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5 PUBLICATIONS of VARIABLE STAB SECTI ROYAL No. 10 (C82) 5 1 1 F FIGURE 5 PUBLICATIONS of VARIABLE STAB SECTI 1 ROYAL ASTRONOMICAL SOCIETY OF NEW ZEALAND to // - X i o Q 5 s2 -t- T T T 10 GU ill SGR Director: Frank M. Bateson P.O. Box 3093, •'•'J GREERTON, TAURANGA, NEW ZEALAND. I wm n XX /3 CONTENTS PAGE THE LIGHT CURVE OF V348 SAGITTARII 1954 June 22 to 1981 October 31. Frank M. Bateson & A.W. Dodson 1 PHOTOELECTRIC PHOTOMETRY OF TY VELORUM & SOME NEARBY STARS Brian F. Marino & W.S.G. Walker 10 OUTBURSTS OF SOME SOUTHERN DWARF NOVAE—PAPER 3. Frank M. Bateson 12 OBSERVATIONS OF SOME SOUTHERN DWARF NOVAE—PAPER 4. Frank M. Bateson 24 PHOTOELECTRIC PHOTOMETRY OF V532 CENTAURI & SOME NEARBY STARS Brian F. Marino & W.S.G. Walker 46 PHOTOELECTRIC PHOTOMETRY OF NOVA CORONAE AUSTRINAE 1981 48 W.S.G. Walker & Brian F. Marino VISUAL OBSERVATIONS OF THE IRREGULAR VARIABLE RX Leporis 51 Frank M. Bateson & C.W. Venimore PHOTOELECTRIC OBSERVATIONS OF THE 1981 SUPERNOVA IN NGC 1316 53 W.S.G. Walker & Brian F. Marino PHOTOELECTRIC PHOTOMETRY OF NOVA RR PICTORIS CSV 6467 AND SOME NEARBY STARS 55 Brian F. Marino & W.S.G. Walker THREE COLOUR PHOTOMETRY OF THE STAR AM CORONAE AUSTRINAE 60 Brian F. Marino & W.S.G. Walker REVISED PERIOD FOR V384 CARINAE 61 Colin W. Venimore VISy/L OBSERVATIONS OF CSV 6467 = NSV 03043—1970 to 1982 63 Frank M. Bateson & Colin W. Venimore REPORT OF VARIABLE STAR SECTION, ROYAL ASTRONOMICAL SOCIETY OF NEW ZEALAND FOR YEAR ENDED 1982 DECEMBER 31 65 PUBLISHED BY ASTRONOMICAL RESEARCH LTD., ! P.O. BOX 3093, GREERTON. TAURANGA, NEW ZEALAND. T 1. THE LIGHT CURVE OF V348 SAGITTARII 1954 June 22 to 1981 OCTOBER 31. Frank M. Bateson (1) & A.W. DODSON (2) (1) Director, Variable Star Section, R.A.S.N.Z. (2) Member, Variable Star Section, R.A.S.N.Z. SUMMARY. A light curve, derived from 2,417 visual observations by members of the V.S.S., R.A.S.N.Z., is presented covering the interval 1954 June 22 to 1981 October 31. Data on twenty-one minima are tabulated and discussed. The mean decline time is nine days and the mean rise time 27 days. The minima and their duration have a random distribution. 1. INTRODUCTION. On the basis of its light variations and spectrum V348 Sgr is termed unique with a photographic range of 10.6 to 17.(1). Hoffleit (2) examined over 500 Harvard patrol plates. She found that between J.D. 2,417,500 and 2,425,000 the light curve appeared to confirm the previous classification of V348 Sgr as of the R CrB type. However, she found that earlier and later observations showed the star more often at minimum than at maximum with little resemblance to R CrB type variations. The observations from J.D. 2,425,000 to 2,429,500 suggested a semi-regular variation with cycles of 200 to 400 days. Herbig (3) stated that V348 Sgr shows recurrent maxima with a mean spacing of about 200 days, at which times the star brightened from m -17 to about mag• nitude 11. The rise seems usually to take 30-60 days witfv'the subsequent decline being very much faster. Herbig also reported on the spectrum and the nebulous envelopes close to the star. He suggested that the general features of the light curve could be explained by the ejection of an opaque shell and its subsequent disolution.. V348 Sgr(4) was shown to have an infra=red excess and to be a hydrogen-deficent and carbon-rich object. It was considered to be closely related to the R CrB variables. 2. OBSERVATIONS. At the suggestion of G. JHerbig observations of V348 Sgr were commenced by A.F. Jones on 1954 June 22. Until 1969 May 23 he was the only observer, but after that date observations were contributed by other members of the Variable Star Section, Royal Astronomical Society of New Zealand. Table 1 shows the number of observations contributed by the observers. TABLE 1. TOTAL OBSERVATIONS CONTRIBUTED BY OBSERVERS. CRAGG, T.A. 25 JONES, A.F. 1,799 JONES, M.V. 148 MATCHETT, V.L. 37 OVERBEEK, M.D. 145 ROWE, G. 41 TAYLOR, N.W. 45 WILLIAMS, P. 119 13 observers with) less than 15 ) obsservations each) 58 TOTAL 2,417 2. All observations were made visually. Charts and a sequence have been published (5) . 