Photometry of the Peculiar Population II Cepheid RU Camelopardalis (1966-1982) B. SZEIDL, K. OLÁH, L. SZABADOS, K. BARLAI and L. PATKÓS Abstract Photoelectric photometry of RU Cam was carried out at Konkoly Observatory on 1343 nights between 1966 and 1982. 1453 observations both in V and B and 30 observations in U have been published. Using all available data the period and light curve changes of the star have been investigated. A slight continuous period decrease took place between 1907 (P = 22.19 days) and 1965 (P = 22.07 days). After 1965 the period has become very unstable and fluctuated between 17.4 and 26.6 days. It happened several times (probably at irregular time intervals) that after a short-lived recovery phase the amplitude decreased again and the light variation almost disappeared. The light curve also showed that there were time intervals when the fight varied irregularly and the count of epoch numbers became very uncertain. The photoelectric data obtained in the years 1965-1982 have been Fourier- analysed. There was no indication for modulation effects. A number of peaks appeared in the spectrum around f = 0.046 cycle/day suggesting that stochastic or chaotic characters have become dominant in the star's pulsation. 1. Introduction Although the peculiar behaviour of RU Camelopardalis was known before 1966, it was regarded as a normal Population II Cepheid. The only strikingly abnormal characteristics in its spectrum discovered as early as in 1919 (Joy, 1919, Cannon, 1920) was that the carbon features were clearly marked. Its spectral type at minimum light was R0 (Sanford, 1927, 1928) or C6_2 (Keenan and Morgan, 1941) or C3_2e (Bidelman, 1954), while at maximum light it was close to K0. The hydrogen lines were in emission near median magnitude on the rising branch of the light curve and at velocity maximum between the 3rd and 6th days after minimum light (Sanford, 1928; Jehoulet, 1954; Climenhaga, 1960). The radial velocity measurements showed evidence of stratification effects and the presence of an expanding chromosphere was indicated by the high negative velocity of the emission components of CaII H and K (Faraggiana and Hack, 1967a, b). In spite of the fact that RU Cam is a Population II star, it is not metal poor, the metal abundance is almost normal, with a slight excess of a factor of 2 or 3 for Ca, Ti, V, Ni and the rare earths with respect to Fe. The star is not H poor either and the excess of carbon is not larger than 2 or 3 (Faraggiana and Hack, 1967b). The high abundance of C3 (relative to C2) (Faraggiana and Hack, 1967b; Climenhaga, 1960) produced by the carbon cycle indicates that RU Cam is in an advanced evolutionary state. In the beginning of 1966 Demers and Fernie (1966) reported that they were unable to detect light variations in RU Cam exceeding 0.1-0.2 mag but the star was apparently still unstable with irregular fluctuations of the order of 0.2 mag. This observation initiated a series of speculations about ceasing pulsation in RU Cam. Since the star showed strong irregular changes in the past, too, there was some suspicion that the star did not stop pulsating, only the amplitude of its light variation decreased temporarily. Detre (1966) even suggested cyclic amplitude variations and predicted the increase of amplitude. Following Demers and Fernie's announcement photoelectric photometry of RU Cam was commenced at some observatories (Wamsteker, 1966, 1968; Cester, 1967, 1968, 1969; Broglia, 1967, 1969; Broglia and Guerrero, 1969a, b, 1971, 1972a, b, 1973; Broglia et al., 1978, Fernie and Watt, 1967; Fernie, 1968; Zaitseva, 1967, 1968; Zaitseva and Ljutiy, 1969, 1971, 1978; Zaitseva et al., 1973, Kovalenko, 1974), in order to investigate the peculiar behaviour of the star. The photoelectric observations at Konkoly Observatory were started in August, 1966. As to a brief historical overview, the light variability of RU Cam (BD +69°417 (8.5) = HD 56167 (K0) = 2.1907) was discovered by Mme L. Ceraski on Blazhko's plate collection obtained between 1899-1906 (Ceraski, 1907). Using his visual estimates of 1907 and photographic observations obtained in the years 1904-1906, Blazhko (1907) determined the period of light variation and gave the elements for maximum light: Max. = J.D. 2417620.0 + 22.27dxE. Luizet (1907, 1912), Ichinohe (1909), Shapley (1913), Silva (1922), Leiner (1923, 1929), Haas (1923), Edelberg (1932), Florja and Kukarkina (1953), published visual or photographic estimates, while Lenouvel and Jehoulet (1953), Lenouvel and Dagouillon (1954), Eggen et al. (1957), Lenouvel and Fiogére (1957), Delsemme and Delsemme-Jehoulet (1958), Michalowska-Smak and Smak (1965), Mitchell et al. (1964), Williams (1966) and Smak (1966) published photoelectric observations of RU Cam obtained prior to Demers and Fernie's announcement. Leiner (1923) already suspected that the light curve of RU Camelopardalis varied from cycle to cycle and the period of the star was also changing. Further investigations (Haas, 1923; Leiner, 1929; Edelberg, 1932; Nielsen and Sjögren, 1943) confirmed this suspicion. Although the star was included in the general list of Cepheid variables, Robinson (1933) called the attention to the peculiarities of RU Cam in its spectrum, light curve, period and radial velocity. He supposed that between these peculiarities certain interrelationships existed but did not see any reason to exclude this star from the list of Cepheids. Payne- Gaposchkin (1941) noted that W Virginis resembled RU Cam in the shape of light curve, the variation of period, the correspondence between light and velocity curves, and the occurrence of bright lines at and following the minima. The complex character of the variability of RU Cam during the 50's and early 60's was traced back on Sonneberg archival plates (Huth and Wenzel, 1966; Huth, 1966, 1967) and Huth ascertained that the light amplitude of the star might undergo considerable changes within several months. The large irregularities in the light variation of this object were obvious from a mere visual inspection of the time series of its luminosity, and it was also clear that the cycle length was also undergoing irregular fluctuations. Parallel with the irregular behaviour of the light variation the radial velocity changes of the star showed complex character (Demers and Crampton, 1966; Wallerstein and Crampton, 1967). During the period when the amplitude was smaller than 0.05 mag, no emission lines were visible in the spectrum of the star and its radial velocity seemed to be constant and approximately equal to Sanford's gamma velocity (Sanford, 1928). Wallerstein (1968) investigated the atmospheric parameters of the star during this "quiescent" period in the early 1965. Lloyd Evans (1983) suggested that there might be a possible connection between extreme irregularity and the occurrence of an overabundance