C. No. 18 (?992)

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PUBLICATIONS of 7 VARIABLE STAR SEQTI f ROYAL ASTRONOMICAL SOCIETY 1 1 OF NEW ZEALAND to to

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PUBLICATIONS OF THE VARIABLE STAR SECTION ROYAL ASTRONOMICAL SOCIETY NEW ZEALAND" No. 18 CONTENTS i & ii. INDEX iii. EDITORIAL 1. THE LIGHT CURVE OF RU PEGASI 1980 - 1992 F.M. Bateson, R. Mcintosh & D. Brunt 8. NOVA SCORPII 1992 - PRELIMINARY LIGHT CURVE Ranald Mcintosh 11. VISUAL OBSERVATIONS OF BL TELESCOPII Peter F. Williams 17. A POSSIBLE OUTBURST OF V4-30 CARINAE M. Morel 22. OBSERVATIONS OF THE TRANSIENT X-RAY SOURCE AO538-66 Frank M. Bateson 28. THE DISCOVERY OF NOVA PUPPIS 1991 Paul Camilleri 30. THE LIGHT CURVE OF NOVA PUPPIS 1991 Frank M. Bateson 32. TWO COLOUR SEQUENCE FOR 0525J52 TV COLUMBAE P.M. Kilmartin 33. THE SEMI-REGULAR VARIABLE RX LEPORIS Frank M. Bateson 37. THE FADING OF S DORADUS F.M. Bateson & A.F. Jones 41. OUTBURSTS OF THE DWARF NOVA IP PEGASI Frank M. Bateson ii

PUBLICATIONS OF THE VARIABLE STAR SECTION ROYAL ASTRONOMICAL SOCIETY NEW ZEALAND

No. 18 CONTENTS (cont.)

45o LIGHT CURVES OF SOME MIRA VARIABLES Ranald Mcintosh & Don Brunt 46. (a) S PICTORIS J.D. 2,426,800 - 2,448,775 Figs. 1 - 8 54. (b) T CENTAURI J.D. 2,425,450 - 2,448,680 Figs. 9 - 16 62. (c) RS SCORPII J.D. 2,427,240 - 2,448,475 FigSo 17 - 24 69 c (d) T GRUIS J.D. 2,427,700 - 2,448,728 Figs. 25 - 32 76. (e) S GRUIS J.D. 2,427,800 - 2,448,728 Figs. 33 - 40 83. (f) R INDI J.Do 2,431,368 - 2,447,000 Figs. 41 - 46 89. REPORT OF THE VARIABLE STAR SECTION, ROYAL ASTRONOMICAL SOCIETY OF NEW ZEALAND, FOR YEAR ENDED 31st December 1992. EDITORIAL

Recent issues of these publications have mainly been devoted to the publication of the results of close visual monitoring of dwarf nova because of the pro• fessional interest in knowing details of their outbursts. Such results are now almost up-to-date with the exception of those dwarf nova being discussed elsewhere.

We commence in this issue the publication of light curves of Miras and other variables based on decades of observation by members of the Variable Star Section, Royal Astronomical Society of New Zealand. These light curves will be continued in Publications Nos. 19 and 20 so that the curves are available to those interested. To conserve space the elements determined from these light curves will be then tabulated in one paper rather than given in separate papers with each set of light curves.

The Section is deeply indebted to our member, Don Brunt, for computer processing of the observations prior to 1st April 198? that had been maintained in ledger sheets by our former Recorder, the late Gordon Smith. This has enabled Ranald Mcintosh to produce the light curves, including observations after 1st April 1987, which he maintains with his well known efficiency. It is only the devoted co-operation and invaluable assistance of these two members that makes the publication of computer light curves possible. 1

THE LIGHT CURVE OF RU PEGASI, 1980 - 1992

Frank M. Bateson, R. Mcintosh s D. Brunt Variable Star Section, R. astr. Soc. of N.Z. P.O. Box 3093, Greerton, Tauranga, New Zealand.

SUMMARY: The visual light curve of the dwarf nova, RTI Pea, from 1979 Sent.23 to 1992 May 31 is reproduced.

1. INTRODUCTION

The visual light curve of RU Peg is shown in Figs.l - 6. The plotted points are from individual observations for the interval J.D. 2,444,100 (1979 Sept.23) to 2,448,774 (1992 May 31). This northern star is one for which the V.S.S. sends observations to the B.A.A. so that they can combine our results with theirs and discuss the com• bined results. The B.A.A. are having problems in bringing their data up to date, and, for this reason we publish our liaht curve so that members can see the results of their estimates but the full dis• cussion of the results are left to the B.A.A,

1. D. Howarth (1) discussed observations from 1927 to 1969. D.R.B. Saw (2) reexamined these results in his paper which also included the observations from 1970 - 79. He gave the mean cycle as 73.5 18.1 days. He stated that long and short maxima occur in about egual mumbers with anomalous maxima 13% of the total. The latter Saw defined as having a long, slow risewith a halt or reversal. He also classified as anomalous two faint maxima, one when the star remained fainter than llm0 with a long flat maximum,irrespective of the rate of rise, and, the other a short maximum with the stefcp barely reaching llm5.

2. OBSERVATIONS

All observations were made visually by members of the Variable Star Section, RASNZ using charts 563-5 and the visual sequence thereon. It should be noted that RU Peg has a close companion (magnitude 12.6). That is the usual minimum magnitude reported. Most observers have instruments capable of separating the two stars. However, it does appear that at times some observers have been unable to do so since there is clear evidence that often , when their estimates are at 12,6 other observers, with larger telescopes and dark skies estimated it around 13.1-13.2.

RU Peg is classified (3) as a dwarf nova, type UGSS+ZZ: with a range of 9.0 to 13.2. The very short/ low amplitude oscillations of ZZ Cet type would not be observable visually. Possibly the faint, short outburst Saw classified as anomalous may have been a flare as these occur in ZZ Cet stars, This suggestion, if correct, implies that the companion may be a flare star. At maximum RU Peg is rarely brighter than 10m0 and very infrequently reaches 9m5.

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RU Peg is unobservable between early January and mid-April which accounts for the breaks in the light curve.

ACKNOWLEDGEMENTS

We extend Our thanks to all observers for their estimates and especially to Danie Overbeek and Abby Jones who between them accounted for 65% of the observations,

REFERENCES

(1) Howarth, I.D. 1975. J.Brit.astron. Assoc.85, 271. (2) Saw, D.R.B. 1983. J. Brit, astron. Assoc. 93,70. (3) Kholopov,P.N. (Editor). General Catalogue of Var. Stars. Vol.Ill, 4th ed.Nauks, Moscow. 1987. 8.

NOVA SCORPII 1992 - PRELIMINARY LIGHT CURVE

Ranald Mcintosh Variable Star Section, RASNZ Unit 68, 36 McLeod Road, Henderson, Auckland 8, New Zealand

SUMMARY: A preliminary light curve of Nova Sco 1992 from J.D. 2,448,766 to 2,448,867 is presented.

1. INTRODUCTION Nova Sco 1992 was discovered by Paul Camilleri on May 22, 1992 in the course of his Nova search programme. The discovery was confirmed by Tom Richards, who immediately produced a chart from the GSC, with comparison stars identified by letters. Mati Morel used this chart for a finder chart on May 25 and a more detailed chart on May 28. V magnitudes for the lettered comparison stars were determined later at the Mount John University Observatory by A. Gilmore. These magnitudes were shown on the final charts, Nos. 1080 and 1081 in Series 23 of Charts for Southern Variables. 2. OBSERVATIONS Members of the Variable Star Section, RASNZ made 612 visual observations between J.D. 2,448,766 and 2,448,867. These are plotted in Figs. 1 and 2. These plots are preliminary because some observers used comparison stars other than the lettered sequence and V magnitudes for these have yet to be measured. 3. DISCUSSION The preliminary light curve is on a large scale which tends to exaggerate differences in the estimates on any one night. It appears, however, that the nova varied on many nights by several tenths of a magnitude. This variation is shown by the most reliable observers who made several estimates on the same night, which showed distinct changes in their estimates from hour to hour. I conclude that the nova did actually vary in brightness by from 0.3 to 0.9 magnitudes on many nights. A few points away from the main light curve are obviously due to either mis- identification or use of incorrect magnitudes for the comparison stars. These will be eliminated when the final light curve is published. The purpose of this paper is to enable observers to see the result of their observations. 9.

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VISUAL OBSERVATIONS OF BL TELESCOPII

Peter F. Williams Sutherland Ast. Soc & VSS, RASNZ 3 McAuley Close, Heathcote NSW 2233 Australia

SUMMARY: Visual observations of the 1987, 1990 & 1992 eclipses of BL Tel are summarised and discussed. Respective dates of mid eclipse for the 1987 and 1992 events are 1987 December 15.0 U.T. and 1992 March 21.5 U.T. Little can be said about the 1990 eclipse due to the lack of observations.

1. INTRODUCTION BL Tel is classified (1) as of type EA/GS + SR with a V range of 7.09 to 9.41. Thus it is an Algol type eclipsing system with one, or both componets giants or supergiants although one component may be a main sequence star. The semi-regular variation is of pulsational character (7-09 - 7.26V), is observed outside eclipses and is sometimes represented by P-65.1 days but sometimes cannot be traced (1) The semi-regular variations are too small for visual observations. Results for the 1983 and 1985 eclipses of BL Tel were discussed by Williams (2)&(3). These showed that BL Tel, a large amplitude long period eclipsing system, is particularly suitable for accurate visual observation. It is an ideal object for long term visual study, being observable at maximum with binoculars whilst a small telescope is capable of reaching it at minimum. 2. OBSERVATIONS Observations were made visually with a variety of instruments Those contributing estimates are listed in Table 1. All used the standard methods of estimating the brightness of a variable as described by Bateson (4). Williams gave a list of suitable comparison stars (2). These are shown in Fig. 1 with their magnitudes. TABLE 1 BEMBRICK, Colin NELSON, Peter BRYANT, Ken SKILTON, Peter FARRELL, Fraser TREGASKIS, Bruce GOLTZ, William WILLIAMS, Peter HENSHAW, Colin WILLIAMSON,Len 12.

Figs. 2 & 3 illustrate the 198? and 1992 eclipses. These were plotted using the "mirror image" method wherein large dots represent original observations and small dots values generated by the mirror plot. This method assumes a symmetrical shape for the light curve. 3. DISCUSSION (A) THE 1987 ECLIPSE: This was a difficult event to observe as BL Tel was essentially a twilight object from shortly after commencement of the eclipse. Table 2 lists the 19 individual observations reported. These are plotted in Fig. 2. There appears to have been a gradual decline from magnitude 7-0 to 7*6 in seven days (0.086 mag/day) after which a more gradual fall of 0.3 magnitude over 12 days (0.025 mag/day) occurred. Finally a much steeper decline 1.5 magnitudes followed during the next 12.5 days (0.120 mag/day), reaching a minimum of 9.3* The actual date of mid eclipse cannot be determined with certainty owing to a lack of observations around minimum. The best date for mid eclipse that could be determined from the available obser• vations is 1987 December 15.0 U.T. (GJD 2,447,144.5). Tbe eclipse commenced on November 13.5 U.T. (GJD 2,447,113.0), suggesting a duration of 63.0 days. However, little can be stated about the rising branch of the light curve as this is solely based on mirror image plots. (B) THE 1990 ECLIPSE: This was another unfavourable event with respect to morning twilight. The following two observations were all that were reported; GJD 2.447,000+ Mag 936.24 7.8 939.23 7.7 All that can be said is that an eclipse occurred. (C) THE 1992 ECLIPSE: This was a well observed event despite its predawn circumstances. A total of 130 obser• vations were used to derive the daily means shown in Table 3. Considerable scatter is present within the raw observations and this remains apparent in the daily mean magnitude. Figure 3 shows the visual light curve of this eclipse based on the derived means. These observations suggest the eclipse commenced on February 21.5 U.T. (GJD 2,448, 674.0), reached mid-eclipse on 1992 March 21.5 U.T. (GJD 2,448,703.0) and returned to maximum on 1992 April 18,5 U.T. (GJD 2,448,731.0). Minimum light was at magnitude 9.2v and the total duration 58.0 days. Mid eclipse for this event occurred some 5 days later than predicted by Kholopov (1) who gives the elements JD 2,434,692.6 + 778.1 days. This, however, is of no great concern as BL Tel has been shown to depart from the dates of predicted mid eclipse by several days. 13.

