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X-rays from Massive Stars



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X rays from Massive Stars David Cohen Swarthmore College X ray spectroscopy of hot plasmas temperature density kinematics in stars charge state distribution in the laboratory B0 I O9 5 I horsehead O9 5 V B2 V O9 5 II B2 V Chandra grating spectra R 1000 300 km s 1 1 Ori C 1 Ori C hotter plasma narrower emission lines Pup Pup O4 I cooler plasma broad emission lines 1 D rad hydro simulation of an O star wind with Stan Owocki U Del Radiation line driving is inherently unstable shock heating and X ray emission Empirical X ray Line Profile Model for Data Fitting brightness Contours of constant optical depth observer is on the left blue red wavelength continuum absorption in the bulk wind preferentially absorbs red shifted photons from the far side of the wind Chandra grating spectrum of Pup Fe XVII line at 15 014 vinf literature mass loss rate o vinf best fit low mass loss rate Mass loss rate is reduced by factor of 4 Laser fusion ICF exps and modeling OMEGA Laser U Rochester Laboratory Astrophysics Sandia Nat l Lab Z Machine Benchmarking photoionized plasma spectra Laboratory Astrophysics Swarthmore Spheromak Exp SSX Characterizing magnetic reconnection heating Swarthmore s on the R3 Maybe you d like to visit and talk about xrays plasma and hot star winds this summer



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