of carbon in RU Cam. 2. Observations The photoelectric photometry of RU Camelopardalis was started by L. Detre and one of the authors of the present paper (Detre and Szeidl, 1967) at Konkoly Observatory on August 10, 1966. The observations were carried out by the observatory's 24 in. telescope at Budapest and by the 20 in. telescope at Piszkéstető Mountain Station. At Budapest the photometer was equipped with an unrefrigerated EMI 9502B photomultiplier and Schott filters UG1 for the U, BG12+GG13 for the B and GG11 for the V band and was placed at the Newtonian focus (f/6) of the 24 in. telescope. Since 1972 photoelectric observations have also been obtained by the 20 in. Cassegrain telescope (f/15) at Piszkéstető. At this location we used an integrating photometer equipped with an unrefrigerated EMI 9058QB photomultiplier and the following Schott filters: UG2 in U, BG12+GG13 in B and GG11 in V. BD +70°448 was used as the main comparison star. Several other stars were also observed in order to check the constancy of the main comparison and to determine the transformation coefficients. Tie-in observations of the comparison stars were made on six nights and Table 1 presents the results of these observations. Their errors are about 0.01 mag in V and B and 0.03 mag in U. Table 1 Brightness and colours of the comparison stars star V B-V U-B BD +69°420 = HD 57201 (F8) 8.906 +0.506 +0.055 BD +69°422 = HD 57308 (GO) 8.021 +0.801 +0.487 BD +70°447 = HD 56323 (F5) 9.056 +0.326 +0.072 BD +70°448 9.059 +1.090 +0.934 In order to get a judgement about the accuracy of the brightness and colours of the main comparison star all these values obtained by different observers for BD +70°448 are collected in Table 2. The agreement between the different observers is fairly good. During 1343 nights 119, 7597 and 7597 observations were made in U, B and V, respectively at Konkoly Observatory. The observations have been corrected for atmospheric extinction and transformed into the UBV system in the traditional way. Each observing run mostly consisted of six observations which were composed into normal values. In this way 30 normal points were obtained in U and 1453 normal values in both B and V. Table 2 Magnitudes and colours of BD +70°448 in other studies V B-V U-B source 9.09 +1.10 +0.98 Lenouvel & Fiogére, 1957 9.058 +1.092 +0.972 Michalowska-Smak & Smak, 1965 9.09 +1.09 Cester, 1967 9.083 +1.077 +0.957 Fernie & Watt, 1967 9.090 +1.089 Cester, 1968 The B and V normal values are given in Table 3 and the U values in Table 4 (see on pages 273-300). The Julian Dates of the observations obtained at Piszkéstető are marked by asterisks. Tables 3 and 4 also present the number of observations (n), the r.m.s. errors, the B - V colour indices and the average zenith distance at the observations. In order to cover the light curve of RU Camelopardalis as fully as possible, the star was observed during the nights of poor quality, as well, and this circumstance explains the lower precision of some of the normals. During the period of our observations (J.D. 2439348 - 2445260) photoelectric photometry of RU Cam was carried out at other observatories, as well. Since there are a number of common nights of observation our photometry can be compared with that of others. While comparing the observations we supposed that the changes in brightness of RU Cam during a night may be neglected. We have 243 common nights of observation in V and 204 in B with Broglia et al., (Broglia, 1969; Broglia and Guerrero, 1969b, 1972a, 1973; Broglia, Conconi and Guerrero, 1978). They used the same comparison star as we did but they accepted Lenouvel and Fiogére's (1957) magnitudes and colours for it. Taking into account the differences in the accepted magnitudes of the comparison star we came to the conclusion that the average systematic differences (zero point shifts) between Broglia et al.'s and our observations in V and B are: mean Delta V = n^(-1) Summa Delta V_i = -0.0002 mag, sigma(V) = Sqrt[(n - 1)^(-1) Summa (Delta V_i)^2] = 0.0125, mean Delta B = n^(-1) Summa Delta B_i = 0.0000 mag, sigma(B) = Sqrt[(n - 1)^(-1) Summa (Delta B_i)^2] = 0.0147, The distributions of the Delta V_i and Delta B_i values are nearly normal and are shown in Figure 1. The above results indicate that our observations fit in well with that of Broglia et al. A comparison with Cester's (1968, 1969) observations led to a similar result. There were 38 and 39 common nights of observation in V and B, respectively. The zero point shifts between his and our V and B are: mean Delta V = +0.0007 mag, sigma(V) = 0.0148, mean Delta B = +0.0038 mag, sigma(B) = 0.0212.
Figure 1. The distribution of the Delta V_i and Delta B_i values
The conformity between Cester's and our observations in V is also good,
however in B it is not quite satisfactory, but still acceptable. The
comparison of Cester's and Broglia et al.'s observations resulted in the
same conclusion.
Wamsteker (1968) observed the star only in yellow light and had 11
common nights of observation with us. Comparing his observations to ours
an average difference of:
mean Delta V = -0.0035 mag, sigma(V) = 0.0061
can be deduced in the characteristic parameters. These values indicate
that Wamsteker's photometric system is close to ours.
Fernie (1968) published 50 observations in V, and 49 ones in B (one of
them, on J.D. 2439646 may be misprinted in his Table). There were 14
common nights of observation in V and 13 in B. The comparison to our
observations gave the following results:
mean Delta V = +0.0091 mag, sigma(V) = 0.0204,
mean Delta B = -0.0137 mag, sigma(B) = 0.0263.
The difference between Fernie's and our photometric systems is
significant, although the discrepancy can partly be attributed to the fact
that the times of observation of the common nights usually differed by
more than eight hours.
Zaitseva and Ljutiy (Zaitseva, 1967, 1968, Zaitseva and Ljutiy, 1969,
1971, 1978) observed the star between 1966 May and 1975 May on 206 nights
of which 95 were common with ours. The comparison of the observations of
the common nights resulted in:
mean Delta V = +0.0154 mag, sigma(V) = 0.0209,
mean Delta B = -0.0025 mag, sigma(B) = 0.0230.
The differences between the two photometries are rather large, both
significant systematic and large random differences occur.
To sum up the discussion about the photometries carried out during the
time interval covered by our observations we conclude that Broglia et
al.'s, Cester's and Wamsteker's photometry is in accord with ours, while
Fernie's (and co-workers') as well as Zaitseva and Ljutiy's photometry
differs from ours rather significantly. Therefore the latter two
photometries are only used in the further discussion for lack of other
photoelectric observations. Figure 2a-i presents our V observations
(dots) and those of Broglia et al., Cester and Wamsteker (crosses).
