 82 81 86 88 87 89 93 92 91 90 Y pixel Pixel Mean Radius Refraction index Pixel [49:93] : a = 0.20 μm m = 1.3 + i0.01 Pixel [49:92] : a = 0.21 μm m = 1.3 + i0.01 Pixel [49:91] : a = 0.36 μm m = 1.3 + i0.01 Pixel [49:90] : a = 0.42 μm m = 1.3 + i0.01 Pixel [49:89] : a = 0.44 μm m = 1.3 + i0.01 Pixel [49:88] : a = 0.48 μm m = 1.3 + i0.01 Pixel [49:87] : a = 0.53 μm m = 1.3 + i0.01 Pixel [49:86] : a = 0.51 μm m = 1.3 + i0.01 Pixel [49:85] : a = 0.53 μm m = 1.3 + i0.01 Pixel [49:84] : a = 0.55 μm m = 1.3 + i0.01 Pixel [49:83] : a = 0.58 μm m = 1.3 + i0.01 Pixel [49:82] : a = 0.59 μm m = 1.3 + i0.01 Pixel [49:81] : a = 0.60 μm m = 1.3 + i0.01 Pixel [49:80] : a = 0.60 μm m = 1.3 + i0.01

13. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto Mass loss (Adams et al. 2004) Disk Mass (McCaughrean et al. 1998; Mann & Williams 2010) Time scale for the mass loss of the disk

14. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto

15. Ancillary slides miotello@stsci.edu August 12 th, 2011

16. Sections Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto  Geometry of the disk  Dust particles sizing  Results and Comments  Observations  Conclusions

17. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto o The largest in ON: D ~ 1000AU. (McCaughrean et al. 1998) o Undetected central star: A v ≥ 60 mag of extinction. (McCaughrean et al. 1998) o Estimation for the disk mass: (McCaughrean et al. 1998; Mann & Williams 2010) Previous works o Properties of disk grains: evidence of chromatic extinction and grain growth (1.9 μm ≤ d ≤ 4 μm). (Throop et al. 2001; Shuping et al. 2003)

18. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto i.Disk Structure Tail

19. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto Extinction curve Q ext x Radius of the spherical particle n = 1.3

20. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto Extinction curve Q ext x Radius of the spherical particle Observational data : Q max

21. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto

22. A nna M iotello Physics Graduated in Physics at University of Milan, Italy (2011) Astrophysics Doing Master’s degree in Astrophysics at University of Milan, Italy Working on 114-426 protoplanetary disk 114-426 protoplanetary disk in the Orion Nebula with Dr. Massimo Robberto (SASP 2011 - STScI) miotello@stsci.edu

23. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto

24. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto

25. Anna Miotello August 12 th, 2011 miotello@stsci.edu Massimo Robberto