4. CONCLUSIONS Williams (3) suggested on the basis of the light curve of the 1985 eclipse that BL Tel shows variations in the rates of decline and recovery during eclipses. The 198? eclipse also suggests varying rates of change on the declining branch, as do the eclipses of 1983 (2) and 1992 but to a lesser extent. This effect is to be expected and is seen in a number of other eclipsing systems. As the interval between successive minima varies it would be interesting to ascertain whether the rates of decline and rising from eclipses bears any relationship to the intervals between eclipses. I recommend to all observers that they monitor future eclipses closely at all phases. It is essential that all observations be accurately timed and made at frequent intervals. ACKNOWLEDGEMENT S I thank all observers for their estimates without which this paper could not have been written. I am indebted to Prank Bateson for his valuable comments and suggestions. REFERENCES: (1) KH0L0POV, P.N. Ed 198?. General Cat. var stars, 4th ed. Vol III, Nauka, Moscow. (2) WILLIAMS, P.F. 1985. Publ. Var. Star Section, R. astr. soc. New Zealand. 12; pp. 8-10. (3) WILLIAMS, P.F. 1988. Publ. Var. Star Section, R. astr. soc. New Zealand. 14, pp.40-43. (4) BATESON, F.M. 1987. The Observation of Variable Stars. 4th ed. Tauranga Print Ltd. Tauranga, N.Z.

TABLE 2 Individual visual observations for 1987 eclipse of BL Tel GJD 2,447,000+ Mag GJD 2,447,000+ Mag 074.91 7.0 121.92 7.7 098.95 7.0 124.92 7.7 100.92 7.0 127.94 7.8 106.93 7.0 128.94 7.8 111.90 7.0 132.93 7.9 112.91 7.0 135.93 8.7 114.92 7.2 144.93 9.3 150.94 8.4 117.92 7.5 151.93 8.6 119.93 7.6 120.92 7.6 14.

TABLE 3 Mean of visual observations for 1992 eclipse of BL Tel GJD 2.448.000+ Mag No. 2,44^60(3+ Mag No. 2.4^5^6&5+ Mag No^ Ob 3 — Obs — OTs 661.0 7.0 1 691.0 8.20 ~~"4* 717.0 8.02 3 664.0 6.8 1 692.0 8.34 5 718.0 7.80 2 669.0 7.05 2 693.0 8.43 4 719.0 8.15 2 670.0 6.95 2 694.0 8.6 1 720.0 7.75 2 671.0 7.3 1 695.0 8.67 3 721.0 7.3 1 672.0 7.30 2 696.0 8.70 3 722.0 7-75 2 674.0 7.17 3 698.0 8.87 3 723.0 7-70 3 675.0 7.27 3 700.0 9.0 1 724.0 7-60 2 676.0 7.20 2 701.0 9.1 1 725.0 7-30 2 677.0 7.30 2 702.0 9.1 1 727.0 7.4 1 678.0 7.27 3 703.0 9.20 2 728.0 7.4 1 679.0 7.75 2 705.0 8.80 2 729.0 7.2 1 680.0 7.63 4 706.0 8.8 1 730.0 7.1 1 681.0 7.40 2 707.0 8.6 1 732.0 7.1 1 683.0 7.7 1 708.0 8.80 2 734.O 7.2 1 684.0 7.6 1 709.0 9.07 3 736.0 7.10 2 685.0 7.90 2 ' 711.0 8.65 2 737.0 7.00 3 686.0 7.80 2 712.0 8.6 1 738.0 7.0 1 687.0 8.20 2 713.0 8.47 3 739.0 7.00 2 688.0 8.10 2 714.0 8.40 3 741.0 7.0 1 689.0 7.9 1 715.0 8.4 1 743.0 7.0 1 690.0 8.20 2 716.0 8.3 1

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A POSSIBLE OUTBURST OF V430 CARINAE

M. Morel Member, Variable Star Section RASNZ 18 Elizabeth Cook Drive Rankin Park NSW 2287 Australia

SUMMARY: A series of visual observations of V430 Carinas = HD 96446 is presented, covering the interval JD 2,443,610 to JD 2,444,116 (1978 April 10 to 1979 August 30). There is tantalizing evidence for a prolonged and unusual brightening of this star, by about 0.5 magnitude. Attention is drawn to the possibility of this star being more strongly variable than previously thought.

1. INTRODUCTION HD 96446, located at R.A. (1950) 11h 03m 59s, Dec. (1950) -59 40.8, is a star of unusual spectral characteristics. Its spectral type has been variously classified as B2 IIIp, B2 V He and B3 Vp (1). It is classified as a Helium star with lines of varying strength (2). The Helium lines are very strong, according to (3). It is a member of an open cluster or stellar group first studied in detail by Feinstein (4). He gives the following UBV data for HD 96446 - V = 6.68; B-V = -0.16; U-B = -0.87. HD 96646 has been studied photometrically by Matthews and Bohlender (5) who determined small amplitude (0.03V) variations, consistent with Beta Cephei-type variability. On this basis the star has been named V430 Carinae (6). This paper describes my own observations of this star. 2. CHARTS AND SEQUENCE HD 96446 « V430 Car is plotted on chart 452 (7), (8), but is not labelled. It lies on an E-W line between stars *83' and '84*. A list of V magnitudes suitable for obser• vation of U Car is given by Morel (7). Three of these stars are especially useful for observing V430 Car, namely HD 95880 (6.9V), HD 96248 (6.6V) and HD 95324 (6.2V). Fig. 1 shows the immediate vicinity of V430 Car in greater detail. 3. OBSERVATIONS My attention was first drawn to this star in 1978 April, purely by chance. I was engaged in the preparation of a chart and sequence for the bright Cepheid U Carinae, which lies a little to the west. HD 96446 and neighbouring stars appeared to be suitable for use as comparison stars for a campaign on U Car, described in (7). None of the bright 18. stars in the vicinity of HD 96446 was known or suspected to be variable at that time. Upon observing the field for the first time on 1978 April 10, I noticed that HD 96446 appeared to be noticeably brighter than its published magnitude. The discordance was quite striking, especially when comparing it with nearby HD 96248 (V=6.55, spec, type BO). The star was thereafter observe d regularly (apart from seasonal gap) until 1979 August 30. The observations from JD 2,443,610 to 2,443,747 were made with 20 x 65 mm binoculars (tripod mounted). When observations resumed on 2,443,902 I used 10 x 50 mm binoculars exclusively until monitoring was ter• minated on JD 2,444,117. The star appeared to be unusually bright in 1978 April-May. 4. DISCUSSION My observations are presented in the form of a light curve (Fig 2). The large scale of 1fais curve permits me to make the following comments on the gross features of V430 Car's behaviour. (a) JD 2,443,610 to 2,443,617. Very steady at 6.2v. (b) JD 2,443,625 to 2,443,685. The overall trend is a decline in magnitude, possibly with fluctuations. There is much scatter in the points during this phase, and it is impossible to state how much of the variation is real, and how much is due to observational error. The night-to-night fluctuat• ions are more erratic here than in other parts of the light curve. (c) JD 2,443,697 to 2,443,950. Fairly steady at about 6.7v with few, if any, significant fluctuations. During this phase the observed magnitude agreed well with the published value for V (6.68). There were no observations from JD 2,443,747 to 2,444,902. (d) JD 2,443,953 to 2,444,030. The observations suggest a slight overall brightening, but it is not possible to be certain about this, as any such increase would have barely exceeded the normal errors of observation. (e) JD 2,444,030 to 2,444,117. Observations are very few and widely scattered, but do not indicate any further rises of a protracted nature. The ability of individual visual observers to resolve small amplitude features in a light curve has been discussed recently by Lawson et al (9), who demonstrated that the estimates of very experienced visual observers can be quite accurate down to the 0.1 mag level. Whilst I do not claim that my estimates are all accurate to +/- 0.1 mag, I do consider that consistent estimates that are 0.5 mag above the normal level, as recorded for V430 Car, do represent an increase in brightness that is real. Obviously, corroboration and confirmation is required from other observers to validate my observations. 19.

5. CONCLUSION There is sufficient information to suggest that in 1978 April/May, V430 Car did show unusual behaviour (a mini- outburst?). The observerations reported here do not cover the early part of the rise, so the duration, and other features, are not known. Confirmation of the event is needed, possibly from suitable archival photographs. My own observations are reported here to draw attention to V430 Car and its potential for substantial variations in brightnesso

6. REFERENCES (1) HOFFLEIT, D., SALADYGA, M. & WLASUK, P. 1983. A supplement to the Bright Star Catalogue, Yale University Observatory. (2) JASCHEK, C. & EGRET, D. 1982. 'Catalogue of Stellar Groups'. Publcation Speciale du CDS No. 4, CDS, Strasbourgo (3) HOUK, N. & COWLEY, A.P. 1975. Michigan Catalogue of Two-Dimensional Spectral Types for the HD Stars, Vol. 1 University of Michigan. (4) FEINSTEIN, A. 1964, Observatory, No. 940, p.111. (5) MATTHEWS, J.M. & BOHLENDER, D.A. 1988, IBVS 3226. (6) KH0L0P0V, P.N. ed, 1990, IBVS 3530 (?0th Name- List of Variable Stars). (7) MOREL, M. 1979, Publ. 7, Var. Star Section, R. ast. soc. New Zealand (C79), p.23. (8) BATESON, F.M., MOREL, M., SUMNER, B. & WINNETT, R. 1979, Charts for Southern Variables, Series 11, Publ. by Astronomical Research Tauranga, New Zealand. (9) LAWSON, W.A., COTTRELL, P.L. & BATESON, F.M. 1988, Publ. 16, Var. Star Section, R. ast.soc. New Zealand (C88), pp 24-27.

A Possible Outburst

o-P VV30 Car V430 CARINAE

• • N • • • 10' • —I V • V430 • • • • •

• * • 4 • •• • • E • • • •

• • • • • • • • • • 0XZ • • • • • • • *

• 4C

Fig. 1. Identification chart for V430 Car and comparison stars. A = HD 96248? B r HD 95880; C = HD 95??4. 21.

V 430 CARINAE 6.0 ir i—i—r

a • ••••••

.6 • • •• • • • • •• • •

7.0 J 1 L 2 443600 3650 3700 3750

Fig. 2(a). JD 2,445,600 - 2,443,750.

6.0 i—i—r i i—r

L 7.0 I 1 J i L J L 2443900 3950 4000 4050

Fig. 2(b). JD 2,443,900 - 2,444,050.

Fig. 2(o). JD 2,444,050 - 2,444,120

Fig. 2. Visual light ourve for V43O Carinae. Individual observations. 22.

OBSERVATIONS OF THE TRANSIENT X-RAY SOURCE AQ538-66

Frank M. Bateson Director, Variable Star Section, RASNZ P.O. Box 3093, Greerton, Tauranga, N.Z.

SUMMARY: Positive visual observations of A0538-66 are tabulated. No definite recurrent cycle is apparent. Two possible flares were recorded. Otherwise fluctuations over a small range occurred. It is pointed out that observers using telescopes with thresholds of 14.0, or slightly brighter, mistake a 13th magnitude star immediately south of the x-ray source for the latter.

1. INTRODUCTION A0538-66 is an extremely powerful LMC recurrent x-ray transient source. P.A. Charles et al (1) discussed photometric, spectroscopic and satellite data from which a model of this system was proposed. It was also shown that A0538-66 had a recurrent period of 16.6 days but it also had intervals of inactivity,, 2. OBSERVATIONS Members of the Variable Star Section, RASNZ, made 867 visual estimates between J.D. 2,446,882 and 2,448,771. Most were negative as can be seen from the light curve in Figs. 1 and 2. All observations were made using Charts 630 and 631 (2) and the sequence of comparison stars thereon with V magnitudes. Some observers using apertures with thres• holds of 14.0 or slightly brighter reported positive observations ranging from 13.3 to 13.6 with a mean value of 13.47. I am satisfied that these observations were of a star of magnitude 13*5 that lies very close to A0538- 66 and immediately south of it. The two objects cannot be separated in small telescopes. In fact A0538-66 would normally be invisible in such telescopes so that an observer would mistake the 13th magnitude star for the variable. This view is supported by observations made with larger apertures that showed A0538-66 was at least a magnitude fainter close to the time when estimates of around 13.5 were made. All positive observations made with small apertures have therefore been rejected. Three observers used larger instruments capable of separating the two objects. These members are shown below with the range of their estimates and the number of positive observations each made given in brackets. Their positive observations are listed in Table 1. On a few occasions they also reported negative estimates when A0538-66 was invisible and fainter than 14.5 to 14.7. These observationsare not shown in Table 1. CRAGG, T.A. (CJ) 13.1? - 15.8 (35) GOLTZ, W. (Gp) 14.0 - 15-0 (133) NELS0N,P. (Nl) 13.7? - 15.0 (49) The observations are scattered in time and mainly confined to the main LMC observing season. All three observers operate from dark sites. 3. DISCUSSION Usually the estimates from Cragg and Goltz indicate con• tinuous fluctuations in brightness with some distinct peaks between 14.0 and 14.3. However Cragg normally made A0538-66 definitely fainter than did Goltz. The obser• vations by Nelson generally showed a small range being mainly centred around magnitude 14.5. Two possible flares were recorded and are marked in Table 1 by question marks and must be regarded with caution in the absence of confirming estimates. The first, magnitude 13.7, was reported by Nelson on J.D. 2,447,188, may indicate activity as the same observer estimated the var• iable at 14.0 on the previous night. The second possible flare, magnitude 13.1, was recorded by Cragg on J.D. 2,447,295, has no other observations near it. There is no evidence for a recurrent cycle due to the scattered nature of the observations. The light curve (Figs. 1 & 2) indicate that A0538-66 mainly varied between 14.3 and 15.0 with most of Cragg1s points falling below 15»0 It should be noted that the brighter observations that were rejected as referring to the star immediately south of the variable have not been erased from the curves and should be ignored. 4. CONCLUSIONS No firm conclusions can be drawn from the data apart from stating that there appears to have been an absence of flare like activity with the exception of two very doubtful examples. This may be due to the scattered nature of the observations which also obscured any evidence for a recurrent cycle. Possibly during most of the interval covered by the observations A0538-66 was comparatively inactive but the limitations of the data make this uncertain. 24.

