evolution of pah features from proto-pn to planetary nebulae
DESCRIPTION
Evolution of PAH features from proto-PN to planetary nebulae. Ryszard Szczerba N. Copernicus Astronomical Center Toruń, Poland. NCAC TORUN. Collaborators. Mirek Schmidt (CAMK) Natasza Siódmiak (CAMK) Grażyna Stasińska (LUTH Obs. Paris-Meudon) Cezary Szyszka (UMK). NCAC TORUN. - PowerPoint PPT PresentationTRANSCRIPT
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Evolution of PAH features from Evolution of PAH features from proto-PN to planetary nebulaeproto-PN to planetary nebulae
Ryszard Szczerba
N. Copernicus Astronomical Center
Toruń, Poland
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2 Gdańsk 2005
Collaborators
•Mirek Schmidt (CAMK)
•Natasza Siódmiak (CAMK)
•Grażyna Stasińska (LUTH Obs. Paris-Meudon)
•Cezary Szyszka (UMK)
NCACTORUN
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NCACTORUN
Sir Frederick William Herschel
• F.W. Herschel (1738 -1822) was born in Hanover.
• From 1757 he lived in England.
• A musician and an astronomer.
• In 1781 he discovered Uranus;
• He created catalogs of double stars and nebulae;
• In 1800 he discovered infrared radiation.....
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Discovery of IR radiation. NCACTORUN
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Dust - CAMK PAN
TORUN
INTRODUCTION: Existence of solid particles was demonstrated by Trumpler (1930) through the measurements of color excess between the photographic (~4300 A) and V (~5500 A) magnitudes. By the end of 30’s, a -1 extinction law in the wavelength range 1-3 m-1 had been established. Greenstein (1938) proposed a power-law size distribution of dust grains (dn(a)/da ~ a-3.6!) in the size range 80A<a<1 cm to explain the -1 extinction law. The discovery of interstellar polarization stimulated Cayrel & Schatzman (1954) to consider graphite as interstellar dust component (strong optical anisotropy).
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Extinction lawNCAC
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R=A(V)/E(B-V) N(H)/E(B-V)~5.8 1021 cm-2 (Bohlin et al. 1978)
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graphitic structureNCAC
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Graphite is highly anisotropic material
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Dust - CAMK PAN
TORUN
INTRODUCTION cont.: Hoyle & Wickramasinghe (1962) proposed that graphite could form in the atmospheres of cool C-stars and be ejected into ISM.In 1960’s and early 1970’s UV space missions allowed to determine extinction law in the wavelength range 0.2-10 m-1.The presence of 2200 A interstellar extinction bump (Stecher 1965) was interpreted as reinforcement of the graphite proposal. However, exact nature of this bump still remains unidentified! Gilman (1969) proposed that grains around M-type stars are mainly silicates (Al2SiO3, Mg2SiO4, ...).Interstellar silicates were first detected in emission in Orion Nebula (Stein & Gillett 1969) and in absorption toward the Galactic Center (Hackwell et al. 1970).
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amorphous silicate featuresNCAC
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9.7 m Si-O stretching mode
18 m O-Si-O bending mode
Dust thermal emission:
m] x T[K] = 3000
ISM: T~20 K; max~150 m
CS: T~150 K; max~20 m
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Dust - CAMK PAN
TORUN
INTRODUCTION cont.: In mid-1970’s the interstellar extinction curve had been determined in the whole wavelengths range & the main dust components had been determined (graphite & silicates).
Mathis et al. (1977) proposed a model of interstellar dust composed of silicates and graphite with grain size distribution dn(a)/da ~ a-3.5 in the size range 50 A < a < 0.25 m (MRN model):MRN model is very successful: 1250 citations in ADS (56 in 2005).
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MRN model of interstellar dustNCAC
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Silicates & graphite:
•dn(a)/da ~ a-3.5
•50A<a<0.25 m
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Dust - CAMK PAN
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Very Small Grains (VSGs): Donn (1968) proposed that particles like Policyclic Aromatic Hydrocarbons (PAHs) may be responsible for the UV interstellar extinction. Greenberg (1968) first pointed out that VSGs with a heat content comparable to the energy of a single photon, cannot be characterized by an equilibrium temperature but are subject to fluctuations in temperature.
Observational arguments that VSGs are present in Interstellar Space:
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VSGs in Inter- & CS-stellar Space
CAMK PAN
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1) The discovery of presolar nanodiamonds (Lewis et al. 1987) and TiC nanocrystals (Bernatowicz et al. 1996).
