Subject:
change to Sec. 5.4
From:
Skinner Steve <Stephen.Skinner@Colorado.EDU>
Date:
Tue, 15 Apr 2008 13:55:33 -0600 (MDT)
To:
David Cohen <dcohen1@swarthmore.edu>
CC:
Marc Gagne <mgagne@wcupa.edu>, Rich Townsend <rhdt@bartol.udel.edu>, Stan Owocki <owocki@bartol.udel.edu>, Steve Skinner <skinners@origins.Colorado.EDU>, Kimberly Sokal <Kimberly.Sokal@Colorado.EDU>


  David:

  In the revised draft I sent out yesterday, I
  mentioned the Cohen et al. 2006 zeta Ori paper
  in Sec. 1 but I forgot to mention it in
  the first par. of Sec. 4, where zeta Ori comes
  up again.

  I've now revised the first par. of Sec. 5.4
  to read as follows:

\subsection{Coronal Models and Late-Type Companions}

The existence of a thin X-ray emitting coronal zone
at the base of the wind was  invoked by Cassinelli \& Olson (1979)
to explain strong O VI, N V, and C IV lines
in some OB supergiants and Of stars. Waldron \& Cassinelli (2001)
have also proposed a composite model involving both wind shocks
and confinement of dense plasma in magnetic loops close to the star
to  explain the broad  emission lines detected in the O9.7 Ib star
$\zeta$ Ori, but Cohen et al. (2006) arrive at  a different
interpretation that does not invoke magnetic confinement.
Magnetic loop confinement close to the star strongly resembles
coronal models for late-type stars.
   -----------------

  Steve

















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     *                                                     *
     *  Steve Skinner                                      *
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     *  Center for Astrophysics and Space Astronomy (CASA) *
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