... spectra

Based on observations by the International Ultraviolet Explorer collected at the Villafranca Satellite Tracking Station of the European Space Agency, on observations made by the Hipparcos Astrometry Satellite, and on ground-based photometric and spectroscopic observations made at the European Southern Observatory, La Silla, Chile.

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...

Figures 4-9, 33-40 and 45-110 and Appendices A-G are only available in electronic form at http://www.edpsciences.org

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... range

Except for ${\rm BD{+09}}^{\circ }{880}$ and HD 100546, which needed higher values to match the calculated spectrum properly to the observed spectrum, since $M_{\rm v}$ and dare well-defined and leave no freedom to the other model parameters.

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... UXORs

After Herbst (1994) and Eaton & Herbst (1995), see also Sects. C.3, C.7, C.16, and C.25.

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...

The numbers in Col. 3 refer to the IUE images used for the observed spectrum (Appendix F). The spectral types in Cols. 4 and 5 refer to those used for the photosphere and boundary-layer (Appendix G). Labels ¹ and ² are used to distinguish comparison stars with the same ST. Column 7 gives the foreground colour excess used to de-redden the observed spectra. Labels ³, ⁴, and ^z in Col. 9 indicate $M_{\rm v}$-values for LC  III, IV, and ZAMS instead of the value from SK82 corresponding to the ST in Col. 4 in the case that there were no comparison spectra of the required LC available. The Cols. 15 to 17 give the relative flux contributions ( $F_{\rm rel}$ in the $V^{\rm J}$-band from photosphere, BL, and disc (Eq. (9)). $\aleph$ is the normalisation factor from Eq. (13). $M_{\star}$, $L_{\star}$ and $t_{\star}$ have been obtained from the Bernasconi tracks (1996), and the mass accretion rate $\dot{M}$ is calculated from the model parameters assuming i=90$^\circ$ (Sect. 6). The $\dot{M}$-value corrected for $v \sin i$ (only if i is known) is given in Col. 24, if, however, the star is seen "pole-on'', i.e. $i\leq20\hbox{$^\circ$ }$, this value was not estimated and is given as (-).

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... SU Aur

The calculated SED of SU Aur is similar to that in BBB88.

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... 1988

In collaboration with dr. A. Brown & dr. J. L. Linsky.

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... disc

Although for the A and F stars the direct flux contribution from the disc is negligible in the wavelength range of IUE, for i < $90\hbox{$^\circ$ }$ the shadow of the disc on the stellar surface affects the result of the calculated spectrum, hence the name "UV3C'' for our analyses (also there is no BL possible without a disc).

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... 211

Proceedings 1st Conference on the Nature and Evolutionary Status of Herbig Ae/Be Stars, Amsterdam 26-29 October 1993, ed. P. S. Thé, M. R. Pérez, & E. P. J. van den Heuvel.

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... obtained

In collaboration with dr. C. Catala, dr. F. Praderie & dr. T. Simon (Catala et al. 1989).

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... nebulosity

Note that deWinter & Thé (1990) obtained d=300${\rm pc}$ for A5 III, because they assumed $V^{\rm J}_{\rm max}$=10 $.\!\!^{\rm m}$32 for KK Oph.

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