In this paper preliminary results are presented based on a study of the low and high resolution ultraviolet spectrum of the peculiar supergiant ( post-AGB star ) HD 101584 .
By a comparison of the low resolution spectrum ( 1200 - 3200 { ~ { } \AA } ) with standard stars , the star is classified as an A7I , indicating an effective temperature of 8150 K , where literature quotes spectral type F0I .
The Doppler shift of the FeII absorption lines in the high resolution spectrum ( 2500 - 3000 { ~ { } \AA } ) show a relation with the line optical depth .
This suggests an expanding accelerating wind , c.q .
pseudo-photosphere .
The relation is extended by a factor 10 ^ { 5 } in optical depth by using available data from optical HeI and NI lines .
The relation suggests that the radial heliocentric velocity of the star is at least 54.5 { ~ { } km~ { } s ^ { -1 } } .
From the { H } \alpha line a velocity of 96 { ~ { } km~ { } s ^ { -1 } } is measured for the terminal velocity of the wind .