CO ro- vibra+onal diagnos+c from the inner regions of protoplanetary disks

Transcription

1 CO ro- vibra+onal diagnos+c from the inner regions of protoplanetary disks Inga Kamp, Rosina Hein Bertelsen, Wing- Fai Thi, Rens Waters, Peter Woitke, Koen Maaskant

2 Observa+ons in the near- IR e.g. [NeII] 12.8 µm H µm HD 56, 112 µm C 2 H 2, HCN CO high J CO low J sub-mm ices H 2 O high T ex CO ro-vib 2-5 µm H 2 O ro-vib [OI] 63 µm H 2 O low T ex planetary systems [CII] 157 µm r cond 1 AU 10 AU 100 AU

3 Observa+ons in the near- IR, HD 56 e.g. [NeII] 12.8 µm H µm 112 µ m CO low J sub-mm C2H2, HCN igh J CO h ices H2O high T ex CO ro-vib 2-5 µm H2O ro-vib [OI] m H2O low Tex [CII planetary systems rcond 63 µ 1 AU 10 AU ] 157 µm 100 AU [figure top: Garufi et al. 2014; CO ro-vib observational work by Brittain et al. 2003, 2007, 2009, Blake & Boogert 2004, Goto et al. 2006, 2012, Pontoppidan et al. 2011, Bast et al. 2011, van der Plas et al. 2009, 2010, 2015, Hein Bertelsen et al. 2014]

4 Relevance of UV for CO ro- vib disk emission! T(r) = T 0 # " r R in $ & % 0.3 [Brittain et al. 2009] T, n log r v kep [ProDiMo: Woitke, Kamp, Thi 2009, CO ro-vib: Thi et al. 2012] Location of CO in a disk is not a free parameter, but determined by the gas temperature (formation) and photodissociation (destruction - UV) Detailed disk structure matters!

5 Relevance of UV for CO ro- vib disk emission! T(r) = T 0 # " r R in $ & % 0.3 [Brittain et al. 2009] T, n log r v kep [ProDiMo: Woitke, Kamp, Thi 2009, CO ro-vib: Thi et al. 2012] Location of CO in a disk is not a free parameter, but determined by the gas temperature (formation) and photodissociation (destruction - UV) Detailed disk structure matters!

6 Relevance of UV for CO ro- vib disk emission! T(r) = T 0 # " r R in $ & % 0.3 [Brittain et al. 2009] T, n log r v kep [ProDiMo: Woitke, Kamp, Thi 2009, CO ro-vib: Thi et al. 2012] Location of CO in a disk is not a free parameter, but determined by the gas temperature (formation) and photodissociation (destruction - UV) Detailed disk structure matters!

7 Relevance of UV for CO ro- vib disk emission! T(r) = T 0 # " r R in $ & % 0.3 [Brittain et al. 2009] T, n log r v kep [ProDiMo: Woitke, Kamp, Thi 2009, CO ro-vib: Thi et al. 2012] Location of CO in a disk is not a free parameter, but determined by the gas temperature (formation) and photodissociation (destruction - UV)? Detailed disk structure matters!

8 The role of CO ro- vib fluorescence Fluorescence populates higher v-bands at the expense of the fundamental v=1-0 band => band ratios change [Thi et al. 2012, Hein Bertelsen et al. 2014] Line fluxes also depend on emitting area => fluxes stay, noses come and go

9 The role of CO ro- vib fluorescence factor ~2 factor ~10 factor ~100 Fluorescence populates higher v-bands at the expense of the fundamental v=1-0 band => band ratios change [Thi et al. 2012, Hein Bertelsen et al. 2014] Line fluxes also depend on emitting area => fluxes stay, noses come and go

10 The role of CO ro- vib fluorescence factor ~2 factor ~10 factor ~100 Fluorescence populates higher v-bands at the expense of the fundamental v=1-0 band => band ratios change [Thi et al. 2012, Hein Bertelsen et al. 2014] Line fluxes also depend on emitting area => fluxes stay, noses come and go