2) The ubiquitous distinctive set of „UIR” emission bands @ 3.3, 6.2, 7.7, 8.6 and 11.3 m (UIR bands were discoverd first by Gillet et al. (1973) in planetary nebulae). This emission can be explained by transiently heating PAHs (e.g model of Li & Draine 2001 for ISM, where UIRs account ~20% of the total power radiated by dust).
3) The mid-IR emission at<60 m, discovered by IRAS (12 & 25 m bands) and confirmed by COBE-DIRBE and IRTS observations (see e.g. Draine 2003 and references therein). This emission can be explained also by transiently heating PAHs (Weingartner & Draine 2001).
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Presolar grains from meteoritesNCAC
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Presolar grainsNCAC
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„typical” dust particle (top)
Presolar SiC (right)
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NCACTORUN
reflection nebulae
PAH features in:
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PAHs: aromatic rings + HNCAC
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Leger & Puget (1984)Allamandola et al. (1989)
•C-H „stretch” @ 3.3m•C-C „stretch” @ 6.2 m•C-C „stretch” @ 7.7 m•C-H in-plane „bend” @ 8.6m•C-H out of plane „bend” @ 11.3 m for mono H@ 12.0 m for duo H@ 12.7 m for trio H@ 13.6 m for quartet H
•aliphatic (chain-like) C-H „stretch” @ 3.4 m
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graphitic structureNCAC
TORUN
Graphite is highly anisotropic material
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PAH features in:NCAC
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galaxies (top)
HII regions (right)
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NCACTORUN
The detection by ISO ofcrystalline silicates marks begining of: ASTROCRYSTALOGRAPHY
PAH features in:
[WR] planetary nebulae: Szczerba et al. (2001)
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The mid-IR emission at <60mNCAC
TORUN
Observed (left)
Model (bottom) Weigartner & Draine (2001)
For T=15-25 K, emission from „large” grains is lower by several orders of magnitude!
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VSGs in Inter- & CS-stellar Space
CAMK PAN
TORUN
4) The far-UV extinction rise (Donn 1968 – see also Kruegel 2003). Dust grains absorbs and scatters light most effectively @~2a.
5) The ”anomalous” Galactic foreground microwave emission in th 10-100 GHz region. Discovered during studies of CMB is probably due to the fats rotation fo nanoparticles (Draine & Lazarian 1998).
6) The Extended Red Emission (ERE), first discovered in Red Rectangle (Schmidt et al. 1980). The ERE is attributed to PL of (possibly?) crystalline nano-silicon clusters (Witt et al. 1998).
7) The photoelectric heating of the diffuse ISM. VSGs are more efficient in heating the gas than large grains. VSGs are responsible for > 95% of the total photoelectric heating of the gas in ISM (Weingartner & Draine 2001) .
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PAHs in LMC: Ciska Markwick-Kemper et al.
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PAHs in LMCNCAC
TORUN
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3.3 & 3.4 m bands in PN: BD+ 30 3639NCAC
TORUN
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7.7 & 8.6 m bands in PN: BD+ 30 3639NCAC
TORUN
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6.2, 7.7 & 8.6 m bands in PN: BD+ 30 3639NCAC
TORUN
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7.7 m band shape in proto-PN:NCAC
TORUN
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6.2 m band shape in galactic objectsNCAC
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3.3 m C-H stretching modeNCAC
TORUN
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6.2 m C-C stretching modeNCAC
TORUN
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7.7 m C-C stretching modeNCAC
TORUN
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Ratio of 7.7 an 6.2 m bandsNCAC
TORUN
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8.6 m C-H in-plane bending modeNCAC
TORUN
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Correlation between 3.3 & 6.2 m bandsNCAC
TORUN
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Correlation between 7.7 & 8.6 m bandsNCAC
TORUN
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3.3 m band in proto-PN:NCAC
TORUN
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6.2 m band in proto-PN:NCAC
TORUN
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7.7 m band in proto-PN:NCAC
TORUN
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8.6 m band in proto-PN:NCAC
TORUN
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•Stasińska, Szczerba, Schmidt, Siódmiak
„Post-AGB objects as testbeds of nuclosynthesis in AGB stars”
submitted to A&A• We can investigate chemistry in objects with smaller mass
• C: smaller uncertainty than in PNe
•....
NCACTORUN
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CNO in post-AGB objectsNCAC
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CNO in post-AGB objectsNCAC
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