Photometry of the eclipsing system AR Pavonis.

UB V measures of the eclipsing symbiotic variable AR Pav are presented covering the years 1967 to 1973. By combining these results with those of Mayall an improved period of days is derived. A comparison of the eclipse curves when the star is bright and faint leads to a model similar to that of Thackeray & Hutchings with a secondary, filling its Roche lobe, losing mass to the primary. The primary is like a planetary nebula with a bright area, which may be responsible for the forbidden emission region, where the stream from the secondary falls on a ring around it. Eruption of the central star of the primary is invoked to cause an increase in size and brightness of the nebula in order to account for shortening of the duration of eclipse when the star is bright. There is also a change of phase of central minimum from when the star is faint.