3. Period changes and discussion
Since the discovery of the variability of RU Cam a great number of visual,
photographic and photoelectric observations have been collected for the
star. As the light minima are sharp and usually well-defined unlike the
light maxima which are broad and blunt, the period changes of the star can
be examined more exactly from the times of minima. Table 5 contains all
the available times of minima prior to the remarkable amplitude decrease
in early 1965. The O-C_1 values are computed by the formula:
C_1 = J.D. 2417610.5 + 22.16dxE_1.
Although changes in the period (either abrupt or smooth) occurred several
times, but on the average, the period P = 22.16 days held on during the
time interval J.D. 2412868 - J.D. 2438680 (1874 February - 1964 October).
The O-C_1 residuals are plotted against time in Figure 3. The abrupt
changes in the period might occur at around J.D. 2421000, J.D. 2423000,
J.D. 2426300, J.D.2434500 and J.D. 2437000 (see the study of period
changes in detail by Huth, 1967), though continuous and/or erratic changes
cannot be excluded. Moreover, Leiner (1929) found jumps in the phase of
minima. He observed a phase shift of 1 1/2 days at the end of 1922. If we
assume that the period fluctuations (P_i - mean P) may be regarded as random
variables with zero mean and that the stochastic process is stationary,
the O-C diagram consisting of cycles of different lengths and amplitudes
can take its origin from the accumulation of random fluctuations in the
period (e.g. Sterne, 1934, or Balázs-Detre and Detre, 1966). By all means,
however, a systematic period decrease can be presumed from 1907 (P = 22.19
days) till 1965 (P = 22.07 days).
The photoelectric observations made at Konkoly Observatory and those
available in the literature were used to determine the moments and
magnitudes of light minima and maxima for the V band. In order to derive
the times and magnitude values as accurately as possible, parabolas were
fitted to the observations around minima and maxima. The results are given
in Table 6 and Table 7, respectively.
Figure 2a. Photoelectric V observations (dots: Konkoly observations)
Figure 2b. The same as Fig. 2a.
Figure 2c. The same as Fig. 2a.
Figure 2d. The same as Fig. 2a.
Figure 2e. The same as Fig. 2a.
Figure 2f. The same as Fig. 2a.
Figure 2g. The same as Fig. 2a.
Figure 2h. The same as Fig. 2a.
Figure 2i. The same as Fig. 2a.
Table 5
Times of minima prior to the amplitude decrease of 1965
t_min E_1 O-C_1 References
2400000+
12868 v -214 -0.3 K07
13601 v -181 1.5 K07
17610.5 v 0 0.0 B07
17655.2 v +2 0.4 L07; L12; I09
17676.5 v 3 -0.5 I09; S13 (E.S. Haynes)
17699.1 v 4 0.0 L07; L12; S13 (E.S. Haynes)
17722.0 v 5 0.7 I09; S13 (E.S. Haynes)
17743.9 v 6 0.4 L07; L12; I09
17766.7 v 7 1.1 L07; L12; S13 (E.S. Haynes)
17788.2 v 8 0.4 S13 (E.S. Haynes)
17831.9 v 10 -0.2 I09 (N36)
17855.1 v 11 0.8 S13 (E.S. Haynes)
17943.6 v 15 0.7 S13 (E.S. Haynes)
17966.0 v 16 0.9 I09; S13 (E.S. Haynes)
18010.8 v 18 1.4 S13 (E.S. Haynes)
18032.1 v 19 0.6 S13 (E.S. Haynes)
18054.3 v 20 0.6 S13 (E.S. Haynes)
18077.0 v 21 1.1 S13 (E.S. Haynes & F.H. Seares)
18099.0 v 22 1.0 S13 (E.S. Haynes & F.H. Seares)
18121.2 v 23 1.0 L12; S13 (E.S. Haynes & F.H. Seares)
18143.8 v 24 1.5 L12; S13 (E.S. Haynes & F.H. Seares)
18232.0 v 28 1.0 L12
18364.5 v 34 0.6 L12; S13 (E.S. Haynes)
18387.4 v 35 1.3 S13 (E.H.Haynes)
18519.0 v 41 -0.1 L12
18586.7 v 44 1.2 L12
18651 47 -1.0 Y16
18719.5 v 50 1.0 L12 (N36)
18741.9 v 51 1.2 L12
18763.2 v 52 0.4 L12
18786.9 v 53 1.9 L12
18940.0 v 60 -0.1 L12
18963.0 v 61 0.7 L12
19051.9 v 65 1.0 L12
19074.8 v 66 1.7 L12
19140.7 v 69 1.2 L12
19229.6 v 73 1.4 L12
19252.0 v 74 1.7 L12
19339.8 v 78 0.8 L12
19450.4 v 83 0.6 L12
19474.4 v 84 2.5 L12
19496.9 v 85 2.8 L12
19539.7 v 87 1.3 L12
20117.6 v 113 3.0 S22
20428.7 v 127 3.9 S22
20494.3 v 130 3.0 S22
20561 133 3.2 Y16
20958.4 v 151 1.7 S22
22178.0 v 206 2.5 L23
22266.5 v 210 2.4 L23
Table 5 (cont.)