One definite conclusion can be stated. It is a waste of time and effort for observers using telescopes with thres• holds of 14.0, or slightly brighter, to observe this object. ACKNOWLEDGEMENTS My appreciation is extended to Tom Cragg, Bill Goltz and Peter Nelson for their observations and to Ranald Mcintosh for the light curves and computer print-out of the data. REFERENCES (1) CHARLES, P.A., BOOTH, L., DEUSHAM, R.H., et al. 1983. Mon. Not. R. astr.Soc. 202, pp. 657-682. (2) BATESON, F.M., MOREL, M. & SUMNER, B. 1982. Charts for Southern Variables, Series 14, Publ. by Astronomical Research Ltd., Tauranga, New Zealand.

TABLE 1 A0558-66 - POSITIVE OBSERVATIONS J.D. Mag Obs J.D. Mag Obs J.D. Mag Obs 2,44 V 2 *» • * • • V 2,44 .... V 6,886.9 14.7 Cj 7,144.01 15.0 Nl . 7,188.19 14.8 Gp 6,905.91 14.7 Gp 7,145.99 14.5 Nl 7,189.03 14.0 Nl 6,906.89 14.4 Gp 7,147.0 14.8 Gp 7,202.0 15.0 Cj 6,907.92 14.7 Gp 7,148.2 14.8 Gp 7,210.0 15.0 Cj 6,910.89 14.6 Gp 7,156.0 15.8 Cj 7,212.0 15.3 Cj 6,912.88 14.4 Gp 7,168.99 14.5 Nl 7,215.00 15.0 Nl 6,914.88 14.2 Gp 7,170.01 14.8 Gp 7,229.0 15-3 Cj 7,059.12 14.8 Gp 7,171.00 14.5 Nl 7,230.96 14.5 Nl 7,062.06 14.7 Gp 7,171.02 14.8 Gp 7,234.0 15.2 Cj 7,080.02 14.5 Gp 7,172.0 14.6 Cj 7,245.9 15.3 Cj 7,082.05 14.7 Gp 7,172.02 14.8 Gp 7,263.9 15.2 Cj 7,089.02 14.8 Gp 7,177-18 14.8 Gp 7,269.01 14.5 Nl 7,094.04 14.8 Gp 7,179.20 14.8 Gp 7,271.9 15.0 Cj 7,097.1 15.1 Oj 7,180.21 14.8 Gp 7,295.9 13.1? Cj 7,112.0 15.5 Oj 7,181.19 14.8 Gp 7,418.09 14.5 Nl 7,136.99 14.5 Gp 7,182.19 14.7 Gp 7,434.0 15.2 Cj 7,140.03 14.7 Gp 7,185.19 15.0 Gp 7,465.05 14.5 Nl 7,141.0 14.5 Nl 7,186.18 15.0 Gp 7,466.01 14.5 Nl 7,142.03 14.8 Gp 7,187.07 14.0 Nl 7,466.98 14.5 Nl 7,144.0 14.7 Gp 7,188.02 13.7? Nl 7,471.99 14.5 Nl 25.

TABLE 1 (Cont.) AQ538-66 - POSITIVE OBSERVATIONS

J.D. Mag Obs J.D. Mag Obs J.D, Mag 2.44 Obs v 2.4TT v 21 < v

7,473.92 14.5 Nl 7,859.14 14.5 Gp 8 ,190.24 14.5 Gp 7,474.0 15.1 CO 7,863.14 14.5 Gp 8 ,191.00 14.1 Nl 7,475.95 15.0 Nl 7,865.14 14.5 Gp 8 ,208„0 15.5 Cj 7,477.01 14.5 Nl 7,867.16 14.7 Gp 8 ,220.18 14.5 Gp 7,478.01 14.5 Nl 7,870.20 14.5 Gp 8 ,236.05 14.5 Gp 7,507.99 15.0 Nl 7,877.04 14.7 Gp 8 ,237.0 15.7 Cj 7,509.99 14.0 Nl 7,879.0 15.2 Cj 8 ,238.20 14.7 Gp 7,532.00 14.3 Nl 7,882„05 14.7 Gp 8 ,254.18 14.3 Gp 7,535.0 15.2 Cj 7,885.19 14.5 Gp 8 ,264.00 14.7 Gp 7,536.01 14.5 Nl 7,890.17 14.7 Gp 8 ,264.99 14.4 Gp 7 ,538.99 15.0 Nl 7,910.03 14.5 Gp 8 ,265.0 15.1 Cj 7,541.12 15-0 Nl 7,914.0 14.7 Cj 8 ,269.01 14.4 Gp 7,553.05 14.5 Nl 7,914.19 14.7 Gp 8 ,270.07 14.5 Nl 7,554.02 15.0 Nl 7,917.15 14.5 Gp 8 ,278.02 14.5 Gp 7,555.00 14.7 Nl 7,920.00 14.3 Gp 8 ,281.00 14.7 Gp 7,558.95 14.5 Nl 7,929.19 14.5 Gp 8 ,284.20 14.7 Gp 7,560.01 14.5 Nl 7,937-99 .5 8, ,291.99 .7 7,563.02 14 Gp 14 Gp 15.0 Nl 7,940.97 14.3 Gp 8, ,292.0 15.1 Cj 7,566„1 15.0 CO 7,941.0 15.0 Cj 8 ,294.98 14.8 Gp 7,569.03 15.00 Nl 7,942.97 14.3 Gp 8 ,298.19 14.5 Gp 7,583.0 15.2 Cj 7,945.94 14.3 Gp 8 ,303.0 15.3 Cj 7,588.06 15.0 Nl 7,948.95 14.5 Gp 8 ,305.98 14.3 Gp 7,597.9 15.1 Cj 7,951.95 14.5 Gp 8 ,307.98 14.5 Gp 7,613o9 15.2 Cj 7,966.93 14.5 Gp 8, ,320.95 14.3 Gp 7,627,9 15.1 Cj 7,968o0 15.5 Cj 8, , 321.0 15.1 Cj 7,677.89 14.5 Gp 7,969.92 14.5 Gp 8, ,322.96 14.5 Gp 7,749.33 14.7 Gp 7,973.01 14.5 Gp 8, ,333.9 14.8 Cj 7,772.29 14.5 Gp 7,977.03 14.5 Nl 8, ,335.94 14.4 Gp 7,776.30 14.7 Gp 7,978.95 14.5 8, ,338.96 14.3 7 .1 Gp Gp ,791 15.4 Cj 7,979.96 14.5 Nl 8, 350.9 14.7 Cj

7,804.03 14.5 Gp 7,980.93 14.3 Gp 8, ,351.93 14.4 Gp 7,805.23 14.3 Gp 7,985.00 14.2 Nl 8, 355.93 14.4 Gp 7,819.06 14.5 Gp 8,003.02 14.7 Gp 8, ,362.92 14.4 Gp 7,823o04 14.7 Gp 8,007.95 14.5 8, ,378.90 14.7 7,831.20 .2 Gp Gp 14 Gp 8,010.93 .5 8, ,383.89 .7 7,833.02 14 Gp 14 Gp 14.3 Gp 8,028.91 .5 8, 389.90 .7 ,029 14 Gp 14 Gp 7,835.17 14.5 Gp 8 .91 14.5 Gp 8, 389.98 14.5 Nl 7,852.14 14.5 Gp 8,039o90 14.5 Gp 8, 391.89 14.4 Gp 7,856.01 .3 Gp 8,055.87 .4 8, 393.91 .4 7,857.14 14 14 Gp 14 Gp 14.5 Gp 8,160.26 14.5 Gp 8, 411.89 14.4 Gp 26.

TABLE 1 (Gont.) A0558-66 - POSITIVE OBSERVATIONS

J.D. Map; Obs J.D. Mag Obs J.D. Mag Obs 2 t) » m * t 2,%4~ v v .5 8,420.88 14.5 Gp 8,645.99 14.4 Gp 8,716.98 14 Nl 8,506.30 14.5 Gp 8,647.00 14.6 Nl 8,718.96 14.8 Gp 8,529.99 14.5 Nl 8,651.00 14.6 Gp 8,720.93 14.0 Gp 8,534.25 14.4 Gp 8,651.99 14.5 Gp 8,768.89 14.3 Gp 8,542.23 14.5 Gp 8,655.99 14.6 Gp 8,768.93 14.2 Gp 8,561.06 14.7 Gp 8,659.00 14.4 Gp 8,771.87 14.5 Gp 8,565.22 14.5 Gp 8,663.02 14.7 Gp 8,574.21 14.4 Gp 8,665.0 15.1 Cj 8,578.22 14.5 Gp 8,667.23 14.7 Gp 8,584.98 14.5 Gp 8,675.97 14.5 Gp 8,593.97 14.5 Nl 8,676.98 14.5 Nl .5 8,677.95 8,598.19 14 Gp 14.5 Gp 8,679.99 .5 8,599.0 15.3 14 Nl 8,600.98 14.5 Nl 8,680.9 15.4 Cj 8,602.21 14.7 Gp 8,689.95 14.7 Gp 14.4 Gp 8,690.99 15.0 Nl 8,619.20 8,707.0 8,622.04 14.5 Gp 15.0 Cj 15.2 cj 8,707.93 14.7 Gp 8,625.1 14.5 8,715.0 15-5 Cj 8,634.00 14.7 Nl 8,715.90 14.4 Gp 8,636.21 Gp

1985 1986 1987 ~H—

8-

10

12-

v". vvv w V *V V V vvv wvv V V rv »v vvv 14-

a • 1 a 0 16 + + + •f 6888 6188 6288 6388 6488 6588 6688 6788 6888 6988 7888

A0538-66 FIGURE 1 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,446,0 0 - J.D. 2,447,000 27.

84

10

124

J _

144 V V V V B • W W W V V V B W V V ^ B |V D B B3 if • V V BE • V V « » g iBB SBB VO BWBI • ID flflB DB •on V t 11/ BJ| 1 • *f ' BBJB B

VB B 0 B J B B BBP I - . D * a • « • o • a • „ o ' B B n 16 H ' I 1 1 1 1 1 1 h 7808 718—0 —7208 7380 7408 7580 7608 7780 7808 7980 8808

18

124

v v v

144 d "flr vvv w v •

w a o D 0 am »B V fl fl B B B 16 8808 8180 8288 8380 8408 8580 8600 8780 8808 8980 9808

A053S-66 FIGURE 2 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,4-47,000 - J.D. 2,448,771 28.

THE DISCOVERY OF NOVA PUPPIS 1991 Paul Camilleri Ast. Soc Victoria & VSS RASNZ RMB 2013, Cottons Rd., Cobram VIC 3644 Australia

SUMMARY: An account of how Nova Pup 1991 was discovered is given. This nova could have easily been discovered visually had any one been observing the old nova CP Pup in December 1991.

I bought a 85mm f/2 lens and EM camera body after the discovery of Nova Oph 1991 No.2. I began taking photos on November 24 1991, but found only some known variables by the end of the moon free period in mid December. A lot of high level cloud after the December full moon prevented me from taking any photos until December 27. However this high level cloud persisted so that the limit• ing magnitude of my photos was 9 instead of the usual 12. The next day I searched a few of the photos but decided to leave the rest until the sky cleared and I could retake these fields down to magnitude 12, after which I would search all fields. The clouds cleared by January 1 enabling me to photograph all my usual fields again. The next day I searched most of the photos finding only a few known variables. I did not have time to search six of the fields I had taken. On January 3 I searched two of these photos finding nothing. I then cut and mounted the third photo and began to search it. I noticed a bright 7th magnitude star near the top centre of the photo. This object was not visible on a photo I had taken on December 11 which reached down to magnitude 12. I was therefore certain it was a nova. I had taken photos of this area on December 27 so on exam• ining these I found that the nova was slightly brighter on them. On comparing the field with the Uraanommetria Atlas I found that the nova was close to the variable, Y Pup and the old nova CP Pup (Nova Pup 1942). I thought for a few seconds that CP Pup was having another outburst until a closer look showed that the new object was about 14 arc minutes north of CP Pup. I was certain that I had dis• covered a nova after comparing my photos to atlases that had a limiting magnitude of 15 and showed no object at the position of the nova. I then measured the position of the nova on my photos and checked that this was not identical with any known or suspected variable listed in the catalogues. 29.

