1. Effects of porosity on emergent synthetic spectra of Massive stars in the X-ray domain Effects of porosity on emergent synthetic spectra on emergent synthetic spectra of Massive stars of Massive stars in the X-ray domain in the X-ray domain

2. Nucleosynthesis after O Stellar winds thousands km/s Stellar formation Galactic winds Supernovae, GRBs Chemicla Enrichment M>8 M ⊙. 20000K< T <100000K 10^5 L ⊙ < L < 10^6 L ⊙ Mdot=10^-4 M ⊙ /yr What is a massive star? Why we study them?

3. X-ray emission sources The “standard model” assumes that the X-ray emission is produced by radiatively cooling hydrodynamic shocks embedded in the acceleration zone of the stellar wind and that develop from the instability of radiatively driven mass- loss. ● A few O-type stars known to have a (rather) strong magnetic field, are likely to have their stellar wind confined into the equatorial plane of the magnetic field (e.g. θ 1 Ori C, Gagné et al. 2005, ApJ 628, 986, τ Sco, Mewe et al. 2003, A&A 398, 203). Their X-ray spectral lines are narrower and their emission is brighter and harder.

4. Evidence of Clumping Observational evidence of strong inhomogeneity: stochastic variable structure distribution of HeII 4686-A emission line in ζ Pup is explain by an excess emission from wind clumps,Eversberg, Lépine & Moffat (1998)‏ Variability of Hα of O-type supergiants explain by broken shells, Markova et al. (2005)‏ OV and NIV profiles and abondance of phosphorus fitting only with clumping in the CMFGEN code, Bouret et al. (2005)‏ Attenuation of Xray in O stars δ Ori (Miller et al. 2002) and ζ Pup (Kramer et al. 2003) is smaller than expected in homogenous winds The composition of interclump medium: Void in a first time Few percentage of homogeneous matter (Zargo et al 2009 ) in the most recent version of radiative transfer code.

5. Massive star: - Radius Modelisation of a synthetic spectrum

6. Massive star -radius Stellar winds: -mass loss rate -velocity law: v(r)=vinf(1-R*/r)^beta vinf=terminal velocity Modelisation of a synthetic spectrum

7. Massive star -radius Stellar winds: -mass loss rate -velocity law: v(r)=vinf(1-R*/r)^beta vinf=terminal velocity -fragmentation of the wind -composition of the interclumps medium (void, % of homogeneous matter)

8. Massive star -radius Stellar winds: -mass loss rate -velocity law: v(r)=vinf(1-R*/r)^beta -fragmentation of the wind -composition of the interclump medium Geometric of the plasma -starting -size Modelisation of a synthetic spectrum

9. Massive star -radius Stellar winds: -mass loss rate -velocity law: v(r)=vinf(1-R*/r)^beta -fragmentation of the wind -composition of the interclump medium Geometric of the plasma -starting of emission -size Theorical plasma spectra Emission Absorption by the wind Modelisation of a synthetic spectrum

10. Theorical spectra from Atomdb data Theorical spectra for a cell Emergent fux for one cell Emergent flux from the star Synthetic spectra of the star seen by the observator Volume and density of the cell Absroption by the wind Summation for all cells Convolution by an instrumental matrix response Modelisation of a synthetic spectrum Emissivity N(H)*N(e)*dV h ≡ l/f

11. Impact of fragmentation on a single X-ray Factor 10 between maxima of intensity of an homogeneous wind and the most porous wind model need to decrease mass lost rate of massive star in clumped model to reproduce observation

12. Impact of porosity on a X-ray spectrum Absorption less important in the low energies In green h=0. In red h=0.05 In black h=0.1 kT=0.2keV

13. A new captor based on surface plasmons resonance -Absorption of a photon by the green medium -Bending of the cantilever -Dimunition of the gap between the cantilever and the prism -Modification of the plasmon surface resonance proprietes -Variation of the reflectivity of the prism -Variation of the intensity of the reflected laser light -Determination of the X-ray proprietes Épaisseur du gap Angle d’incidence

14. Surface plasmon resonance dectector caracteristics Astrophysic caracteristics: -0.1 to 10 keV energy band -high energie resolution=1eV -high spatial resolution -short readout Instrument contraints: -high sensiblility to Xray matter (Si or Bi) -low temperature (1K) (termal noise!) -small detector (10nm*10nm)()not a problem a priori) -1 ms (not a problem) COST

15. Future Code evolutions: -creation of a database -insertion of the interstellar medium absorption -convolution by differents instruments (currents and futures) -confrontation of yours models to observations Plasmon surface resonance detector: -find best ratio (energy resolution)/(instrument cooling) -size and geometry of instrument and of each pixel -comparison to others methods on others instruments