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The mass-loss return from nearby evolved stars as deduced by Herschel
Leen Decin
- n behalf of
the MESS GTKP, HIFISTARS GTKP and HIFI Scan team on IRC+10216
VOOR STERREN K U N D E I N S T I T U U T
The mass-loss return from nearby evolved stars as deduced by - - PowerPoint PPT Presentation
The mass-loss return from nearby evolved stars as deduced by - - PowerPoint PPT Presentation
The mass-loss return from nearby evolved stars as deduced by Herschel Leen Decin on behalf of the MESS GTKP, HIFISTARS GTKP and HIFI Scan team on IRC+10216 I VOOR STERREN K N S U N T I D E T U U T Stellar mass loss: the Sun
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M~2*10-14 Msun/yr Stellar mass loss: the Sun
.
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Stellar mass loss: red giant M~10-8 - 10-4 Msun/yr
.
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Stellar mass loss: Luminous Blue Variable M~10-4 Msun/yr
.
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Importance of mass loss of evolved stars
Cosmic Chemistry Cycle
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Importance of mass loss of evolved stars
Cosmic Chemistry Cycle Important:
* chemical elements created in stellar core * enrichment of interstellar medium via mass loss Carbon on Earth forged by evolved stars
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+ circumstellar gas and dust: 10 - 1000K
It's cool ...
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... and complex
(Guélin et al. 1993) Evidence for overall spherical symmetry
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... and complex
Evidence of departure from overall spherical symmetry
1¨ (Weigelt et al. 1998) 2.5' (Groenewegen et al. 1997) 2.2' (Mauron & Huggins 2000)
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... and complex
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Chemistry in evolved stars
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- 1. Non-equilibrium chemistry
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- 1. Non-equilibrium chemistry
(IK Tau, Decin et al. 2010)
Few lines – long integration times
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- 1. Non-equilibrium chemistry
Herschel-PACS (4400 sec) ISO-LWS (1930 sec)
Royer et al. 2010 Matsuura et al. 2012
O-rich supergiant VY CMa
Spectral movie of VY CMa
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- 1. Non-equilibrium chemistry
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- 1. Non-equilibrium chemistry
Royer et al. 2010
[SiO/H2]=4.5·10-5 [H2O/H2]=3·10-4 [HCN/H2]=4.5·10-6
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- 1. Non-equilibrium chemistry
Royer et al. 2010
[SiO/H2]=4.5·10-5 [H2O/H2]=3·10-4 [HCN/H2]=4.5·10-6 [SiO/H2]=3.5·10-5 [H2O/H2]=7·10-5 [HCN/H2]=6·10-11 (TE)
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- 1. Non-equilibrium chemistry
Royer et al. 2010
[SiO/H2]=4.5·10-5 [H2O/H2]=3·10-4 [HCN/H2]=4.5·10-6 [SiO/H2]=3.5·10-5 [H2O/H2]=7·10-5 [HCN/H2]=6·10-11
(TE)
NON-TE
(Duari et al. 1999)
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- 2. Gas-grain reactions
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- 2. Gas-grain reactions
Lombaert et al. 2012
OH127.8+0.0
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- 2. Gas-grain reactions
low dust-to-gas, high water abundance high dust-to-gas, low water abundance Lombaert et al. 2012
OH127.8+0.0
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- 2. Gas-grain reactions
low dust-to-gas, high water abundance high dust-to-gas, low water abundance Lombaert et al. 2012
OH127.8+0.0
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- 2. Gas-grain reactions
low dust-to-gas, high water abundance high dust-to-gas, low water abundance Lombaert et al. 2012
OH127.8+0.0
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- 2. Gas-grain reactions
low dust-to-gas, high water abundance high dust-to-gas, low water abundance Lombaert et al. 2012
OH127.8+0.0
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- 2. Gas-grain reactions
Lombaert et al. 2012
OH127.8+0.0
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- 2. Gas-grain reactions
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- 2. Gas-grain reactions
IK Tau – HIFI + ground-based observations
Decin et al. 2010
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- 2. Gas-grain reactions
O-rich AGB stars: HIFI observations
Justtanont et al. 2012
v=v0+(ve-v0)[1-E0/E]β vturb?
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- 3. Photodissociation and ion-molecule reactions
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- 3. Photodissociation and ion-molecule reactions
Warm water in the sooty
- utflow of the luminous
carbon star IRC+10216
Decin et al. 2010, Nature
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- 3. Photodissociation and ion-molecule reactions
(Decin et al. 2010, Neufeld et al. 2011)
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- 3. Photodissociation and ion-molecule reactions
Melnick et al. 2001
sublimation
- f
icy bodies
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- 3. Photodissociation and ion-molecule reactions
H2O: shock-induced chemistry vaporization of icy bodies grain surface reactions radiative association O+H2
(Melnick et al. 2001) (Willacy 2004) (Agundez et al. 2006) (Cherchneff 2006)
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- 3. Photodissociation and ion-molecule reactions
Weigelt et al. 2002
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- 3. Photodissociation and ion-molecule reactions
Weigelt et al. 2002 Cherchneff 2011
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- 3. Photodissociation and ion-molecule reactions
Weigelt et al. 2002 Mamon et al. (1999, 2000), Leao et al. 2006
arcs from 4” to 80”
100 mas
IRC+10216
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- 3. Photodissociation and ion-molecule reactions
Weigelt et al. 2002 Mamon et al. (1999, 2000), Leao et al. 2006
arcs from 4” to 80”
100 mas
Herschel PACS
70 μm 100 μm 160 μm
Decin et al. 2011
10' x10' IRC+10216
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- 3. Photodissociation and ion-molecule reactions
Weigelt et al. 2002 Mamon et al. (1999, 2000), Leao et al. 2006
arcs from 4” to 80”
100 mas
Herschel PACS
100 μm
Decin et al. 2011
arcs from 23” to 320”
influence gas-phase chemistry IRC+10216
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- 3. Photodissociation and ion-molecule reactions
I R A M H E R S C H E L C2H in IRC+10216 (De Beck et al. 2011) C2H2+hν C2H+H
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- 3. Photodissociation and ion-molecule reactions
C2H in IRC+10216 (De Beck et al. 2011) without density enhancements including density enhancements
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- 4. CSM-ISM interaction
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- 4. CSM-ISM interaction
CW Leo PACS 160 μm 16' x 11'
CSM-ISM interaction region at ~450 – 480”
(Ladjal et al. 2010)
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- 4. CSM-ISM interaction
blue: PACS 70 mic; green: PACS 160 mic; red: SPIRE 250 mic
Decin et al. 2012
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- 4. CSM-ISM interaction
Cox et al. 2012
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Fermata Eyes Rings Irregular
#22 #6 #14 #6
53 out of 81 objects show interaction!
- 4. CSM-ISM interaction
Morphological Classes
Cox et al. 2012
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- 4. CSM-ISM interaction
BASIC MODEL higher v higher Mdot higher TISM low ISM density low dust content
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- 4. CSM-ISM interaction
Hydrodynamical simulations: Kelvin-Helmholtz & Rayleigh-Taylor instabilities
Large scale 'KH' vortices downstream
New hydro code: AMRVAC (Van Marle et al. 2011)
Turbulent instabilities
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- 4. CSM-ISM interaction
gas density gas velocity gas temperature ρwind / ρtotal
Hydrodynamical simulation
Decin et al. 2012
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