Once I was satisfied that it was a nova and I had measured its position as well as determining its mag• nitude on my photos it was a matter of advising Eob McNaught, Frank Bateson and Alan Gilmore, so that confirmation could he made of the discovery, accurate positions measured and advice sent to Brian Marsden. The resultant details have already been published so there is no need to repeat them here. It was at this stage I realised, because the nova was close to CP Pup, that there was already available a suitable chart with a good sequence. It is worth pointing out that had any visual observer been ob• serving CP Pup the nova could easily have been dis• covered visually. Nova Pup 1991 is the first nova to be discovered in Puppis since 1963 and the fifth to be found in that constellation. I suggest that the few discoveries of novae in Puppis is simply due to the lack of searches in this area. I estimate that this area of the Milky Way should produce 2 or 3 novae each year. It is interesting to recall that, excluding novae in the Magellanic Clouds, the years with the most novae discoveries have been:

1936 (7); 1962 (6); 1975 (6); 1991 (8) As far as I know I have found the most novae discovered by any observer in one year. This is a record I hope to keep adding to. 30. LIGHT CURVE OP NOVA PUPPIS 1991 Prank M. Bateson Director, Variable Star Section RASNZ P.O. Box 3093, Greerton, Tauranga New Zealand

SUMMARY: The light curve of Nova Puppis shows a decline of three magnitudes in 286 days. The decline rate for the first $0 days was 0.03 magnitudes per day, thereafter it was 0.003 magnitudes per day.

1. OBSERVATIONS The light curve of Nova Pup 1991 appears in Pig. 1 * This is based on 637 observations made by members of the Variable Star Section, RASNZ from J.D. 2,448,624- to 2,449, 047. The estimates were made using the visual sequence for CP Pup as shown on charts 1078/9 (1). This sequence was subsequently replaced by the V magnitudes for comparison stars determined by Alan Gilmore at Mt. John University Observatory (2;3). 2. DISCUSSION Daily Means were used to determine the decline rate. Nova Pup 1991 declined at 0.03 mags per day for the first 50days. Thereafter this rate slowed to 0.003 mags/day. A decline of three magnitudes from a maximum of 8.80 occurred in 286 days. 3. CONCLUSION Nova Pup 1991 is a slow nova. The observations are continuing. ACKNOWLEDGEMENTS All observers are thanked for their estimates. Ranald Mcintosh kindly produced the computer light curve. REFERENCES: (1) Bateson, P.M. & Morel, M. 1992. Charts for Southern Variables, Series 23. Publ. by Astronomical Research Ltd., Tauranga, New Zealand. (2) Gilmore, A.C. 1993. Circ. Nova Pup 1991 Photometry of Comparison Stars. (3) Bateson, P.M. & Morel, M. In press. -888734 HV PUP 1991 31.

1 1 1 1 1 1 1 1 1 1 1 1 i -i 1 1 1 1 1 1 1 1 1 1 1 1 1 r

8-

18-

12-

14

' ' • I I I I I 1 1 1 1 IE 1 ' ' I I I I I 1 1 1 1— 2448696 788 888 988 (Individual observations)

-888734 HV PUP 1991

4 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 i 1 1 1 1 1 1 1 1 1 1 1 1 1 r

E-

8-

18-

12

0 •• o

14-

'»•••' I I I I I I I I IE I I 1 I I 1 1 1 L. 2448988 1B88 1188 1288 (Individual observations)

NOVA PUP 1991 FIGURE 1 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,448,624 - J.D. 2,449,047 32.

TWO COLOUR SEQUENCE FOR 0525J52 TV COLUMBAE

P.M. Kilmartin Mount John University Observatory P.O. Box 57, Lake Tekapo, N.Z.

Comparison stars for TV Col were lettered on Charts 1097 and 1098 (1). V and B-V measures were obtained for these stars on March 5 & 6 1993« Three readings were obtained for each star except "s" which had one reading. Star "r" could not be measured owing to its proximity to the variable. An attempt will be made later to measure this star. The values obtained are shown below: STAR V S.D. B-V S.D. ADOPTED Mag for visual estimates k 12.66 +/-0.02 0.59 +/-0.02 12.7 1 12.29 +/-0.01 1.01 +/-0.03 12.3 m 12.89 +/-0.03 0.61 +/-0.02 12.9 P 13.16 +/-0.03 0.55 +/-0.07 13.2 q 13.87 +/-0.06 0.67 +/-0.13 13.9 s 15.2 0.5 15.2 Visual observers should use the magnitudes in the last column in their estimates for TV Col.

REFERENCE (1) Bateson, F.M. & Morel, M. 1993. Charts for Southern Variables, Series 23. Publ. by Astronomical Research Ltd., Tauranga, New Zealand. 33.

THE SEMI-REGULAR VARIABLE RX LEPORIS

Frank M. Bateson Director, VSS, RASNZ P.O.Box 3093 Greerton TAURANGA, NEW ZEALAND

SUMMARY: RX Lep is shown to have a visual range of 5.1 to 7.0 with semi-regular period of 62.5 days from maxima and 70.2 days from minima. Suggestions are given to improve the accuracy of observations of bright Binocular variables.

1. INTRODUCTION Variable stars which can be observed with Binoculars appeal to observers without previous experience in observing variables. This is because they are both bright and easy to locate, whereas experienced observers tend to avoid such stars in favour of more important objects. Thus there is usually more scatter in the estimates than is desirable. The absence of observations from experienced observers prevents the determination of the sysmetic deviation for new observers. However, some simple precautions will improve the accuracy of any new observer. All observations must be made with binoculars or a small finder telescope and never with the naked eye or your main telescope. Make certain that the binoculars or finder are in perfect adjustment. Always use the same instrument. Make certain that you allow your eyes to become dark adapted; in other words don't dash outside from bright indoor lights and commence observing at once. Always use the binocular chart provided and the sequence of comparison stars thereon. Avoid observing in bright moon• light; in fact it is best to make observations with the moon absent. Make certain that you identify the variable and comparison stars correctly, always checking with the chart and not relying on memory. These guide-lines should be followed for all binocular variables and will help the inexperienced observer to greatly improve the accuracy of his or her observations. 2. OBSERVATIONS Visual observations from J.D. 2,446,800 to 2,448,765 are plotted in Figs. 1 & 2. The majority of the estimates were made by new observers gaining experience in the art of visual observations. This causes more scatter in the estimates than usual. There are a few data points that are 34. obviously in error, probably due to misidentification of the variable or comparison stars and these have been rejected. All observations were made using Binocular Chart B3 and the sequence of V magnitudes shown thereon. The 496 estimates were grouped into ten days means, each of which had from 1 to 11 individual estimates with an average of 3 observations in each mean. Table 1 lists the dates of maxima and minima determined from these means.

3. DISCUSSION The dates given in Table 1 must be regarded as approximate due to the nature of the observations. For example, RX Lep can remain at maxima for a protracted interval making the determination of the date of maximum a matter of personal judgement having regard to the weight given to the observations in each mean. The individual observations range from 5.1 to 7.0 whilst for maxima range from 5.43 to 6.20 and minima from 6.07 to 6.8. Columns 4 and 7 in Table 1 give the intervals between sucessive maxima and minima respectively. These are enclosed in brackets when the dates are not considered to be consecutive, mainly due to breaks in the records when RX Lep was unobservable. RX Lep has a slow, semi-regular variation with a wide variation in the intervals between consecutive maxima (or minima).

4. CONCLUSIONS RX Lep is a semi-regular variable with a visual range of 5.1 to 7.0. Thirteen maxima that appear to be consecutive give a period of 62.5 days with intervals showing a wide spread of from 22 to 102 days. The mean period from 12 minima is 70.2 days with intervals between minima that are considered to be consecutive ranging from 28 to 106 days. These results should be regarded as approximate because of the nature of the observations as pointed out in Section 1 on the previous page.

ACKNOWLEDGEMENTS My thanks are extended to all observers for their estimates and to Don Brunt for processing the data and to Ranald Mcintosh for the computer light curves. 35.

TABLE 1 RX LEPORIS - MAXIMA & MINIMA

MAXIMA MINIMA Mean Max Mean Max No, o Int. Mean Minimum Mean Min Int, JD 244 . Mag JD 244

6920 6828 6.7 1 7070 6.05 7010 6.8 (182) 2 5.97 (150) 7099 6.32 89 3 7130 6.16 60 7142 6.47 43 4 7209 79 7248 106 5 7260 6.2 51 7288 6.42 40 6 7387 5.93 (127) 7440 6.07 (152) 7 7489 5.7 102 7528 6.40 88 8 5.70 32 7549 60 7560 6.07 9 7619 5.90 70 7642 82 10 7651 5.70 32 7763 6.10 (121) 5.90 6.10 11 7933 6.03 (282) 7844 6.20 81 12 7998 6.00 65 7960 6.7 (116) 13 8020 5-6 22 8038 6.57 78 14 8169 5.5 (149) 8250 (112) 15 8301 5.68 (132) 8240 6.8 90 16 8378 5.43 77 8506 6.47 (166) 17 8552 5.7 (174) 8590 6.51 84 18 8601 6.0 49 8618 6.7 28 19 8669 5.87 68 8710 6.48 92 20 8747 5.7 78 6.50 6.40

8-

18-

12

5888 5188 5288 5388 5488 55BB 5&B8 5788 5888 5988 6BB8

RX LEP FIGURE 1 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2445,000 - J.D. 2446,000 1 r T 1

64

c B

104

124

14 H h 6800 6180 6200 6300 6400 6580 6600 6700 6808 6980 7808

6-

184

124

14 H 1 1 1 1 1 1 1 h 7808 7188 7280 7380 7408 7580 7608 7780 7808 7980 8808

a 8 " a '

8-

10-

12-

14 H 1 1 1 1 1 h 8808 8180 8208 8380 8400 8580 8608 8780 8808 8980 9800 RX LEP FIGURE 2 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2446,000 - J.D. 2448,900 37.

THE FADING OF S DORADUS F.M. Bateson (1) & A.F. Jones (2) Variable Star Section, RASNZ (1) P.O. Box 3093, Greerton, Tauranga, N.Z. (2) 31 Ranui Road, Stoke, Nelson, N.Z.

SUMMARY: Visual observations show that there was a very small decline in the mean magnitude of S Dor from 1987 to 1990. The rate of decline increased from 1991. It is suggested that this marks the start of a fading to a deep minimum.

1. INTRODUCTION S Dor is the protype for a small group of high luminosity, blue irregular variables. These objects are amongst the brightest ones found in galaxies. Members interested in a review of these stars should consult A.S. Sharov (1). S Dor had deep minima in 1891, 1900, 1930, 1940, 1955 and 1964 (2) 2. OBSERVATIONS The visual observations are given in Table 1 as a means for every 100 days from J.D. 2,447,000 as shown in column 1. One of us (AFJ) was responsible for by far the largest number of estimates. The means from his observations are shown in the second column withtiie number of estimates for each mean in brackets. Column 3 gives the same results from the estimates by Peter Williams, whilst the means from the few observations by other members appear in the last column. The light curve is shown in Fig 1. S Dor is a difficult star to observe due to the diffuse nebula in which it is situated in the Large Magellanic Cloud. The variable and a sequence of comparison stars with V magnitudes are shown on chart 906 (3). 3. DISCUSSION The means in the second column of Table 1 shows there was an irregular decline of 0.17 magnitudes over the first 1,200 days (1987 to 1990). The rate of fading then increased in 1991. T. Cooper (4), a member of the VSS, used data from our Monthly Circulars in his paper (4). He suggested that the start of a decline may have commenced in 1991• From about mid-June 1991 southern skies were dimmed by a huge blanket of volcanic dust. This appears to have formed a continuous sheet high in the strato• sphere and was not patchy. We believe its effect was uniform and affected both the variable and the comparison stars equally. The first eight means from P. Williams in column 3 of the table show that he made S Dor definitely fainter than APJ with a tendency to show a possibly irregular brightening. His later means appear to confirm a fading with means becoming very close to those in column 2. One of us (PMB) was responsible for research• ing the data. He was confronted with the fact that both observers are highly skilled and extremely accurate visual observers. Then why is there such a marked difference in their estimates? Possibly the lower altitude and the much greater light and other pollution over the general Sydney area compared to better sky conditions over Nelson might account for the difference. However, that idea is not acceptable because it fails to explain why their more recent estimates are in close or precise agreement. Perhaps as the sheet of volcanic dust drifted over more southerly latitudes it had the effect of dimming stars over Nelson leaving Sydney skies unaffected by this cloud. Then why are their estimates for other variables close to the same declination as S Dor in such perfect agreement? Unfortunately there were few observations from other observers. Only in one 100 day interval were there sufficient to provide a comparison. That mean agreed very closely with the mean from APJ. Otherwise these means appear to support a fading of S Dor. The conclusion is that S Dor is a difficult object to observe and estimates are affected by prevailing sky conditions. CONCLUSIONS We are satisfied that S Dor has faded to a marked degree from 1991 and may be heading towards another deep minima. ACKNOWLEDGEMENTS We thank Peter Williams for his observations in particular and other observers for their limited estimates. Also Don Brunt and Ranald Mcintosh for computer processing the data and for the computer light curves. 39.

