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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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