t_min E_1 O-C_1 References t_min E_1 O-C_1 References
22355.3 v 214 2.6 L23 26748.4 pg 412 8.0 H67
22443.3 v 218 1.9 L23 27081.2 v 427 8.4 P56
22487.4 v 220 1.7 L23 (S28) 27214.7 pg 433 8.9 H67
22531.5 v 222 1.5 L23 28076.4 v 472 6.4 L38
22576.4 v 224 2.1 L23 (S28) 28519.4 v 492 6.2 K37
22619.8 v 226 1.1 L23 29382.4 v 531 4.9 NS41
22641.8 v 227 1.0 L23 (S28) 30002.9 v 559 5.0 N52
22708.6 v 230 1.3 L23 (N36) 30201.8 v 568 4.4 NS43
22797.2 v 234 1.3 L23 30314.3 v 573 6.1 M64
22818.6 v 235 0.5 L23 (S28) 30334.3 v 574 4.0 M64
22841.7 v 236 1.4 L23 (S28) 30623.4 v 587 5.0 M64
22885.6 v 238 1.0 L23 30645.3 v 588 4.7 M64
22907.8 v 239 1.1 L23 (S28) 31044.1 v 606 4.6 N52
22930.1 v 240 1.2 L23 (S28) 31996.3 v 649 4.0 N52
22974.4 v 242 1.2 L23 32217.8 v 659 3.9 LJ53 (P. Ledoux)
23085.1 v 247 1.1 L23 32771.0 v 684 3.1 N55
23129.4 v 249 1.1 L23 (S28) 32859.7 pe 688 3.1 E57
23173.4 v 251 0.7 L23 32968.3 pg 693 0.9 H67
23240.2 v 254 1.1 L23 33568.2 pg 720 2.5 H67
23261.9 v 255 0.6 H23(S28;N36)33656.1 pg 724 1.8 H67
23283.4 v 256 -0.1 L23 (S28) 33678.5 pg 725 2.0 LJ53 (B.S.Whitney)
23328.7 v 258 0.9 L23 33744.8 v 728 1.8 N55
23440.9 v 263 2.3 L29 34010.4 v 740 1.5 N55
23529.4 v 267 2.2 L29 34076.4 pe 743 1.0 LJ53
23618.1 v 271 2.2 L29 34298.7 pg 753 1.7 H67
23706.6 v 275 2.1 L29 34430.8 pe 759 0.9 LD54
23750.7 v 277 1.9 L29 (N36) 34652.5 pg 769 1.0 H67
23839.7 v 281 2.2 L29 34696.5 pe 771 0.6 LD54
24105.5 v 293 2.1 L29 35052.6 pg 787 2.2 H67
24282.3 v 301 1.6 L29 35362.8 pg 801 2.1 H67
24616.8 v 316 3.7 L29 35539.8 pe 809 1.9 LP57
24683.3 v 319 3.8 L29 35605.0 pg 812 0.6 H67
24772.5 v 323 4.3 L29 35895.0 pe 825 2.5 DJ58
25039.6 v 335 5.5 L29 (N36) 35917.2 pe 826 2.5 DJ58
25173.5 v 341 6.4 L29 36005 v 830 1.7 AAVSO(N.O. Hutchings)
25306.1 v 347 6.1 L29 36073 v 833 3.2 AAVSO(N.O. Hutchings)
25417.2 v 352 6.4 L29 36161.0 pg 837 2.6 H67
25461.9 v 354 6.8 L29 36227.2 pg 840 2.3 H67
25484.3 v 355 7.0 L29 36316 v 844 2.5 AAVSO(N.O. Hutchings)
25506.3 v 356 6.8 E32 36603.4 pg 857 1.8 H67
25528.1 v 357 6.5 E32 36958.2 pg 873 2.0 H67
25617.2 v 361 6.9 E32 37024.5 pe 876 1.8 Mi64
25683.3 v 364 6.6 N30 37401.2 pg 893 1.8 H67
25706.0 v 365 7.1 E32 37577.4 pg 901 0.7 H67
25862.1 v 372 8.1 E32 37731.6 pg 908 -0.2 H67
25884.2 pg 373 8.0 H67 37775.5 pe 910 -0.6 MS65
25994.3 v 378 7.3 E32 37886.5 pg 915 -0.4 H67
26040.6 pg 380 9.3 H67 38085.6 pg 924 -0.7 H67
26416.5 pg 397 8.5 H67 38284.3 pg 933 -1.5 H67
26439.0 v 398 8.8 E32 38415.5 pg 939 -3.2 H67
26483.0 v 400 8.5 E32 38504.4 pg 943 -3.0 H67
26571.3 v 404 8.2 E32 38680.4 pg 951 -4.3 H67
26594.5 v 405 9.2 E32
References: K07 = Kreutz 1907; B07 = Blazhko 1907; L07 = Luizet 1907; L12
= Luizet 1912; I09 = Ichinohe 1909; S13 = Shapley 1913; Y16 = Yendell
1916; S22 = Silva 1922; L23 = Leiner 1923; L29 = Leiner 1929; H23 = Haas
1923; S28 = Sanford 1928; N30 = Nielsen 1930; N36 = Nielsen 1936; N52 =
Nielsen 1952; N55 = Nielsen 1955; E32 = Edelberg 1932; K37 = Krebs 1937;
L38 = Larson 1938; NS41 = Nielsen & Sjögren 1941; NS43 = Nielsen & Sjögren
1943; LJ = Lenouvel & Jehoulet 1953; LD54 = Lenouvel & Daguillon 1954; E57
= Eggen et al. 1957; LF57 = Lenouvel & Fiogére 1957; DJ58 = Delsemme &
Delsemme-Jehoulet 1958; P56 = Parenago 1956; M64 = Model 1964; Mi64 =
Mitchell et al. 1964; MS65 = Michalowska-Smak & Smak 1965; H67 = Huth 1967
Figure 3. O-C_1 diagram of RU Cam
Although most observers took note of light curve changes of RU Cam,
especially in the depth of the light minima (sometimes it reached 0.5 mag.)
and called attention to the peculiarities of RU Cam (Silva, 1922;
Leiner, 1923, 1929; Haas, 1923; Edelberg, 1932, Robinson, 1933;
Nielsen and Sjögren, 1943) no one realized the star's extreme nature
until the announcement of Demers and Fernie (1966). They observed the
unprecedented amplitude decrease of the star in 1965.
After the 1965 event the period of the star has become very unstable
and fluctuated between 17.4 and 26.6 days. Figure 4 presents the frequency
distribution of the observed P_i = t^min_i+1 - t^min_i periods since 1965.
