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GAS FLOW AND GENERATION OF X-RAY EMISSION IN WR+OB BINARIES
Pages 394-402

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From page 394...
... X-ray emission is caused by gas heating up to temperatures of 107-108 K behind the front of shock waves. These are formed in the collision of gas flowing out from the WR star with either the OB star's surface or the gas of the OB star's wind.
From page 395...
... the winds flowing out of WR and OB stars can collide. ~ estimate approximately the distances row and row from WR or OB stars, respectively, to the region where these winds meet, it is necessary to put dynamical gas pressures of both winds equal to each other: PwR(rwR)
From page 396...
... the undisturbed gas stream in the vicinity of an OB star can be assumed plane-parallel. For WR + OB binaries and with Apical parameters of WR stars (I'm = 108 cm/s, M = 10-5 M/year, D = 10~3cm, the stellar wind gas temperature T = 105 K)
From page 397...
... here N+ = p/mpA is the concentration of nuclei N+ = N+Z Is the concentration of electrons; A is the atomic weight; Z is their electrical charge; k is the Boltunann's constant; mp is the proton mass; ~ = A/~1+Z3 is the mean molecular weight; ~ is the ratio of heat capacities with the constant pressure and the constant volume, equal to S/3 for the rarefied totally ionized plasma. Helium predominates in the gas of the WR stellar wind.
From page 398...
... . With a distribution of p and T lmown behind the shock front it is easy to find the spectral power of the bremsstrahlung of the gas heated in the shock
From page 399...
... emission of rather wide binaries WR + OB (roB ~ ray. The stellar wind of a WR star Is much more powerful Ban that of an OB star (WRY v(WR)
From page 400...
... With these values Mown we also got the total and spectral powers of the hot gas bremsstrahlung. This emission spectrum shape turned out to be close to that described by equation (15~.
From page 401...
... it is evident that rO6 coincides with (2) derived above, i.ee, the allowance for the WR star wind deceleration does not change the position of the stagnation point of the contact surface.
From page 402...
... ~ 108 cm/s. Thus, the allowance for the deceleration of the gas of the WR star's stellar wind in the O star's vicinity can lead to gas velocities ahead of the shock front equal to about (0.5 to 1)


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