Pierre Bergeron - Los Alamos National Laboratory
Transcript of Pierre Bergeron - Los Alamos National Laboratory
White Dwarf Atmospheres
Pierre BergeronUniversité de Montréal
Sirius B
What is a stellar atmosphere?
What is a stellar atmosphere?
Atmosphere
Input parameters
• Effective temperature (Teff)
• Surface gravity (log g)
• Atmospheric composition (NHe/NH, Z)
• Rotation
• Magnetic field
• Mass loss
« If the Sun did not have a magnetic field, it would be as boring a star asmost astronomers believe it to be »
(attributed to R.B. Leighton)
center surface
Basic structure
center surface
Basic structure
Gilles
Fontaine
Photosphere
H conv
He conv
P/g 270 km for the Sun
What are white dwarfs showing us ?
80% are DA stars 20% are «non-DA stars»
DB
DA
DB
DA
Gravitational settling
Magnetic White Dwarfs
Basic Atmospheric Equations
H : Radiation (Eddington) Flux
Opacity calculations cross-section + population calculations
bound-bound transition
bound-free transition
free-free transition
scattering
Population calculations
• Local Thermal Equilibrium (LTE) Saha / Boltzmann
• Non-local Thermal Equilibrium (NLTE) Statistical equilibrium equation
• Equation of state (ideal gas, but not always…)
H b-f
H f-f
H–
H+2 f-f
e-scat
+ hydrogen lines
(Stark broadening)
H–
H+2 f-f
H b-f
H2– f-f
H f-f
H– b-f / f-f
H2– f-f
H2 collision
induced opacity
Temperature structure Emergent (Eddington) flux
Boundary conditions for stellar interior models
Measuring atmospheric parameters using model atmospheres :Spectroscopic technique
NLTE
convective
Flux calibration is difficult…
Flux calibration is difficult…
Balmer line profiles are sensitive to both Teff and log g
Balmer line profiles are sensitive to both Teff and log g
Stark broadening
atomic level destruction
i
Hummer-Mihalas occupation probability formalism
j
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j
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Hummer-Mihalas occupation probability formalism
j
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j
photoexcitation(bound-bound opacity)
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j
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photoionisation(bound-free opacity)
κ
e−
wj
wj ››
wj ‹‹
occupationprobability
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Hummer-Mihalas occupation probability formalism
j
i
j
photoexcitation(bound-bound opacity)
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j
i
photoionisation(bound-free opacity)
κ
e−
wj
wj ››
wj ‹‹
occupationprobability
Spectroscopic technique used for measuring Teff and log gσ(Teff) = 1.2 % Teff σ(log g) = 0.038 dex
log g converted into mass using the mass-radius relation for WDs(mechanical structure provided by degenerate electrons)
log g ~ 8
Smallerradii !
log g converted into mass using the mass-radius relation for WDs
Mass and log g distributions of 770 DA stars
Chandrasekhar mass ~ 1.36 M⊙
Chandrasekhar mass ~ 1.36 M⊙
electronsbecome
relativistic
ZZ Ceti stars + photometrically constant white dwarfs
Mass distribution as a function of Teff
DA stars from the SDSS / DR4
high-log g problem
Mass distribution as a function of Teff
DA stars from the SDSS / DR4
high-log g problem
Application to DB (helium-line) white dwarfs
Application to DQ (carbon-line) white dwarfs
Application to DZ (metal-line) white dwarfs
Application to hot DO (helium-line)
white dwarfs
Application to DC (featureless!) white dwarfs
Stellar flux integrated over filter bandpasses (magnitudes)
http://www.astro.umontreal.ca/~bergeron/CoolingModels/
http://www.astro.umontreal.ca/~bergeron/CoolingModels/
For Dummies
Photometric method
fλ = π (R/D)2 4Hλ
Hλ = Hλ(Teff , log g)
D = 1 / π
g = GM / R2
M-R relation for WDs
Hybrid spectroscopic and photometric approach
Application to «ultracool» white dwarfs
H2 collision-induced absorption (CIA)
DB gap
Cooling time →
G. Fontaine & F. Wesemael (1987, 2nd conf. on Faint Blue Stars)
DB gap
Cooling time →
Evidence for the spectral evolution of white dwarfs
H → HeHe → H
G. Fontaine & F. Wesemael (1987, 2nd conf. on Faint Blue Stars)
He
H
Photosphere
He
H
DO DA
Photosphere
Requires only10-16 M
of
hydrogen
Photosphere
HeII conv
HeI conv
Photosphere
HeII conv
HeI convH
He
Convective dilution DA DB
Photosphere
H conv
Photosphere
H conv
H
He
Convective mixing DA ???
Photosphere
H conv
H
He
Convective mixing DA ???
Photosphere
H conv
H
He
Convective mixing DA ???
Origin of carbon in DQ stars
Helium convection zone
Helium convection zone
Carbon core (diffusion tail)
Helium convection zone
Carbon core (diffusion tail)
Carbon in DQ stars is being dredged up from the core
The Z in DZ stars !