The values of the period usually fell into the 20-24 day time interval
with an average value of 21.75 days. After 1965 the O-C residuals have
been computed by the formula:
C_2 = J.D. 2439079.6 + 21.75dxE_2
where E_2 = E_1 - 969. The O-C_2 diagram (Figure 5) also shows that the
period underwent large fluctuations, especially during the times when the
amplitude of the light variation
Figure 4. Frequency distribution of the observed P_i periods since 1966
Figure 5. O-C_2 diagram of RU Cam
Table 6
Times and brightness of minima from photoelectric V observations
t_min m^min_v E_2 O-C_2 References t_min m^min_v E_2 O-C_2 References
2400000+ 2400000+
32859.7 9.09 -281 -108.2d E57 40460 8.62 63 10.2d Pp
34076.4 9.15 -226 -87.7 LJ53 40482.4 8.603 64 10.8 Pp
34430.8 9.27 -210 -81.3 LD54 40504.8 8.591 65 11.4 Pp; BG72
34696.5 9.26 -198 -76.6 LD54 40525.9 8.550 66 10.8 Pp; BG72
35539.8 9.17 -160 -59.8 LF57 40547.1 8.540 67 10.3 Pp
35895.0 9.58 -144 -52.6 DJ58 40568.5 8.578 68 9.9 BG72
35917.2 9.60 -143 -52.1 DJ58 40588 8.53 69 7.7 Pp; BG72
37024.5 9.11 -93 -32.3 M64 40609.2 8.574 70 7.1 Pp; BG72
37775.5 9.77 -59 -20.9 MS65 40629.9 8.555 71 6.1 Pp; BG72
39079.6 8.61 0 0.0 W66 40652.0 8.567 72 6.4 Pp; BG72
39272.6 8.55 9 -2.8 Z67 40673 8.56 73 5.6 BG72
39364 8.55 13 1.7 Pp 40692.6 8.546 74 3.5 Pp; BG72
39385.4 8.568 14 1.3 Pp 40718.0 8.526 75 7.1 Pp; BG72
39408.4 8.548 15 2.6 Pp 40739.5 8.544 76 6.9 BG72
39431 8.52 16 3.4 W68 40761.0 8.550 77 6.7 Pp; BG72
39453.7 8.514 17 4.4 Pp 40783 8.54 78 6.9 Pp; BG72
39475 8.52 18 3.9 Pp; B69 40807 8.51 79 9.2 Pp; BG72
39493.7 8.559 19 0.9 Pp; C68 40831 8.51 80 11.4 Pp
39518.9 8.595 20 4.3 Pp 40853.0 8.476 81 11.6 Pp; BG73
39539.4 8.602 21 3.1 Pp; B69 40872.7 8.506 82 9.6 Pp; BG73
39559.9 8.582 22 1.8 Pp 40893.6 8.554 83 8.7 Pp; BG73
39580.8 8.581 23 0.9 Pp; B69 40915.6 8.588 84 9.0 BG73
39601.7 8.593 24 0.1 Pp; C68; B69 40938.3 8.611 85 9.9 Pp; BG73
39625.3 8.589 25 1.9 Pp; B69 40958.9 8.610 86 8.8 Pp; BG73
39646.5 8.628 26 1.4 Pp 40981.5 8.533 87 9.6 Pp; BG73
39667.9 8.639 27 1.0 Pp; B69 41000.0 8.504 88 6.4 Pp; BG73
39689.8 8.620 28 1.2 Pp; B69 41020.0 8.503 89 4.6 Pp; BG73
39712.9 8.685 29 2.6 Pp 41037.4 8.504 90 0.3 Pp; BG73
39735.3 8.666 30 3.2 Pp 41058.3 8.516 91 -0.6 Pp
39757.0 8.624 31 3.2 Pp 41076.6 8.539 92 -4.0 Pp
39780.9 8.613 32 5.3 Pp 41102 8.53 93 -0.3 ZL78
39802.0 8.615 33 4.6 Pp; W68 41125.5 8.580 94 1.4 Pp
39824.3 8.552 34 5.2 Pp; BG69 41147.1 8.565 95 1.2 Pp
39845.5 8.559 35 4.6 Pp 41169.5 8.607 96 1.9 Pp
39867.9 8.554 36 5.3 Pp; BG69 41190.5 8.606 97 1.1 Pp
39888.4 8.562 37 4.1 Pp 41214.6 8.568 98 3.5 Pp
39912.4 8.543 38 6.3 Pp; BG69 41236.3 8.575 99 3.5 Pp
39939.0 8.558 39 11.2 Pp; C69; BG69 41262.2 8.574 100 7.6 Pp
39964.5 8.563 40 14.9 Pp; C69; BG69 41283.6 8.561 101 7.2 Pp; BG73
39985.0 8.548 41 13.7 Pp; BG69 41305.0 8.604 102 6.9 Pp; BG73
40007 8.53 42 13.9 Pp 41344.1 8.635 104 2.5 BG73
40029.7 8.570 43 14.8 Pp; BG69 41364.9 8.639 105 1.6 Pp
40047.5 8.550 44 10.9 Pp 41407.8 8.604 107 1.0 Pp; BG73
40065^i) 8.51 45 6.7 Pp 41452.9 8.606 109 2.6 Pp; BG73
40085.2 8.562 46 5.1 Pp 41474.8 8.593 110 2.7 Pp; BG73
40105^ii) 8.57 47 3.2 Pp 41495.7 8.576 111 1.9 Pp
40150.5 8.54 49 5.2 Pp; C69 41519 8.58 112 3.4 Pp
40263.6 8.530 54 9.5 Pp 41542^iv) 8.56 113 4.6 Pp
40286^iii) 8.51 55 10.2 Pp 41600 8.53 116 -2.6 Pp
40436.9 8.624 62 8.8 Pp 41686.9 8.590 120 -2.7 Pp
Table 6 (cont.)