REFERENCES (1) Sharov, A.S. 1975. IAU SYMP.67. ed. V.E. Sherwood. Publ D. Reidel Pub. Co., Dorecht. pp 275-284. (2) Hoopopov, P.N. (ed) 1985. Gen. Cat. var. stars 4th ed. Vol 2, Nauka, Moscow. (3) Bateson, F.M. & Morel, M. 1988. Charts for Southern Variables, Pub. Astronomical Research Ltd. Tauranga, New Zealand. (4) Cooper, T.P. 1992. Mon. Notices A.S.S.A. Vol Nos. 11 & 12, pp 121.

TABLE 1 S DORADUS - 100 DAY MEANS 100 JD d.. Fro. m Mean Mag Mean Mag Mean Mag 2 *) ^l' • AFJ PW Others 7000 — 7100 8.79 (56) _ 7100 - 7199 8.79 (40) — 9.0 (1) 7200 — 7299 8.75 (56) - 7300 - 7399 8.74 (59) - — 7400 - 7499 8.70 (43) 9.60 (4) 8.88 (6) 7500 — 7599 8.79 (43) 9.47 (12) 8.81 (37) 7600 - 7699 8.90 (42) 9.27 ( 7) - 7700 - 7799 8.89 (34) _ — 7800 - 7899 8.89 (3D 9.55 ( 8) — - 7900 7999 8.93 (30) 9.41 ( 7) — 8000 - 8099 8.86 (27) 9.33 ( 3) - 8100 8199 8.89 (24) 9.45 ( 2) 9.40 (5) 8200 - 8299 8.96 (21) 9.57 (13) 9.23 (3) 8300 - 8399 9.20 (19) 9.41 ( 7) 9.55 (2) 8400 — 8499 9.34 (22) 9.5 ( D 8500 - 8599 9.65 (27) 9.66 ( 5) — 8600 - 8699 9.60 (22) 9.64 (13) - 40.

6808 6188 6288 6388 6488 6588 6688 6788 6888 6988 7888

J L T 1 1 1 r

8-

10-

12-

14-

16 H 1 1 1 1 1 1 1 V 7780 8 7180 7208 7380 7408 7580 7600 7700 7800 7900 8808 L 6 i 1 1 1—i 1 1 1-1 1 1 r

84

104

124

14

16 .....+ . 8880 8180 8208 8380 8400 8580 8608 8788 8800 8900 9808

S Dor FIGURE 1 Light Curve from Individual Observations J.D. 2,446,800 - 2,448,800 41.

OUTBURSTS OF THE DWARF NOVA IP PEGASI

Frank M. Bateson P.O. Box 3093, Greerton, Tauranga, New Zealand.

SUMMARY: Sixteen outbursts of IP Peg from 198? to 1992 were observed. The mean cycle is 74.8 days with long outbursts more frequent than short. Segments of the light curve are reproduced.

1. INTRODUCTION V.P. Goranskij, et al (1) summarised photographic obser• vations of IP Peg, classifying it as a dwarf nova of SS Cyg type with eclipses. A mean cycle of 95 days was found from six outbursts found on the Moscow plates. The B maxima magnitudes ranged from 12.0 to 13.9. 2. OBSERVATIONS This paper reports on the visual observations, totalling 802 by members of the V.S.S., RASNZ between J.D. 2,446,924 and 2,448,629 (1987 May 8 - 1992 October 28). Observations were made using charts 855/6 (2). Large gaps occur in the estimates during the interval when the star is unobservable. 3. DISCUSSION Details of observed outbursts are given in Table 1 and segments of the light curve are shown in Figs. 1-3. IP Peg has not been as closely monitored as the southern dwarf novae. Nine of the outbursts in Table 1 are probably consecutive with intervals ranging from 16 to 111 days, giving a mean cycle of 74.8 days, compared to 95 days from the Russian observations (1). Outbursts for which the maxima magnitudes appear reliable range from 12.0 to 13.3. Long outbursts are more frequent than short, but this is probably because the former are more likely to be seen. The monitoring has not been close enough to show any effect of eclipses. There are a few observations between 14.0 and 15.0 but as minima are well below the threshold of the instruments used nothing can be stated concerning behaviour at minimum. 4. CONCLUSIONS IP Peg has a mean cycle of 78.4 days with long and short outbursts. The former have a mean maximum magnitude of 12.15 and a width of 7.5 days at _3.0. The corresponding values for short outbursts are 12.4 and 3 days. Minima are far to faint to be observed and the estimates are too scattered to show eclipses at maxima. The observed outbursts are too few to make the conclusions definite. 42. ACKNOWLEDGEMENTS My appreciation is extended to all observers for their estimates, and especially to Danie Overbeek who was responsible for 65% of the observations, I thank Ranald Mcintosh for the light curve. REFERENCE (1) GORANSKIJ, V.P. et at 1985. Inf.Bull.Var.stars No.1653 (2) BATESON, F.M. & MOREL. M. 1987. Astronomical Research Ltd. Tauranga, New Zealand. TABLE 1 IP PEG - OBSERVED OUTBURSTS JD Max Max Int. Type Width No. Remarks No. 2,44... .~JT d^_ 13.0 I 13.0 D 13.0 I-D 5bs 37 1 6,633 12.0 ? 5 2 6,744? 12.5 111 ? - 1 3 6,993 12.2 (149) L 993? 999 6? 6 (a) 4 7,080? 13.3 87 - - 1 5 7,122 12.5 12 - 122 - - 2 (b) 6 7,347 11.6?(225) L 347 355 8 10 (c) 7 7,657 12.9 (310) ? - 1 (d) 8 7,718 12.0 61 L 717 724 7 9 9 7,797 12.4 79 L 796 803 7 12 10 7,888 12.5 91 S 888 891 3 4 11 8,092 12.7 (204) ? 091 - 3 12 8,154 12.2 62 L 153 160 7 10 13 8,292? 12.0 138 ? — — - 1 (e) 14 8,437 11.5? 145 L 436 445 9 12 (f) 15 8,551 12.3 114 S 550 553 3 2 16 8,577 12.0 26 L 576 584 8 4 2" Remarks: (a) Gap of id befor„ e 993. (b) Gap 11 122 (c) Max Probably too bright, magd11.6? - (d) Gap before 657* 144 d (e) Gaps 15 before & 3aafter 292. (f) Max mag of 11.5? - Probably too bright.

IB

12-

v W v v W V 14-

-L -I I 1 I l_ _t I L_ 16 1 1 I 2446686 78B 888 986

IP Peg FIGURE 1 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,446,600 - 2,446,900 43.

8 1 1 1 1 • ' i 1 1 1 1 1- -i 1 1 r 1 1 I 1 1 1

18

124 •w V

144

-m> v

16 I 1 1 1 1 1 ' • i i—i i • ' 1 I | I —i—•— ——i— —i—I_J 2446986 1886 1188 1286 8 -i 1 1 r I i 1 1 1 i " l i 1 1 , 1 , , T 1 , , , R

IB 4

12

VV V v

V WV V DV W W VWWtv V V WW VV \ -wv w v 144 HflW

I—1 I • 16 •J— —I—I— —I ' ' « ' 1 1 i • . . 1 1 1 1 1 1 1 1 1 2447286 386 468 506

8 1 1 1 1 i 1 r—i r 1 1 1 ~l 1 1 1 1 1 1 r—| 1 1 1 ! r 1 i 1

164

12

wnw v w v a w v v v xotrv v vB4

• v 144 V *v VV V V VW M UVH^, v v

16 I 11—1 1 I ' 2447588 686 7BB 886

IP Peg FIGURE 2 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,446,900 - 2,447,800 44.

1 1 1 1 1 1—i 1 p ™l 1 i 1 r 1 1 1 1 1 —i i j 1 i 1 r 1 1 1

18

12-

•ror V

v P • D V V

W V ~wW W V v a w W V 14 t* V V -

L_I 1 L_Li » i I 1 1 1 1 _ i —i .i i i i i i l_ —' 1 1 1 L _ 1 1 2447888 988 1888 1188

8 1 1 1 1 ~| 1 ! 1 I r~— 1 ! 1 1 1 1 1 1 1 1 1— 1 1 1 1 1— 1 1 1

18

V

12- as a 0 - V V V -w v V V v V V

VV V JpOV • o v v^, WW v v v^s v v

v V v -ww^v^ w 14- V V V

V V

i 1 1 t t 1 1 16 1 1 1 1 1 1 1 1 I I 1 I 1 1 1 1 2448188 281 8 138 8 488

i i I I i I i" 1 1 1 1 1 8 I I -T 1 r -i 1 1 r

18-

12- •w V >»• V B V W V V W WVW

wvwWfe w^vW wy^v D VBVWWV V B VVV

14- WWI-HMHWM'VOW' X? "WW

' • I L_ _1 16 I I I L_ 2448488 588 688 780

IP Peg FIGURE 3 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,447.800 - 2,448,700 45. LIGHT CURVES OF SOME MIRA VARIABLES Ranald Mcintosh & Don Brunt Variable Star Section, RASNZ P.O. Box $093, Greerton, Tauranga, New Zealand.

SUMMARY: Computer light curves covering six decades of visual observations are reproduced for the Mira variables S Pic; T Cen; RS Sco; T Gru; S Gru and R Ind.

1. INTRODUCTION On July 27, 1928 Bateson (1) formed the N.Z. Branch, Southern Variable Star Section of the B.A.A. (N.S.W.). The following year this became the VSS of the Astronomical Society of N.Z., which became the RASNZ many years later. The initial programme was that of the B.A.A. consisting of Mira variables and one R CrB variable. In the late 1930s and early 1940s the programme was extended to include a larger number of southern Miras and a variety of other types of variables. In the 1950s southern dwarf novae were added to the observing list. All observations to 1st April 1987 were entered by hand on to ledger sheets. The results were published in Circulars (2) and the First Memoir (3). Computers have made it possible to transfer all the old records on to disks to which are added each month data after 1st April 1987. This has made it possible to commence publication of computer drawn light curves. This paoer commences the publication of the light curves for Miras, which will be continued in subsequent publications and concluded with a table of the elements found from the light curves. 2. OBSERVATIONS All observations have been made visually by members of the VSS, RASNZ, using the standard charts and sequences. The following pages contain the light curves for: S Pic; T Cen; RS Sco; T Gru; S Gru; and R Ind. The earliest plots contain few observations but sufficient to determine a few points of maxima and minima. Comments on the light curves will be made in the final paper listing the elements found. REFERENCES: (1) Bateson, F.M. 1928. Circ. 1, Southern var. star section, BAA, N.Z. Branch. (2) Bateson, F.M. 1929-1972. Circs. 4-199. VSS, ASNZ & RASNZ (3) Bateson, F.M. 1944. First Memoir, VSS, Ast. Soc. of N.Z. 6000 6100 6200 6300 6400 6500 6600 6700 6800 6900 7000

6 L

84

•V V

10 •TV V V V VVvW V X'

if WV WV V V vv vvv a w v v v w v v w 12 V V V

VV V "V V 14-

16 1 h 7800 7180 7208 7300 7408 758+0 7608 7788 7888 7980 8800

• o a• • oD i

104 V V W V V V v

124

14-

16 H r 8008 8180 8208 8388 8488 8580 8600 8780 8888 8980 9908

S PIC LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,426,800 - J.D. 2,429,000

Fig. 1 9908 9198 9208 9380 9408 9580 9608 9700 9808 9980 0000

& 1 r 1 1 1—i • , i ,

8-

10-

v v 12-

14

16 + + + 8 100 200 388 400 588 688 780 800 980 1808 6 4 1_ i—• 1 ( _L

10-

W WW v wv 124

crv w -vwv v v v B 144 D B

16 + 1800 1180 1200 1300 1400 158+8 1600 1780 1808 1988 2800

S PIC Fig 2

LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,429,000 - J.D. 2,432,000 i i i 1 1 • 1 1 1 r 48. 8 V 1B-

12 > -

V V V W w 144 B O

16 1 1 1 1 h 2868 21BB 22BB 239B 24BB 25B0 2688 27BB 28BB 2988 3808

-1 so 8 B -a a" a ^. a D BB "A a 10 B

12

V V V WV W ^. V V V V

B B 14-1 9 9 0 0

16 1 1 1 1 , 1 , 1 1 3868 3188 3268 3386 3468 3588 36BB 37BB 3888 3988 4BB8

6 1 r—™— 1 1 1 1 1 1 1 H i L-

'f mm 84

B

18

\ 124 •

t D B 14 fl fi

16 H h 4B8B 4186 42B8 4386 4488 4588 4668 4786 4868 4986 586B S PIG Fig. 3 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,432,000 - J.D. 2,435,000 t— r 49. 8

18

• = 12-(

V V \-W D W v V W V V V V 144 •a * - •

16 i 1 1 1 1 1 1 1 , 1_ 5BBJ8 5188 5288 5388 5488 5588 5&B8 5788 5888 5988 6888

6 , R

6888 &1BB 6288 6388 6488 6588 66B8 6788 6888 6988 7888

1 1 1 1 1 — i 1 1 i 1

84

IB

124

• V VV V V " V w V 144

16 H 1 1 1 1 1 1 1 h 7BB8 71BB 72BB 738B 74BB 7588 7688 7788 7888 79BB 8BB8

S PI C Fig. 4 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,435,000 - J.D. 2,438,000 50.

