## A generalized version of the Rankine-Hugoniot relations including ionization, dissociation, radiation and related phenomena
^{1} Laboratory for Space Research, Sorbonnelaan 2, 3584 CA, Utrecht, The Netherlands^{2} Astronomical Institute, Princetonplein 5, 3584 CC, Utrecht, The Netherlands^{3} Center for Space Plasma, Aeronomy, and Astrophysics Research, University of Alabama in Huntsville (UAH), TH S101, Huntsville, AL 35899, USA ^{4} Armagh Observatory, College Hill, Armagh BT61 9DG, Northern IrelandAstron. Astrophys. In Eq. (6) on page 196 a minus sign should be introduced, so that Eq. (6) reads or, alternatively, should be replaced by . Here is the velocity behind the shock (usually positive), and is the velocity in front of the shock (usually negative). In this case we assumed with being the amplitude of the flow speed. This assumption corresponds to a symmetric sawtooth-type shock. In this case Eq. (5) follows directly from Eq. (6). In the general case, the LHS of the above given equation should read . The modified version of the Rankine-Hugoniot equations (see Sect. 2) is however not affected by this assumption. © European Southern Observatory (ESO) 1999 Online publication: March 1, 1999 |