t_min m^min_v E_2 O-C_2 References t_min m^min_v E_2 O-C_2 References
2400000+ 2400000+
41707.2 8.63 121 -4.2d B78 42591 8.60 162 -12.1d Pp
41729.0 8.618 122 -4.1 B78 42684 8.63 166 -6.1 Pp
41750.9 8.609 123 -4.0 Pp; B78 42728 8.72 168 -5.6 B78
41773.7 8.627 124 -2.9 Pp; B78 42751.4 8.633 169 -4.0 B78
41795.6 8.644 125 -2.8 Pp 42774.9 8.623 170 -2.2 B78
41818.3 8.651 126 -1.8 Pp; B78 42797 8.59 171 -1.9 Pp; B78
41860.5 8.661 128 -3.1 B78 42817.8 8.534 172 -2.8 Pp; B78
42033.6 8.663 136 -4.0 Pp 42837.9 8.515 173 -4.4 Pp; B78
42097 8.60 139 -5.8 Pp 43164.5 8.595 188 -4.1 Pp; B78
42118 8.62 140 -6.6 Pp 43187 8.59 189 -3.4 B78
42141.5 8.637 141 -4.8 Pp 43209.4 8.571 190 -2.7 Pp
42162.6 8.701 142 -5.5 Pp 43230.3 8.592 191 -3.6 Pp
42205 8.71 144 -6.6 Pp 43250.6 8.533 192 -5.0 B78
42270.1 8.744 147 -6.7 Pp 43272.2 8.529 193 -5.1 B78
42291.9 8.770 148 -6.7 Pp 43293.9 8.593 194 -5.2 B78
42422.4 8.713 154 -6.7 Pp 43314.4 8.608 195 -6.4 B78
42445.1 8.679 155 -5.7 Pp 43335.0 8.647 196 -7.6 B78
42466.2 8.663 156 -6.4 Pp;B78 43379 8.59 198 -7.1 Pp
42486.7 8.660 157 -7.6 Pp 43424.2 8.617 200 -5.4 Pp
42529.6 8.580 159 -8.2 Pp;B78 43604.7 8.610 208 1.1 Pp
42550.6 8.569 160 -9.0 B78 45254 8.62 284: -2.6 Pp
References: LJ53 = Lenouvel and Jehoulet, 1953; LD54 = Lenouvel and Daguillon, 1954;
LF57 = Lenouvel and Fiogére, 1957; E57 = Eggen et al., 1957,
DJ58 = Delsemme and Delsemme-Jehoulet, 1958;
M64 = Mitchell et al., 1964; MS65 = Michalowska-Smak and Smak, 1965;
W66 = Wamsteker, 1966; Z67 = Zaitseva, 1967; W68 = Wamsteker, 1968;
C68 = Cester, 1968; C69 = Cester, 1969; B69 = Broglia, 1969;
BG69 = Broglia and Guerrero, 1969b; BG72 = Broglia and Guerrero, 1972a;
BG73 = Broglia and Guerrero, 1973; B78 = Broglia et al., 1978;
ZL = Zaitseva and Ljutiy, 1978; Pp = Present paper
Remarks:
i) The brightness of the star hardly varies.
ii) Nearly constant, irregular light variation between J.D. 2440110 and 2440145 (m_v~8.52).
iii) The star's brightness is nearly constant between J.D. 2440310 and 2440380 (m_v~8.48).
iv) From this time a slow increase occurs in brightness until J.D.2441595, no minimum
during this time period.
became very small. Figure 6 presents the brightness of maxima and minima
between J.D. 2439000 and J.D. 2443640. It can be seen from this figure
that it happened several times that after a short-lived recovery phase the
amplitude decreased again and the light variation almost disappeared (e.g.
around J.D. 2439450, J.D. 2440100, J.D. 2440850 etc.). From the light
curve (Figure 2) it is evident that the brightness of the star varied
nonperiodically between J.D. 2440050 and J.D. 2440150 as well as between
J.D. 2440320 and J.D. 2440380. The light was almost constant during this
latter time period. Between J.D. 2441540 and J.D. 2441595 there were
neither minima nor maxima and the stellar brightness was slowly
increasing. During these time intervals the count of epoch numbers is, of
course, very uncertain and jumps in phase could occur. In fact, such kind
of jumps had already been observed (e.g. Leiner, 1929).
Table 7
Times and brightness of maxima from photoelectric V observations
t_max m^max_v E_2 O-C_2 References t_max m^max_v E_2 O-C_2 References
2400000+ 2400000+
32824.2 8.28 -283 -100.2d E57 40493.7 8.320 64 22.1d Pp
34064.7 8.24 -227 -77.6 LJ53 40515.1 8.382 65 21.8 Pp; BG72
34421.2 8.15 -211 -69.1 LD54 40536.2 8.415 66 21.1 Pp
35905.2 8.13 -144 -42.4 DJ58 40557.8 8.435 67 20.9 Pp; BG72
37012.2 8.18 -94 -22.9 M64 40578.2 8.438 68 19.6 Pp; BG72
37698.0 8.20 -63 -11.3 MS65 40619.8 8.430 70 17.7 Pp; BG72
37964.0 8.22 -51 -6.3 Wi66 40640.8 8.429 71 16.9 Pp; BG72
39025.5 8.47 -3 11.2 W66 40661.9 8.415 72 16.3 Pp
39354.9 8.452 12 14.3 Pp; W66 40683.5 8.448 73 16.2 Pp; BG72
39375.7 8.459 13 13.3 Pp; W66 40705.4 8.438 74 16.3 Pp; BG72
39397.5 8.443 14 13.4 Pp; W66 40728.8 8.463 75 18.0 Pp; BG72
39419.6 8.468 15 13.8 Pp 40749 8.47 76 16.4 Pp; BG72
39443 8.47 16 15.4 Z67 40774 8.48 77 19.7 Pp; BG72
39463.6 8.422 17 14.2 Pp 40797.7^vii) 8.442 78 21.6 Pp; BG72
39481.9 8.465 18 10.8 Pp; C68 40819.3 8.425 79 21.5 Pp
39509.4^i) 8.485 19 16.6 Pp 40840.7 8.409 80 21.1 Pp
39529.6 8.485 20 15.0 Pp; C68; B69 40861.0 8.450 81 19.7 Pp; BG73
39551.1 8.464 21 14.8 B69 40881.6 8.444 82 18.5 Pp; BG73
39571.3 8.430 22 13.2 Pp; C68; B69 40903.0 8.484 83 18.2 Pp; BG73
39591.4 8.407 23 11.5 Pp; W68; B69 40928.4 8.449 84 21.8 Pp; BG73
39612.6 8.452 24 11.0 Pp; W68; B69 40947.6 8.410 85 19.2 Pp
39635 8.43 25 11.6 Pp; B69 40970.7 8.421 86 20.6 BG73
39656.4 8.399 26 11.3 Pp; B69 40991.9 8.441 87 20.0 BG73
39678.5 8.391 27 11.6 Pp 41011.0 8.456 88 17.4 Pp; BG73
39701.9^ii) 8.459 28 13.3 Pp 41026.7 8.475 89 11.3 Pp; BG73
39723.9 8.389 29 13.6 Pp 41047.7 8.477 90 10.6 Pp
39745 8.38 30 12.9 Pp 41067.5 8.472 91 8.7 Pp
39769.9 8.434 31 16.0 Pp; C69 41087.8 8.446 92 7.2 Pp