• 10

"•I

* • d i i n a 12- a

Do a •R • a V Vff V v v 144 o o 0 •

16 H 1 1 1 1 1 1 1 r - 8869 81B0 820B 8388 8488 8588 8688 8788 8888 8988 9888 , 1 1 1 1 1 —r 6 ~i—' 4 1

fi• • a a a a B

le - D fl • D ° V OB H * fl DBS Ip D B • 12 B

• B fl B V V V w V V V V D V V WW w 144 D V

16 I 1 1 1 1 1 1 1 1 1 9868 9188 9280 9380 94BB 9588 96B8 97BB 9888 99BB BBBB

i_ T

8-

1B-

12- fl W •

B " I B 14-

16 H h 8 188 288 38B 4B8 588 688 788 8BB 988 1888

S PIG Pig. 5 LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,438,000 - J.D. 2,441,000 51. 8

18-

E • 12-

V V V

V V V V V 14

16 H I - 1888 1188 1288 1388 14B8 1588 1688 1788 1888 1988 2888

16-

12- " p

V V V W \AW 14

16 + H h 2868 218B 2288 2388 2488 2588 2688 278B 2888 2988 3868

18 1 \iH

12-

14

16 H h + 3888 3188 3288 3388 34B8 3586 3688 3788 3888 3988 4868

S PI C Pig. 6 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D, 2,441,000 - J.D. 2,444,000 4969 4186 4268 4386 4468 4586 4680 4786 4868 4986 5868

6 _ L

a "L. fl 8- • • TS 0

a 16-

1 V 12- V • if V | B B V B % B _ wwrr vww/v w v B wn # o « a o °- 14- • B B BB V V

16 H 1 1 1 1 1 1 1 h 5888 5186 5288 5386 5468 5586 5688 5788 5888 5988 6868 6 , 1 —• . . l

v a n

16 *"2. .

12- B B B •

• v v v v . f v v • ^ V V V V\iVV VW 0 V V V 144 • v v v • g « I » v g

16 H 1 1 1 h 6868 6186 6268 6386 6488 6588 6688 6786 6888 6986 7868

s PIC Pig. 7 LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,444,000 - J.D. 2,447,000 53. -T— D 0 B

8_l s. .

• B

124 V B V <4W V nBD B V V v y • _ . B _ d •?

B>\ "BV v imrv B fin

H 1 1 1 1 1 1 1 h 7888 7188 7288 7388 7488 7588 7688 7788 7888 7988 8888

84

18

124 •a v" • j _ • V B V V B

^ B * * V B V P S . * U w V ^

'»* lltl A.B VB DB 144 BB • • •

16 H 1 1 1 1 1 1 H 8888 8188 8288 8388 8488 8588 8688 8788 8888 8988 9888

S. P I C Fig. 8

LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,44-7,000 - J.D. 2,448,775 5888 5188 5288 5388 5488 5588 5GB8 5788 5888 5988 G8B8 4

• in, 1 = _J• • JV. If

8

184

124

14 E888 6188 E28B 6388 G4BB 6588 66BB 6788 G8B8 69BB 7BBB

64

a o • • . 4 • ° • 84 . 0

1B4

124

14 + + 7888 718B 7288 73BB 74B8 7588 7688 7788 78BB 7988 8BBB

T GEN Pig. 9 LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,425 ,450 - J.D. 2,428 ,000 8868 8188 8288 8388 8488 8588 8688 8788 8888 8988 9888

9888 9188 9288 9388 9488 9588 9688 3788 9888 9988 B88B 4 . . . . 1 —• . , — L .

188 2B8 388 488 586 688 786 868 986 1888

T CEN Pig. 10 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,428,000 - J.D. 2,431,000 188B H B B 12BB 13BB 14BB 15BB 1SBB 17BB 18BB 19BB

184

124

14 29BB 2188 22BB 23'BB 24BB 25BB 26BB 27BB 28BB 29BB

84 V * ff " • * I s

IB

1 2

14 38BB 3188 3288 3388 3488 3588 3SBB 378B 38B8 3988

T GEN Pig. 11 LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,431,000 - J.D. 2,434,000 104

124

5988 5108 5288 5388 5408 5588 5688 5788 5888 5988 6888

• "•• • *»\ * rt * ••d! 1 o • B> o » / S . " \V B - iff 84 f

1 0

124

14 H 1 1 1 1 1 f - 6888 6188 6288 6388 6400 6508 6600 6788 6888 6988 7808

T GEN Fig. 12

LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,434,000 - J.D. 2,437,000 7908 7180 7208 7380 7408 7586 7600 7700 7880 7980 8888

4 —L

8080 8108 8200 8388 8488 8588 8688 8788 8888 8988 9888

4

9888 9188 9288 9388 9488 9588 9680 9708 9888 9998 0800

T.OEN Fig.1 3 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,437,000 - J.D. 2,440,000 64 TO

• l «• r Vsa= ft- !• * 5 84 • oo , J i . b a

184

124

14 + 1888 1188 1288 1388 14B8 1588 1688 1788 1888 1388 2888 4 , ' , , , r J , , . L

2888 2188 2288 2388 2488 2588 2688 2788 2888 2988 3888

T CEN Fig. 14

LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,440.000 - J.D. 2,443,000 12-

14 1 1 1 1 1 1 1 1 1 1 ' 3909 3100 3209 3300 3400 3596 3600 3796 3800 3998 4989

4 I 1— 1 r 1 —I i 1 1 1 J 1 1 1

12-

5989 5198 5289 539B 5488 5598 5609 5798 5888 5988 6989

T GEN Fig. 15

LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,443,000 - J.D. 2,446,000 61.

6- OB B

• s 7 1 { ' * 8- OB I" 4 mi S 18-

12-

14 6888 6188 6288 6388 6488 6588 66B8 6788 6888 6986 7888

7888 718B 72B8 7388 7488 7588 7688 7796 7868 7988 8888 4 | , r - 1 , . _|

8888 8188 8268 8388 8488 8586 8668 8786 8868 8986 9888

T GEN Fig. 16 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,446,000 - J.D. 2,448,680 62.

64

8 -

184 v v

vv B 124

14 7888 7188 7288 7388 7488 7588 7G88 7788 7888 7988 8888

6-

8-

18- A

12-

14 8888 8188 8288 8388 8488 85*88 8688 87"8B 8888 8988 9888

4 r-

8-

18-

12-

144 ' 1 1 1 1 1 H 9060 9186 9268 9388 9488 9586 9668 9786 9868 9988 8888

RS SCO Fig. 17 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,427,240 - J.D. 2,430,000 8 188 288 388 488 588 G88 788 888 988 1888

8- • f 0=

5 •#

10-

12-

14 1888 1188 1288 1388 1488 1588 1GBB 1788 1888 1996 2888

4 , R

28B8 2188 22B8 2388 2488 258B 2688 2796 2888 29*883888

RS SCO Pig. 18 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,430,000 - J.D. 2,433,000 3BBB 3188 3288 3388 3488 3588 368B 3788 3888 3988 4BBB

48BB 4188 4208 43BB 44BB 4588 4688 47BB 4808 4988 5888 4

5BBB 518B 52B8 5388 54BB 5588 5688 5788 5888 5988 6BBB

RS SCO Fig. 19 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,433,000 - J.D. 2,436,000 bb"* 8 1 |

1 0 4

124 rwvv

14 + 6888 6188 G288 6388 G488 6580 6688 67'8B 6888 6988 7888 4

64

•Si V.

184 4. V v v IP

,'5^»r www 1 2 •IV, • j A • vv" a a # • •

14 + H h H 1 - 7888 7188 7288 7388 7488 7588 7688 7788 7888 7988 8888 4 r—1 . , 1 1, . 1

64

M 8 5 °^

i 18

V V xlf • V V D D B • • 124 V V V V . ^ W • ° | a • a

14 1 1 h 8888 8188 8288 8388 8488 8588 8688 8788 8888 + 8988 9888

RS SCO Pig. 20 LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,436,000 - J.D. 2,439,000 9888 9188 9288 9388 9488 9588 9G88 9788 9888 9988 8888

4 1 1" 1 - J 1 1

64

• ; bjV. ^ V • 8- fl 9 . B

i

o # • J 1B4 V Bpj

° 3 0 B •

12 A ' •

, , 1 14 1 1 1 1 1 1 8 188 288 388 488 588 688 788 888 988 1808

4 1 1 1 1 T H 1 LT r

84 • a s • i I • i

18 •Hi

B B D W 124

14 1088 1188 1288 1388 1480 1588 1688 1788 1888 1988 2888

RS SCO Fig. 21 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,439,000 - J.D. 2,442,000 T

1—h u: 64

i • a

o g 84 ^ 8 .

H'g • i % 104

124 T1V "W

VO

1 4 2088 2180 2288 2388 2488 2588 2600 2788 2888 29*88 3888

3888 3188 3288 3388 3488 3588 3608 3 7 8 8 3 8 8 8 3988 4888

4888 4188 4280 4388 4488 4588 4688 4700 4888 4988 5880

RS SCO Pig. 22 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,442,000 - J.D. 2,445,000 68.

64

B4 , TP* *

1B-

v v v j 1 12- •i B ti a r D i • H i -a D BIB D

14 + + + 59BB 51BB 52BB 5388 5488 5588 5688 5788 5888 5988 6888

6888 6188 6288 6388 6488 6588 6688 6788 6888 6988 7888

64

8 Y

IB

•I ^fl_ V V B B V B° B 124 • fl H

14 7888 7188 7288 7388 7488 75*88 7688 7788 7888 7988 8888

RS SCO Fig. 23 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,445 ,000 - J.D. 2,448 ,000 — 1 1 i i 1 1 H 1 r 69 64 B fl BJfl fl n

8 J!

i ie4 B • • • B

v • °s 12^ x:

• i • 1 4 H 1 Y 8000 8108 8288 8388 8488 8588 8608 87'88 8888 89'BB 9888

RS SCO Fig. 24 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,448,000 - J.D. 2,448,475

7888 71BB 7288 7388 74B8 7588 76BB 7788 7888 7988 8888

T GRU Pig. 25

LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,427,700 - J.D. 2, 428,000 8888 8198 8288 8300 8488 8588 8688 8780 8880 8980 9088 6 T T T

8-

I 0*

18 I 0

12-

14-

16 H h 1888 1188 1288 1388 1488 1588 1688 1788 1888 1988 2888

6 . . u 1 , . — l

8 a • Jmm • I • e 18- B ^ .1* "

B B

12-

14

16 H h 2808 2108 2280 2300 2480 2588 2688 2788 2888 + 2988 38B8

T GRU Fig 26 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,4-28,000 - J.D. 2,4 -33,000 . 1 h , , l

8-

18-

12-

14-

16 1 1 H- 1 h 3888 318B 3288 3388 3488 3588 3688 3788 38BB 3988 4888 6 r1-

4888 4188 4288 4388 4488 4588 4688 47BB 48BB 4988 5888

HI •>» II'I D f 1 n ^ S * f g o

I • i ». "q •(! ' . " 18

o ° ; , i n ° a • 124

144

16 1 H h 5BB8 5188 52B8 5388 5488 5588 5688 5788 5888 5988 68B8

T GRU Fig. 27 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,4-33,000 - J.D. 2,4-36,000 72.

84 lB-r

124 a if

144

1 6 6088 6188 6288 6388 64B8 6588+ 6688 6708 6888 69BB 78BB 6 i 1 1 1 1 —" 1 1 ' ' 1 '

8

1 • m fl B D 1 IT, i D^ 1 8 a 0 ' 1 • D

124

144

1 6 7080 7108 7288 7388 74BB 7588 7688 7788 7880 7908 8888 6 1 I— 1 1 1 \ 1 1 —i 1 1

84

1 8 a a

i * 1

124

144

1 6 8888 8188 8288 8388 84BB 8588 86B8 87BB 8880 89BB 9888

T GRU Pig. 28 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,436,000 - J.D. 2,439,000 14

16 + 9888 9188 9288 93BB 94B8 9588 9688 + 9788 9888 9988 8888

" 1 6 ' ' 1 ' • 1 h , , L_

84

on • •iSS " a B O B ° o 8 18- 8 •" s." o "bo

B

12- gOIB

14-

16 8 188 288 388 488 58B 688 788 888 988 1888

1888 1188 1288 1388 1488 i 1588 - i 1688 1 1788 1 1888 1 1988 1 2888

T GRU Fig. 2 9 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,439,000 - J.D. 2,442,000 74. 8 V .

