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A STUDY OF ACCRETION DISK WIND EMISSION
Raul E. Puebla1
Marcos Perez Diaz1
D. John Hillier2
1IAG. Universidade de So Paulo. Brazil.2University of Pittsburgh. USA.
The Golden Age of Cataclysmic Variables and Related Objects
12th September, 2011
Palermo, Italy
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SIGNS OF WIND IN UV SPECTRA
P Cyg profiles of C IV,
N V or Si IV lines arean evidence of mass
loss from CVs.
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SIGNS OF WIND IN UV SPECTRA
Hartle et al. (2002)IX Vel (NL)
Blue shifted absorption profiles
Blue edges of absorption profiles up to 5000 km s-1
5000 km s-1
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SIGNS OF WIND IN UV SPECTRA
Low to intermediate
Inclination: Absorption to
P Cyg.
High inclination:
Emission profiles.
The line profiles are
strongly dependent on
the orbital inclination:
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THE DISK-WIND MODEL
v(z)
NLTECMFGEN
model
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THE DISK-WIND MODEL
WindWind
Photosphere
)(/)()( zrmzv
TLUSTY disk model
)()()()( rmzazvz
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THE DISK-WIND MODEL
l1110 A
dM/dt=10-8 Msunyr-1dM/dt=10-9 Msunyr
-1
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THE DISK-WIND MODEL
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TEMPERATURE STRUCTURE
Puebla et al. 2011
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TEMPERATURE STRUCTURE
Model e
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IONIZATION STRUCTURE
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MODEL RESULTS
dcba MMMM MnMw
1110
A
1yr
Accretion Rate Mass Loss
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MODEL RESULTS
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COMPARISON WITH UV DATA
RW Tri
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COMPARISON WITH UV DATA
RW Tri
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COMPARISON WITH UV DATA
V347 Pup
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COMPARISON WITH UV DATA
V347 Pup
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COMPARISON WITH MONTE-CARLO METHODS
Ion Structures
Noebauer et al. 2010,
Long et al. 2002 Puebla et al. 2011
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COMPARISON WITH MONTE-CARLO METHODS
Puebla et al. 2011
Noebahuer et al. 2010
The Monte-Carlo models
generate larger high ionizedregions. This bears stronger
lines for C IV and NV
RW Tri
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EFFECT OF ACCELERATION IN PHOTOSPHERE-
WIND INTERFACE ON LINES
Puebla et al. 2011
Acceleration in the photosphere-
wind interface has strong effects on photosphere lines
like C II (1335)
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CONCLUSIONS
The model treat the photosphere and the
photosphere-wind interface consistently
The model cannot treat the non-local
interaction between disk and wind
It is necessary to improve the models to
lead them to a at least 2D approximation
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