39791.2 8.434 32 15.6 Pp 41113 8.48 93 10.6 Pp
39813.6 8.423 33 16.3 Pp 41137.6 8.409 94 13.5 Pp
39834.0^iii) 8.412 34 14.9 Pp; Z68; BG69 41158.0 8.403 95 12.2 Pp
39857.2 8.400 35 16.4 Pp 41179.8 8.443 96 12.2 Pp
39880.2 8.424 36 17.6 Pp; BG69 41202.0 8.439 97 12.7 Pp
39902 8.48 37 17.6 Pp 41225.1 8.462 98 14.0 Pp
39924.3^iii) 8.475 38 18.2 Pp; C69; BG69 41249.4 8.384 99 16.6 Pp
39955^ii) 8.47 39 27.1 C69 41272.3 8.380 100 17.7 Pp; BG73
39974.6^iii) 8.481 40 25.0 Pp; C69; BG69 41293.7 8.372 101 17.3 Pp; BG73
39996.7 8.458 41 25.3 Pp; BG69 41314.8 8.439 102 16.7 Pp
40015.6^iv) 8.47 42 22.5 Pp; BG69 41334.5 8.479 103 14.6 Pp
40037.9 8.468 43 23.0 Pp; BG69 41354.3 8.436 104 12.7 Pp
40060 8.50 44 23.4 Pp; BG69 41396.5 8.445 106 11.4 Pp; BG73
40074 8.50 45 15.7 Pp 41418.3 8.484 107 11.5 Pp; BG73
40093.9^v) 8.519 46 13.8 Pp; BG69 41441.1 8.485 108 12.5 Pp
40159.3 8.449 49 13.9 Pp 41464.0 8.505 109 13.6 Pp; BG73
40181.6 8.424 50 14.5 Pp; BG69 41487.6 8.510 110 15.5 Pp; BG73
40206 8.42 51 17.2 Pp 41512^viii) 8.49 111 18.2 BG73
40252.5^vi) 8.410 53 20.1 Pp 41532.0^ix) 8.496 112 16.4 Pp
40426.5 8.420 61 20.1 Pp 41613 8.46 116 10.4 Pp
40448.2 8.328 62 20.1 Pp 41634.1 8.454 117 9.8 Pp
40471.7 8.344 63 21.8 Pp 41654.4 8.420 118 8.3 ZL78
Table 7 (cont.)
t_max m^max_v E_2 O-C_2 References t_max m^max_v E_2 O-C_2 References
2400000+ 2400000+
41675.6 8.394 119 7.7d Pp 42519.5 8.400 158 3.4d B78
41698.5 8.405 120 8.9 Pp 42560.1 8.454 160 0.5 Pp
41718.1 8.379 121 6.7 Pp; B78 42672.6 8.399 165 4.3 Pp
41739.5 8.406 122 6.4 Pp; B78 42694 8.37 166 3.9 B78
41762.3 8.386 123 7.4 B78 42716.0 8.466 167 4.2 Pp; B78
41784.5 8.393 124 7.9 Pp; B78 42740.2 8.411 168 6.6 Pp; B78
41806 8.38 125 7.6 Pp 42786.1 8.370 170 9.0 Pp; B78
41828.5 8.360 126 8.4 Pp; B78 42807.7 8.409 171 8.9 B78
41936.3 8.364 131 7.4 Pp 42868^x) 8.44 174 3.9 Pp; B78
41958.7 8.362 132 8.1 Pp 43131.5 8.41 186 6.4 B78
41981.6 8.392 133 9.3 Pp 43151.7 8.390 187 4.8 B78
42023.2 8.361 135 7.3 Pp 43177.0 8.342 188 8.4 Pp; B78
42106.4 8.388 139 3.6 Pp 43198.9 8.376 189 8.5 Pp; B78
42129.9 8.391 140 5.3 Pp 43218.1 8.382 190 6.0 Pp; B78
42152.2 8.368 141 5.8 Pp 43241 8.40 191 7.1 Pp
42173 8.33 142 4.9 Pp 43261 8.39 192 5.4 B78
42194.5 8.352 143 4.6 Pp 43303.0 8.351 194 3.9 Pp
42259 8.25 146 3.9 Pp 43325 8.42 195 4.2 B78
42281.1 8.260 147 4.3 Pp 43344.9 8.451 196 2.3 B78
42302.4 8.259 148 3.8 Pp 43415.2 8.410 199 7.3 Pp
42366.3 8.292 151 2.5 Pp 43435.2 8.396 200 5.6 Pp
42433.6 8.299 154 4.5 Pp 43456.7 8.403 201 5.3 Pp
42455.5 8.374 155 4.6 Pp 43640 8.43 209 14.6 Pp
42477 8.39 156 4.4 B78 45222.1 8.350 282: 9.0 Pp
42498.0 8.369 157 3.7 B78
References: The same as in Table 6 and Wi66=Williams 1966; Z68=Zaitseva 1968.
Remarks:
i) large hump before maximum
ii) hump before maximum
iii) hump after maximum
iv) large scatter in maximum
v) nearly constant, irregular light variation between J.D. 2440110 and
2440145 (m_v~8.52)
vi) nearly constant between J.D. 2440310 and 2440380 (m_v~8.48)
vii) hump on the ascending branch
viii) long (9 days) stillstand on the ascending branch
ix) slow, continuous increase in brightness between J.D. 2441540 and 2441595
x) maximum light was constant during five days (mm_v^max~8.44)
The fluctuations in other parameters have also increased after 1965. For
example, the length of the ascending branch, M-m, fluctuated between 9.3
and 10.1 days before 1965, while the fluctuations were between 6.7 and
16.3 days, with a mean M - m = 10.91 days after 1965.
Huth (1967) suspected a connection between the changes of the period and
the light amplitude, while Broglia and Guerrero (1973) and Broglia et al.
(1978) denied the existence of such a correlation. They found, however, a
correlation between the amplitude (sine fitting) and the period (sine
fitting). Our investigations do not support the existence
Figure 6. The observed photoelectric maxima (circles) and minima (dots)
since 1965
of either the correlation between the variation of the period and the changes
of the light curve amplitude or the correlation between the amplitude and period.
As it was pointed out by Broglia and Guerrero (1973) and Broglia et al. (1978)
the mean luminosity of RU Cam did not vary significantly, consequently the
energy production of the star was the same after 1965 as before. This means
that the outer layers of the star are responsible for its irregular behaviour.
The photometric data obtained in the years 1965-1982 were Fourier analysed,
but there were no indications for a modulation effect; instead of some
separate peaks a bunch of peaks appeared in the spectrum around the frequency
f = 0.046 cycle/day suggesting that the star might pulsate rather in chaotic
or stochastic way (see a more detailed discussion in a forthcoming paper of
Kolláth and Szeidl, 1993).