10-

a • DD D 12

144

16 H h 2800 2100 2200 2380 2400 2500 2600 2700 2880 2908

3080 3188 3288 3388 3400 3588 3688 3788 38BB 3988

6 1 i 1—1 1 1 1 r 1 r

84

• • i r iff o n • o ? V 18

'I

D • 124

14

16 H h 4888 4188 42BB 438B 448B 4580 4688 4788 4888 49BB

T GRU Fig. 30 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,44 -2,000 - J.D. 2,44 -5,000 75. 8-

i f ."fa

10- u —

1,», 12-

14-

16 H h 5888 51BB 5289 53BB 5488 5588 56B8 + 5788 5889 5988 6988 6 1 „ I 1 1 1 r - ,

84

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a B 0 104 *' *r' J" * » V B B w V vl' °B ID

124

144

+ 1 1 1 16 1 1 1 1 I I , 6888 6188 62BB 6388 6488 6588 66B8 6788 6888 6988 7988 6 I 1 ' 1 1 1 •—I , L

1 .•»•• . M 184 v 4" « s • i • f

• B B fl/fl 12

14-

16 7888 7188 7288 7388 7488 7588 7688 7788 7888 7988 8888

T GRU Fig . 31 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,445,000 - J.D. 2,448,000 76.

8 A,

18- 4.- • D B B d L r^B

•• •V. • « s. • i >J] 12- • I' e

14

16 + + + + 8880 8188 8288 8388 8488 8508 8688 8788 8888 8980 9080

T. GRU Fig. 32 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,44-8,000 - J.D. 2,448,728

7888 7188 728B 7388 74BB 7588 7680 7700 7800 7988 8888

S GRU Fig. 33 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,427,800 - 2,428,000 8868 8188 8288 8388 8488 8588 8688 8788 8888 8988 9888

8 4

18

124

V V V V D

144 • V V B D

16 + J h 1888 1188 1288 1388 1488 1588 1688 1788 1888 1988 2888

8-

18-

12-

t V W V V W W V B I OB fl B • 14 0 B

16 H 2888 2188 2288 2380 2400 2508 H 2680 2780 2880 2900 3088

S GRU Pig. 34 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,428,000 - J.D. 2,433,000 78.

B g . 8 -

18-

124

144 V V V V

1 1 1 1 16 l 1 1 1 1 1 3989 3188 3288 3388 3488 3588 3688 3788 3888 3988 4888

L b m _ B B o 8 • « -

•l 18 •J,

12-

14-

16 4888 4188 4288 4388 4488 4588 4688 4788 4888 4988 5888

fl• an0 0 %^ an

184

0°

12-

14-

16 H 1 1 1 1 1 h 5888 5188 5288 5388 5488 5588 5688 5788 5888 5988 6888

S GRU Fig. 35 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,433,000 - J.D. 2,436,000 6908 6180 6200 6388 6400 6500 6600 6700 6800 6980 7808 6 T T

84

1 0

124

144 W V V vw

16 7888 7188 7288 7388 74BBH h7588 7688 77BB 78BB 798B 8808

6 •—L

i i —i 1 1 1 8868 8186 8288 8386 8488 8588 8688 8788 8888 89BB 9880

S GRU Fig. 36 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2.436,000 - J.D. 2,439,000 r 80. BO B p

8 4

104

12 w

at? W W B 14 fl B B

1 1 16 1 1 1 1— 9989 9108 9280 93BB 9480 9508 %00 9708 9880 9908 8080

' . r - J . L T

8 4

104

124

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V V V W 14 v v v v1

16 H 0 180 288 388 4B8 H 5BB 688 7BB 888 988 1888 6 -i 1 r1 1 1 , i

8 4

IB

12-

14-

16 f - H 1 1 1 1 f - 1888 1188 1288 1388 14BB 15BB 1688 1788 18BB 1988 2888

S GRU Fig. 37 LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,4-39,000 - J.D. 2,44-2,000 8

IB-

a 12- D a

14 vwv

16 2BB8 2188 22B8 2388 2488 2588 2608 2780 2808

8

1BH • •

1 2

144

16 1 h 3888 3188 3208 3380 3408 3580 36BB 3788 3888 6 , — . L

8

10-

12-

14- B "

V VV

16 H 1 4888 4188 4288 4386 4488 4588 46BB 47884868

S GRU Fig. 38 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,442,000 - 2,445,000 82.

8 4

18

a B

B D 124 .3> B B V V V V V

VB ™Bff V*V# 144 • • V w

h + 16 1 1 4 1- 5888 5188 5288 5388 5488 5588 5688 5788 5888 598B 6888 6 i 1—i 1 1 1—1 1 1 1 \

a % B 8- a •

1B-

Si 12- •"V • HI

14

16 h 6888 6188 62BB 6386 6488 6586 4 6688 6788 6868 69B8 78BB

7BBB 7186 7288 7388 74BB 7586 7688 77BB 7888 79BB 8868

S GRU Fig. 3 9 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,44 -5.000 - J.D. 2,448 ,000 83,

104

V B » 1 2 V B ll V V V

vv D fl V n a 144 B jjfl

16 8800 8108 8280 8308 8488 8598 8688 8788 8888 8988 9800

S GRU -4-0 Fig. LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,4-4-8.000 - J.D. 2,44-8,728

8 4

10

124

144

16 1888 1188 1288 1388 1488 1588 1688 1788 1880 1900 2888

R IND Fig. 4-1 LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,4-31,368 - J.D. 2,4-32, Q0Q —r 84.

D D 16

124

• o 1 w g n a • D D Vo B 14

16 H 1 1 1 1 1 h 2BBB 2180 2200 2390 2400 2590 2600 2790 2800 2980 3908 6 -h 1 1 1 1 r

84

10

124

144

16 ...... 3888 3180 3208 3300 3400 3500 3600 3780 3808 3980 4808 6

8-

18 s

124

V w v v 14- B B

16 1 1 1 1 1 1 1 1 1 1 4888 4180 4208 4380 4408 4580 4608 4780 4808 4980 58

R IND 42 Fig. LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 242,000 - J.D. 2,435,000 8-

10- • • • .

° f " r B a 12-

14- V V W W

16 +: 1 1 1 1 1 1 1 1 - 5000 5108 5280 5300 5409 5598 5688 5708 5880 5 9 8 8 6 9 8 9 6

8-

Q B 1B-) •

12

14

16 + 1 1 1 1 1 1 1 h 6888 6188 6288 6388 6488 6588 6688 6788 6888 6988 7800 6 +

84

10

a BB

12-

www 14- V

16 H 1 1 1 1 1 h 7900 7190 7209 7300 7400 7500 7608 7780 7808 7980 8808

R IND 43 Fig. LIGHT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,435,000 - J.D. 2,438,000 8989 8180 8208 8380 8408 8580 8608 8780 8808 8980 9800 6

8 4

18 • • • -« • o

9 . X 124

• s * VVVWV « V W V V 14

16 H 1 1 1 1 H \ 9808 9180 9208 9380 9408 9580 9608 9780 9808 9980 0808 6

8 -

18

12

V V w 144

16 H 1 1 1 1 1 1 1 1- 0 188 2BB 388 48B 588 608 780 808 980 1080

R IND 44 Fig. LIG-HT CURVE FROM INDIVIDUAL OBSERVATIONS J.D. 2,438,000 - J.D.2,441,000 1868 1188 1288 1388 1488 1588 1668 1788 1888 1988 2888

8 4

184

i 124

14-

16 + + 2888 2188 2288 2388 2468 2586 2688 + 2788 2868 2986 3888 6 1 1 L

8 4

10

124

v vv v 144

16 I 1 1 1 1 1 1 1 1 1 3888 3188 3288 3386 3468 3586 3668 3788 3868 3988 4868

R IND Pig. 45 LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,441,000 - J.D. 2,444,000 4988 4188 4288 4388 4488 4588 4689 4798 4888 4988 5888 6

• A 10

124

D V 144 a.

16 + + 5988 5188 5288 538B 54BB 5588 5688 5788 58BB 5988 6888

6 1 1 i '—i 1 1 — 1 1 1 *r

8-

V V V V W V . 18-

12

V V 144 \°0 *

16 ...... + 6B8B 6188 628B 6388 6488 65BB 6688 6788 68BB 6988 7888

R IND P i g . 46 LIGHT CURVE PROM INDIVIDUAL OBSERVATIONS J.D. 2,444,000 - J.D. 2,447,000 89.

REPORT OF THE VARIABLE STAR SECTION ROYAL ASTRONOMICAL SOCIETY OF NEW ZEALAND

For year ended 31 DECEMBER 1992

1. OBSERVATIONS. Total 76,299 exclusive of those received from the B.A.A. (U.K.) for southern stars as part of a co-operative programme with the B.A.A. This a g a i n i s a r e c o r d , d e s p i t e the u n u s u a l a d v e r s e weather during the prime observing season. The individual totals from each observer appears follow• ing this report. As usual totals are for the 12 months to 31 August, 1992, i n order to provide strict comparison with previous years before the Society's year was changed to 31 December. The monthly distribution of observations shown i s on the last page of this report, showing the normal decrease ilate n spring and early summer. The large i n c r e a s e i n May was due t o t h e c l o s e m o n i t o r • ing of many dwarf novae i n outburst and novae of discovered by Paul Camilleri. This graph was kindly supplied by Ranald Mcintosh. As usual Danie Overbeek and Abby Jones made out• standing contributions whilst 12 other observers contributed over 1,000 each.

2 * GRANTS. We w i s h t o e x p r e s s our v e r y s i n c e r e appreciation to the following for grants specific for purposes: The Edward Corbould Trust of the Astronomical Association Queensland; of The Scientific Research Committee, N.Z. Lottery Board and the Trust Bank, Bay of Plenty.

3. DONATIONS. An appeal was issued in Publications No. 17 seeking donations particularly to provide part-time office assistance at Headquarters. This has brought a most gratifying response and I sincerely thank all the following fortheir support. W.M.B. Albrecht; Auckland Astronomical Society; Auckland Observatory & Planetarium Trust Board; Canterbury Astronomical Society; Dr. S. Dreves; E. Harries-Harris; Dr. B.J.M. Hassall; G . Herdman; Mrs. A. Leslie; R. Mcintosh; M.D. Overbeek; A. Pearce; N.J. Rumsey; J. Simpson; Sutherland Astronomical Soc; Tauranga Rock & Mineral Club; Dr. N.W. Taylor; Mrs. Watson. D. 90.

4. COMPUTER DATA PROCESSING. The 1991 Annual Report outlined the objectives in processing on computer all the hand written observational records prior to 1 April 1987* Excellent progress i n so doing had been made through the splendid assistance of Don Brunt as w e l l as help from Bill Goltz and Maureen Phizacklea. Ranald Mcintosh has added a l l these results to his files and produced the resultant light curves and print-outs. Bob Winnett, Peter Nelson and Stan Walker are assisting me i n reducing some of the data to a suitable form for publication. I workingam on a large stack of these light curves for publication. Ranald Mcintosh has continued to punch into the computer all current observations as they come to hand each month. He supplies a l l the print-outs for Monthly the Circulars which are now printed on our computer at headquarters. Ranald has also supplied a l l the light curves and print• outs for requests from professionals for data. Dr. T.J. Richards, TrobeLa University, has agreed to provide storage for our data and i n due course those requiring our data will be able to obtain fromi t the Computer Department at La Trobe. In 1993 I hope to list the variables for which records can be transferred to La Trobe. An announcement will be made i n due course of the stars concerned and the dates that the records cover. Ultimately the aim i s to have a l l records, other than recent and current observations stored there so anyonethat interested can obtain whatever they require. This will relieve any storage problems which Ranald Mcintosh has. Naturally it will require some time to accomplish this.

5. PUBLICATIONS. Publications No. 1 7 was distributed early in the year. No. 18 should be available from the printer within a few weeks and will be followed by No. 19.

6 . CIRCULARS. In addition to the Monthly Circulars, two Special Circulars were published and number a of others dealing with Novae discoveries were faxed to observers. There were four issues of CHANGING TRENDS, which serve to keep observers in touch with each other also and list special programmes.

7. REQUESTS FROM PROFESSIONALS FOR VISUAL DATA. Throughout the year there has been a steady and increasing request from professionals for both prompt alert notices when the variables in which they are interested exhibit unusual behaviour. There were also many requests for subsequent visual light curves and print-outs of the observations covering the period of unusual activity. This i s understandable because the observations from large ground based telescopes and from space are made at wavelengths other than the visual yet i t i sessential to 91.

BEQUESTS FROM PROFESSIONALS FOR VISUAL DATA (Cont.) know how t h e particular variable behaved i n the visual. Obviously i would t be a sheer waste of time and money to use the costly modern technology tomonitor stars i n the hope that something unusual would happen. This i s why visual observations have become so important and their results cannot be duplicated by any othermethod even in this age of automated photo-electric instruments. I stress these facts merely to show observers that 1hey play a vital, if humble part, i n astronomical research. The aim of our Alert Notices i s to have the advice of any unusual event reach those requesting such notices within 5 to 1 0 minutes of the event being observed. Most members are aware of the special programmes run during the year but seems i t that the main ones should be summarised in this report as this will show members the value of their efforts. Brief details of where so much of our data has gone to appear on the following pages.