3. LIGHT CURVE The normal observing season is from mid-February to mid-November, although in some years observations did not commence until late March. The light curve, shown in Figures la to le, is arranged in calendar years so that the results for each observing season is shown separately. The threshold of most instruments used was around 14.0 . As a result no information can be given on the star's be• haviour below tKis limit. In some years V348 Sgr was always(e.g. 1965,Fig.lb), or mainly (e.g. 1959, Fig.la) below this threshold.The light curve is from 10 day means. 4. RESULTS Data on the declines of V348 Sgr are summarised in Table 2. Each decline has been given a number, which appears in the first column of the table. The second column gives the last observation at maximum prior to the decline with the J.D. in this column and the visual magnitude in the third column. The fouith column shows the J.D. when V348 Sgr reached 14.C on the decline. The fifth column gives the J.D. when the star reached 14.0 on the rise and is followed in the next column by the time, in days, that V3$B Sgr was fainter than 14.0V. The seventh column shows the time, in days, that V348 Sgr took to fade from the magnitude in the third column to 14.0, The next three columns show the intervals, in days, vetween successuve dates when the variable reached 14.0 on the decline; between successive points at 14.0 on the rise, and the interval between 14.0 on the rise and the following 14,0 on the decline. The final column gives the rise time, in days. That corresponds to the time taken to increase from 14.0 to maximum at 11-7 to 12.3. When the star did not fully recover from a minimum no figure appears in the final column. 5. DISCUSSION. For the purpose of this discussion maximum brightness of V348 Sgr falls between 11.6 and 12.3, whilst when it declines below 14.0 it is treated as a decline to minimum. The variable, during the intervals reported in this paper, spent about 45% of the time fainter than 14.0 and 55% brighter than this limit. The star did not always recover after a minimum to full maximum brightness but oscillated between 12.7 and 14.0 for long periods. The decline times from maximum to 14.0 ranged from 2 to 4^ days. Minimum No. 12 was unusual in having both a much slower decline and slower rise than normal.. Omitting minimum No. 12 and those for which the dates in Table 2 are uncertain, the mean decline time for 15 minima is 9 days. In 9 cases the rise time from 14.0 to maximum can be reasonably well determined. They range from 8 to 50 days with a mean of 27 days. For most of the remaining rises the variable did not recover to maximum brightness. The time that V348 Sgr remained fainter than 14.0 ranged widely from one minimum to another being from 14 to 670 days. The intervals between successive phases of the light curve appears to be entirely random. The decline rate showed no definite relationship with the time spent at minimum. There is an indication that the shorter the interval spent at minimum the steeper was the subsequent rise to maximum. This might be due to the variable at such times not falling far below 14.0 but no information can be offered on this point. The light curve certainly, at times, shows many features common to variables of the R CrB type, e.g. steeper declines than rises; random distribution of minima and long intervals oscillating around maximum brightness. On the other hand the time spent at an intermediate magnitude is much longer than R CrB variables. At times the variable shows an irregular variation, with amplitudes of from one magnitude to 0m2. This amplitude is greatest when the star is between 13.0 and 14.0 and least when it is at maximum. No period could be found for these variations. 6. CONCLUSIONS The light curve reveals so many features that are closely akin to those seen in R CrB stars that we conclude that this variable is related to that class. The variable spends 45% of the time at, or near, minimum brightness and 55% of the time at maximum or at an intermediate magnitude between 12.7 and 14.0. In that respect it differs from R CrB stars, but its steep falls; less rapid rises and the random distribution of minima resembles R CrB variables. There is no reason to doubt that the rapid falls and more leisurely rises would also operate in the lower part of the curve beyond the limit of the instruments used. He urge those members of the V.S.S., R.A.S.N.Z. equipped with instruments capable of reaching 15.0-16.0 magnitude to observe V348 Sgr more often.
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