


7/30/08  Go back and analyze the Helike lines in ε Ori and ζ Ori.  Still looking up phi ratios. 
7/22/08  Analyze some of zeta Pup's weaker lines.  link 
7/22/08  Fit the entire spectrum of zeta Pup with the same u0 and either the same taustar, or a taustar scaled with the opacity.  link 
7/11/08  Check Xi Persei's and 9 Sgr's spectra. 
9 Sgr is more promising than ξ Per: ξ Per. 9 Sgr. Update 7/30: 9 Sgr is actually pretty interesting: revisions to the massloss rate 
7/9/08  Check Cyg OB2 8A's spectrum.  Cyg OB2 8A's lines, as presented in Waldron et al. 2004, don't look that shifted to me. link 
7/9/08  Analyze τ CMa's spectrum and/or 15 Mon's spectrum.  Weak spectra, but I can work with them. Spectra are up: τ CMa. 15 Mon. 
7/9/08  Analyze HD93129AB's spectrum.  Working on it: link 
7/9/08  Analyze HD150136's spectrum. 
HD 150136 is CWB, so there may be more going on here than a simple wind shock model can fit. I'm getting taustar values < 0.1 for this source. link This is a lowpriority source. 
7/9/08  Analyze ζ Ori's spectrum.  link 
6/25/08  Fit an isotropic porosity model to the spectrum, starting with the strongest lines 
OVIII 18.9689 FeXVII 15.014 NeX 12.1339 OVIII 16.006 OVII 21.6015 
6/23/08  Fit the strongest lines with vinf=1910 
OVIII 18.9689 FeXVII 15.014 NeX 12.1339 OVIII 16.006 
6/23/08  Make fake data sets from wind profile models with taustar = 1 & 3 and u0 = 0.9, 0.8, 0.7, 0.6, & 0.5. Refit the fake data to see if the original models are found.  link 
6/23/08  Fit Eps. Ori's entire spectrum with an APEC model to find its temperature. To do this, first rebin the spectrum with a minimum number of counts/bin so that the continuum has less bins than the lines.  Data rebinned with minimum counts of 50 and 100. APEC gives ~.25 keV temperature, but the fits have rejection probabilities of 100%. 
6/23/08  Once the temperature of Eps. Ori's xray producing plasma is known, check the highresolution APEC model to see if the FeXXIII line at 12.161 angstroms is contaminating the NeX line at 12.1339 angstroms.  Postponed until better temperature model is obtained. Assume that there is no contamination. 
6/23/08  Once the temperature of Eps. Ori's xray producing plasma is known, use the highresolution APEC model to find the ratio of the FeXVII lines at 17 angstroms to each other and the line at 16.78 angstroms. Using these ratios, fit the three lines together. 
Instead of finding the ratio for a specific temperature, I tried several different ratios for the two lines at 17 angstroms: link Entire line complex, with normalization ratios as free parameters: link 
6/23/08  Once the temperature of Eps. Ori's xray producing plasma is known, use the highresolution APEC model to find the ratios of Lyman alpha lines to Helium beta lines to find the ratio between the NVII and NVI lines at 24.781 angstroms.  Lost cause. 