ROSAT. Last year I reported that this programme had finished. However, this year I received an urgent request for light curves of VW Hyi f o r use meeting at a a t the University of Birmingham where a discussion on theROSAT results were to be held. Subsequently Barbara Hassall, R.G.O., obtained our results on anumber of past super outbursts of this well studied dwarf nova. Later she advised that they had obtained much so data - almost too much - that reduction would take some time. I.U.E. Programmes were run on several dwarf novae with Tim Naylor (Keele University) which for light curves and print-outs of our data were supplied. GALACTIC HALO DWARF NOVAE. Several alert notices were faxed to Steve Howell (Planetary Science Institute.U.S.A.) as p a r t of the long term observation of these stars for which spectroscopic and other observations made are with several large ground-based telescopes inU.S.A. PRE MAIN SEQUENCE STARS. John Graham (Carnegie) obtained spectra of a group of these stars in Corona Austrina for which we supplied light curves and print-outs.

HST. The only CV fwhich o r priority was given i n the first year of HST was OY Car. I was informed Marsh by Tom (Oxford) that the success of the observations depended entirely on our detection of the super outburst promptly. The response from observers was wonderful. several For months prior to this outburst OY Car was observed on every night except December on 26, 1991 and on most nights there were at least three, and usually more observations. The outburst was detected promptly and throughout the outburst the coverage was perfect. Complete light curves were supplied toboth Oxford and the Space Telescope Science Institute. 92.

NOVAE. (a) Michael FriedJung (France) requested light curves of a number of past novae to compare their published variations of emission line fluxes with light curves i n order to test the classification claimed by Bob Williams. We supplied several light curves. (b) H . Durbeck (Germany) used our data on onovae l d that are still visible in members instruments for use i n his theoretical papers on the hibernation theory novae. of (c) Light curve ofNova Sgr 1992 No. 2 was supplied to James Bryan (U.S.A.) f o r use i n paper a he i s submitting to A.S.P.

(d) V603 Aql (Nova Aql 1918). Alex Schwarzenberg-Czerby requested our visual data during the period October i n 1992 that observations were being made from ROSAT/IUE/ Voyager. H e also asked that we continue these observations throughout the current observing season and again 1993* i n He has been sent a l l our records plus some photo-electric data kindly supplied by Budding. Ed.

Was Eta Car. Roberto Viotti (Italy) supplied with our light curve f o r use i n the s t u d i e s a tinstitution h i s of this star and of AG Car. Details of the latter had already been supplied to our member, Tim Cooper, for presentation of his paper at a meeting in South Africa. The up-dated light curve of AG Car forViotti i s now being processed.

V517 Oph. A l l our data, mainly from observations by Abby JoneB, of this probable R CrB variable went to S.A.A.O. Jones and myself were co-authors wtththe S.A.A.O. group of the paper that was published i n OBSERVATORY.THE

TV Col. At the request of Coel Heller (Mullard Space Science Laboratory but now U.S.A.) i n TV Col and V1223 Sgr were placed on our observing list and charts issued in Series 23. A Jones has made observations of TV Col which will be reduced as soon as reliable magnitudes of the comparison stars are available. Meanwhile the preliminary results indicate that these stars are intermediate polars and similar to EX Hya imany n respects. EX Hya. Coel Heller wa,s also supplied with a l l the details of the b r i g h t outbursts of EX Hya. He may request the complete light curve covering many decades and I am awaiting word from him about this.

ASSISTANCE T O GRADUATES. Karen Pollard (University of Canterbury, N.2.) spent a daysfew at headquarters collecting data on RV Tau stars for her thesis. Light curves and observations of Ceti WW were supplied to University of SUSBSX f o r use by a graduate and h i s supervisor; S. Duck (Leicester, U.K.) also requested light curves for use with his thesis. 93.

CO-OPERATIVE PRO GRAMME WITH B.A.A., (U.K.) Monthly print- outa have "been supplied to the B.A.A. for stars north of the equator iwhich n they and the V.S.S. combine data. They are having some problems in bringing their processing up to date but these will be overcome, and they have supplied us with some earlier observations. John Isles retired as Director of the Variable Star Section, B.A.A. and I would like to thank him for the long and pleasant association over so many years. I am certain that the same close co-operation will be established with his succesor.

R CrB VARIABLES. W e have continued to send S.A.A.O. alert notices whenever one of these stars has faded.

The foregoing are additional to many routine programmes that have continued with many professionals for years. Abby Jones has observed variables not on our regular programme for requests from Ed. Budding, Peter Cottrell and Warwick Lawson. He was co-author with Warwick Lawson for apaper published i n the OBSERVATORY.

8. CHARTS FOR SOUTHERN VARIABLES. 23 Series was published by ASTRONOMICAL RESEARCH LTD. Series 24 will be issued during 1993. As usual the drafting of a l l charts has been done by Mati Morel, who has maintained his very high standard.

9. SEQUENCE MAGNITUDES.

There i sstill need for reliable magnitudes in many variable star fields. During the year, as arranged with Alan Gilmore and Pam Kilmartin John(Mt. University Observatory) I prepared two lists of the fields con• cerned. The first listed a limited number of fields for which the requirement i s urgent and the second listed a number of fields from charts issued over the past several years. I t ishoped that as time permits it will be possible for Alan and Pam work to through these lists. Dr. Tom Richards has supplied preliminary charts on request from the G.S.C. and especially for Novae as they have been discovered. These were distributed by fax followed later by charts prepared Mati by Morel. We are indebted to Alan Gilmore and Pam K i l m a r t i n fo r supplying V magnitudes for these novae, discovered by Paul Camilleri and Bill Liller.

10. FUTURE OF THE V.S.S. Members and myself have been concerned for some time about the future direction of the V.S.S. after I go. Late i n 1992 Icirculated two Circulars to selected senior members. One s e t out what the V.S.S. does and how i t operates; the other listed a number of options for the future. 94.

FUTURE OF THE V.S.S. (Cont.) The replies received to date show agreement on some points, whilst other members have requested more time to consider the problems raised.

The points of agreement are:

(a) That, despite the fact that Abby Jones is Deputy Director, it would be most undesirable he i fhad to shoulder the routine running of the Section. This recognises the fact that i he f had t o do so it would mean either t h e end o f h i s observing or a considerable curtail• ment thereof. Everyone agrees that this would not be desirable considering hispre-eminence as an observer.

(b) There is also agreement that the Section should continue to be directed from New Zealand and/or Australia and that amalgamation with any similar foreign organis• ation should not be considered under any circumstances.

(c) There is a definite preference for Option No. 2, i.e. the establishment of a permanent Headquarters with sufficient finance to employ at least one permanent staff member.

(d) Failing ( c ) being impossible there is, so far, agreement that Options 3 or 4 should be chosen, i.e. to find a person, or group, to eventually take over. I t i s suggested that thef o r sake of the reputation of New Zealand astronomy the V.S.S. should continue to operate from New Zealand but i f that i s not possible then from Australia.

At this stage I refrain from comment pending the receipt of replies from members who requested more time to consider the problem, except to say that the professionals I consulted are in agreement with the conclusions of members.

11. HEADQUARTERS.

There has been a marked increase i n the number of observers wishing to take up visual observation of Variable Stars, especially in Australia. This interest has been to a great extent stimulated by Peter Williams with his regular articles on Variable Stars. Fraser Farrell has been responsible for forming an active group in Adelaide.

The result of this interest i s that supplies of the 4 -th edition of "THE OBSERVATION OF VARIABLE STARS" i s now exhausted. The 5th edition will be written in 1933 which will also include instructions from Ranald Mcintosh on the format in which observations should be submitted on diskettes. This is necessary a s more observers now submit their results on diskettes and this tendency is likely to increase i n the future. 95.

HEADQUARTERS (Cont.) The financial donations acknowledged earlier in this report has permitted Maureen Phizacklea to be employed throughout the year which has been a great help t o me. Maureen now has acquired the experience that has allowed m e t o leave the accountancy work t o he r as well as the production of the Monthly Circulars on our computer. She also transcribes from the Dictaphone nearly all the very large volume of correspondence.

The special grants acknowledged earlier in this report will greatly facilitate the publication of light curves of which there now i sa large accumulation due to the work o f Don Brunt, Bill Goltz and Ranald Mcintosh.

Over the next few months I will be concentrating on this work which may mean some delay in answering letters but the objective is to have a l l data published at least to the end of 1991. If this can be attained imeans t that any successor will only have to deal with current data especially when records that have already been published are transferred to La Trobe. Last year I referred to the problems of space at head• quarters. The situation now reminds m e o f what m y wife said years ago .. "One day I can see al l your papers being inside and we will be outside in the garden!"

I will not elaborate further on the work at headquarters since all members have been kept informed on what goes on through "CHANGING TRENDS". ACKNOWLEDGEMENTS First and foremost I wish to thank a l l observers for their observations. Your efforts be the number of observations large or small, are why the Section exists. The care and high standards you al l maintain are why the V.S.S. has acquired such a high reputation. In particular I thank Danie Overbeek and Abby Jones for their outstand• ing observations.

M y special thanks go t o Ranald Mcintosh for h i s wonderful processing of observational results on his computer and the light curves he produces with such cheerfulness and alacrity. Don Brunt has kindly continued to process the earlier data at an almost alarming rate. Bill Goltz has also given valuable assistance in this. I a m indebted to Jan Hers, Director of the Southern African Section for his co-operation and sending their estimates on diskettes. Peter Nelson, Fraser Farrell and Sue Dreves are thanked both for their support and for stimulating interest in observing in their respective Australian groups. 96.

ACKNOWLEDGEMENTS (Cont.)

As always I appreciate the very high standard maintained by Mati Morel in chart production and his continued support and assistance to observers.

Tom Richards has provided rapid and prompt preliminary charts for novae and for other variables on request.

Alan Gilmore and Pam Kilmartin have given the Section invaluable assistance by providing sequence magnitudes. Without their help and friendship the Section would be much poorer.

Dich Hull has, as always, supplied the Julian Date calendar distributed with the last issue of CHANGING TRENDS.

M y appreciation is expressed to the many professionals who have supported the Section as well as finding our results useful.

M y sincere appreciation goes to Maureen Phizacklea for so cheerfully and efficiently coping with a varied and at times perplexing work load.

Finally m y grateful thanks are extended to all members and supporters for their friendships and assistance i n so many ways.

1992 December 31 Frank M . Bateson DIRECTOR 97. VSS OBSERVATIONS RECEIVED FOR YEAR ENDED 1992 AUGUST 31

Observer Obs. code Obs. total 5245 Albrecht, W.M.B. A d Brown, N.J. B A 106 Bryant , K. Bk 53 Bennie, I.D. BN 4 Boattini, A. BS 334 Blane, D . Bz 1170 Cooper, T. CH 1581 Cragg, T.A. CJ 2464 Cook, J.C. CJ 63 Camilleri, P. CM 200 D e Beer, G. DE 52 Dreves, Dr. S. Dx 1052238 Farrell, F. Fm Goltz, W. Gp 6698 Geyser, M.J. Gq 49 Herdman, G. HA 1337 Hernshaw, C. H H 703 Harries-Harris, E. Hi 889 Hull, O.R. HI 4285 Hers, J . Hz 680 Ives, F. Iv 895 Jooste, J.L. Jf 33 Jones, R.W. Js 1962 Jones, A.F. Jo 15966 Kent, Mrs. K.E. Kn 62 Lumley, E . Lm 331 Leslie, Mrs. A. La 71 Menzies, B. Mf 540 Murray, A.M. MG 247 Monard, L.A.G. MIA 333 Morel, M. Mv 19 Nelson, P. Nl 826 O'Kane, J . Ok 1732 Orchiston, Dr. W. Or 199 Overbeek, M.D. Ov 21326 Park, J. Pj 196 Robinson, 9. RB 297 Richards, T. Ri 122 R N 22 Stabenow, R. SE 344 Stephanopoulos, G . SK 108 Smit, Dr. J.A. SP 913 Skilton, .P. SU 193 Turner, D . Tq 129 Tregaskis, T.B. Tr 883 Taylor, D r . N.W. Ty 2198 Venimore, C.W. Ve 1734 Villar, W . Vf Van Blommestein, P. Vn 9 Watson, Mrs. D. WJ 363 Williamson, L.J. W m 395 Wadhwa, S.S. WM 52 Walsh, S. WP 229 Warnes, P. WQ 51 Ward, R. Wr 38 Williams, P. Wy 3038

TOTAL: 76299 98.

Variable Star Section Observations 1991/92

S e p t 9 1 O c t 9 1 N o v 91 D e c 9 1 J a n 9 2 F e b 9 2 M a r 9 2 April 9 2 M a y 9 2 J u n 9 2 J u l 9 2 A u g 9 2