11 CO ro- vib characteris+cs CO ro- vib fluxes fairly flat versus wavelength (factor <3 between low & high J) [HD100546: CRIRES, Hein Bertelsen et al. 2014, HD163296: CRIRES, Hein Bertelsen et al. submieed; HD135344B: CRIRES Carmona et al. 2014; to be checked for larger Herbig sample: van der Plas et al. 2015] FWHM either flat with J or increasing with J => signature of gaps? [Hein Bertelsen et al. in prep., van der Plas et al. 2015] Grid of generic models based on HD97048 properxes [Maaskant et al. 2013]: zone 1 zone 2 - lower the dust content in zone 1 and/or 2 - lower the dust and gas content in zone 1 and/or 2 - change the flaring angle of the enxre disk < 2.5 AU 2.5 < r < 30 AU

12 CO ro- vib characteris+cs zone 1 zone 2 < 2.5 AU 2.5 < r < 30 AU CO can self-shield and does not need dust to protect it Below a critical gas mass (column density), CO cannot exist dust+gas gap dust gap zone 1,2 M dust x 1.e- 6 zone 1,2 M disk x 1.e- 6

13 CO ro- vib characteris+cs removing the inner gas (!), CO ro- vib fluxes go up by 1-2 orders of magnitude log λf λ [erg/cm 2 /s] F line [W/m 2 ] flux flat versus J flux flat versus J flux strongly varies with J dust gap dust+gas gap zone 1,2 M dust x 1.e- 6 zone 1,2 M disk x 1.e- 6 λ [µm] λ [µm] λ [µm]

14 CO ro- vib characteris+cs FWHM either flat with J or increasing with J - > signature of gaps? FWHM increases with J FWHM flat versus J FWHM flat versus J log λf λ [erg/cm 2 /s] dust gap zone 1,2 M dust x 1.e- 6 dust+gas gap zone 1,2 M disk x 1.e- 6 λ [µm] λ [µm] λ [µm]

15 CO ro- vib characteris+cs FWHM either flat with J or increasing with J - > signature of gaps? log λf λ [erg/cm 2 /s] dust gap zone 1,2 M dust x 1.e- 6 dust+gas gap zone 1,2 M disk x 1.e- 6 λ [µm] λ [µm] λ [µm]

16 CO ro- vib diagnos+cs for planet forma+on CO cannot live anywhere in a disk => photodissociaxon data, dissociaxve collisions with hot H, H 2, He CO cannot emit anywhere in a disk => collision rates If we understand where CO exists and what its excitaxon is, we can invert the problem and draw conclusions on the detailed inner disk structure => planet forming region

17 CO ro- vib diagnos+cs for planet forma+on CO cannot live anywhere in a disk => photodissociaxon data, dissociaxve collisions with hot H, H2, He CO cannot emit anywhere in a disk => collision rates If we understand where CO exists and what its excitaxon is, we can invert the problem and draw conclusions on the detailed inner disk structure [VLA: Greaves et al. 2008] => planet forming region, they are there! [HD100546: Quanz et al. 2013] [ALMA: disk around HL Tau] [Reggiani et al. 2014]

18 COST Action CM1401: Our Astrochemical History Our$Astro)Chemical$History$$$$$ In%a%nutshell%!% Working groups on: - Gas-phase chemistry - Icy surface chemistry - Photo-chemistry - Isotope chemistry Laurent Wiesenfeld (IPAG) Inga Kamp (University of Groningen) Helen Fraser (Open University) Contact us! Scientific Kick-Off Meeting: Prague, May 26 May 29, 2015 Petr Slaviček, J. Heyrovský Institute

19 COST Action CM1401: Our Astrochemical History Our$Astro)Chemical$History$$$$$ In%a%nutshell%!% Working groups on: - Gas-phase chemistry - Icy surface chemistry - Photo-chemistry - Isotope chemistry Laurent Wiesenfeld (IPAG) Inga Kamp (University of Groningen) Helen Fraser (Open University) Contact us! Scientific Kick-Off Meeting: Prague, May 26 May 29, 2015 Petr Slaviček, J. Heyrovský Institute