spectroscopy & variable stars · 2016-06-20 · why studying variable stars ? large domain of...
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Spectroscopy & variable stars
Philippe Mathias – IRAPOMP-UPS
Variable star classification
Linear pulsation
Why studying variable stars ?
● Large domain of physical conditions● Probing of the stellar structure● Constrains on stellar evolution● Various excitation mechanisms● Atmospheric dynamics● Period-luminosity law(s)● ...
Real-time Laboratories
Stellar pulsation
● Conservation equations : mass, impulsion,energy
● Energy generation (core)
● Energy transport mechanism(s)
● Equation of state
System of coupled differential equations
Start from hydrostatic equilibrium
Perturbation : ρ=ρo+δρ
Pulsating stars HRD
R ρ
P ~ ρ-1/2
What to get ?
Linear pulsation
● Small amplitude motion : linearisation● Displacement of the form :
ξ (r ,θ ,ϕ , t)=ξnlm (r)Y ml(θ ,ϕ)exp(iσnlm t)
NRP & Doppler shifts
Vogt & Penrod 1986
Synthetic Line Profiles
Theory vs. observations
l=0 l=1,m=1 l=2,m=-1Telting et al. 2008
m: only spectroscopy
Spectral resolution
Effect of rotation
● Dependent on the inclination angle : i
Rotation broadening
Role of rotation
l=4, m=0 l=7, m=-7 l=9, m=3
Better pixel sampling
➔ Blends to be taken into account➔ Requires higher S/N
Phase smearing
P/1 P/10 P/30
Exposure time below ~ P/10
Residual spectra
● LPV evidences
Often multiperiodicities
Long term observationsrequired
Rayleigh criterion :∆T > beat periodS
Kochukhov 2006
Multiperiodicities & LFT
Uytterhoeven et al. 2001
Multisites campains
OHP + KPNO
Zero point equalization
● Requires radial velocity standards (e.g. from planets search surveys
From LPV to ∆R, RV & a variations
Mathias et al. 1991
Atmospheric dynamics
Line profile to velocity measurements
● Pixel minimum, gaussian fit, line bissector, 1st moment...
Line profile to velocity measurements
● First moment adapted to one-layer motions, e.g. NRP
v n=∫ vn f (v)dv
Line forming region
Wave propagation
α v α v2 α ev
Velocity gradient
Albrow & Cottrel 1995
Asymmetry & convection
Line asymmetries
Nardetto et al. 2006
Line doubling : Schwarzschild (1952)
Mathias et al. 1998
Line doubling and velocities
Fokin et al. 2004
Multiple doublings ?
Mathias et al. 2006
Velocity differences● Progressive waves, but difficult interpretation
Stankov et al. 2003
Contribution functions
The Van Hoof effect
● Exist in many types of pulsating stars➔ Atmosphere stratification➔ Time delay : progressive wave velocity
α Lupi RR Lyrae
Mathias & Gillet 1993 Mathias et al. 1995
Correlation profiles
Importance of the mask
● Red/dash: FeI only
Josselin & Plez 2007
Correlation profiles : tomography
● Z Oph, φ=0.08
Alvarez et al. 2011
RP & NRP in Cepheids ?
● Or binarity, or shocks...
Kovtyukh et al. 2003
Spectroscopic binaries
P = 134.9 de = 0.68K = 38 km/sM1/M2 = 1.11
Mathias et al. 2004
Composite spectra
Mathias et al. 2004
Emission associated to shocks
Kovtyukh et al. 2011
Monitoring of Be stars
● Circumstellar envelope● Variability at different time scales
Rivinius et al. 2001
Doppler imaging
Image reconstruction
Wade et al. 2010
Conclusions
● « Amateur » spectroscopy towards professional standards (R~20000)
● Long runs difficult for « professional » but essential for a better comprehension, discrimination of physical phenomena...
● Coordinated campains possible● Low S/N partially(?) compensated through
CCFs● Many subjects of interest : NRP, RP, Be,
binarity, ... for stellar/pulsation parameters...