The unique behaviour of RU Cam - as it was pointed out by Wallerstein (1968)
- may be associated with the processes of mass loss and mixing which modify the
pulsational conditions in the outer layers of the star. Nevertheless, the
problem is still unsolved how the more or less regular pulsation of RU Cam
ceased in a very short time interval (within one year) and gave place to an
oscillation in which the erratic component is sometimes dominant (Broglia and
Guerrero, 1972a) or which has become chaotic (Perdang, 1985).
Acknowledgements
The authors are grateful to dr. G. Kovács for obtaining some of the observations
and for valuable discussions. This work has been supported by research grant
OTKA No. 829.
Budapest, Svábhegy, December 31, 1992
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Table 3
Photoelectric V and B observations of RU Cam
(variable - BD +70°448)
J.D. Delta V Delta B Delta(B-V) n Z
39348.576 -.552+-008 -.456+-013 .096 3 51
39350.572 -.581+-004 -.500+-006 .081 3 51
39351.569 -.584+-002 -.517+-002 .067 5 50
39352.584 -.580+-004 -.516+-010 .064 4 48
39354.583 -.612+-005 -.541+-009 .071 6 48
39355.572 -.607+-003 -.525+-005 .082 6 49
39356.573 -.595+-005 -.531+-008 .064 6 48
39358.555 -.570+-002 -.509+-006 .061 4 50
39359.585 -.543+-003 -.441+-006 .102 2 46
39361.577 -.537+-002 -.447+-007 .090 3 46
39367.557 -.531+-005 -.442+-002 .089 4 47
39370.569 -.577+-001 -.505+-005 .072 6 44
39371.564 -.566+-005 -.498+-007 .068 4 45
39372.564 -.588+-004 -.510+-006 .078 3 45
39374.577 -.606+-002 -.548+-004 .058 5 42
39376.567 -.598+-004 -.537+-005 .061 5 43
39380.572 -.572+-006 -.477+-018 .095 4 41
39381.553 -.520+-004 -.441+-012 .079 5 43
39382.515 -.509+-004 -.418+-003 .091 4 47
39383.511 -.501+-003 -.427+-005 .074 5 47
39383.611 -.493+-006 -.418+-002 .075 2 35
39384.615 -.495+-002 -.398+-008 .097 3 34
39388.495 -.513+-002 -.402+-014 .111 3 47
39388.575 -.512+-001 -.401+-002 .111 3 38
39390.564 -.539+-003 -.451+-005 .088 5 39
39391.585 -.567+-006 -.482+-003 .085 3 35
39392.544 -.572+-003 -.486+-004 .086 5 40
39393.528 -.590+-005 -.515+-003 .075 6 42
39396.367 -.616+-004 -.537+-007 .079 5 58
39396.534 -.608+-003 -.568+-007 .040 5 40
39400.591 -.599+-006 -.541+-007 .058 3 32
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43218.279 -.679+-008 -.632+-014 .047 3 22
43220.517 -.664+-008 -.586+-004 .078 4 46
43221.362 -.629+-006 -.565+-015 .064 4 28
43224.386 -.587+-008 -.472+-006 .115 4 32
43226.427 -.558+-004 -.436+-002 .122 4 37
43228.368 -.524+-006 -.394+-005 .130 5 31
43229.485 -.467+-006 -.393+-010 .074 5 46
43234.455 -.575+-003 -.467+-007 .108 3 44
43240.364 -.651+-005 -.606+-012 .045 4 34
43244.547 -.642+-008 -.523+-010 .119 5 56
43251.345 -.541+-008 -.416+-007 .125 4 36
43287.394 -.570+-003 -.450+-002 .120 4 53
43289.355 -.532+-006 -.388+-004 .144 5 50
43298.380 -.571+-007 -.541+-011 .030 4 54
43302.512 -.706+-002 -.610+-009 .096 4 63
43372.473 -.583+-006 -.497+-002 .086 3 58
43375.582 -.518+-006 -.403+-004 .115 3 47
43381.558 -.511+-006 -.367+-009 .144 3 48
43385.596 -.572+-004 -.476+-010 .096 3 42
43390.587 -.601+-005 -.553+-002 .048 3 42
43393.595 -.612+-008 -.552+-005 .060 3 40
43399.484 -.457+-005 -.370+-006 .087 3 51
43414.461 -.646+-005 -.610+-004 .036 3 49
43415.503 -.648+-008 -.595+-004 .053 3 43
43420.574 -.533+-007 -.394+-003 .139 3 33
43422.620 -.470+-005 -.328+-009 .142 3 27
43423.597 -.463+-011 -.320+-003 .143 3 29
43424.560 -.437+-002 -.303+-007 .134 3 34
43425.565 -.472+-010 -.326+-007 .146 3 32
43430.518 -.566+-011 -.517+-011 .049 5 36
43432.550 -.631+-006 -.590+-005 .041 4 32
43434.519 -.664+-004 -.617+-007 .047 4 35
43435.509 -.663+-005 -.611+-003 .052 3 36
43436.478 -.650+-002 -.579+-004 .071 3 40
43437.443 -.642+-010 -.565+-005 .077 4 44
43438.537 -.605+-002 -.526+-007 .079 3 32
43455.598 -.649+-002 -.582+-017 .067 3 23
43458.586 -.637+-003 -.582+-002 .055 3 23
43459.663 -.610+-004 -.552+-003 .058 3 24
43465.673 -.467+-005 -.354+-005 .113 4 26
43477.564 -.638+-005 -.601+-007 .037 3 22
43482.592 -.604+-009 -.502+-008 .102 4 24
43483.687 -.568+-004 -.481+-009 .087 3 33
43490.367 -.444+-004 -.320+-003 .124 3 35
43513.640 -.498+-002 -.360+-005 .138 9 38
43514.466 -.494+-003 -.372+-006 .122 5 22
43558.416 -.480+-003 -.404+-006 .076 4 26
43560.500 -.486+-006 -.372+-006 .114 4 36
43578.278 -.515+-008 -.419+-006 .096 5 22
43579.388 -.508+-009 -.439+-008 .069 5 29
43598.367 -.553+-008 -.422+-009 .131 4 32
43599.369 -.535+-012 -.427+-007 .108 3 33
43606.322 -.474+-005 -.362+-007 .112 3 30
43607.373 -.462+-005 -.427+-016 .035 4 36
43608.326 -.502+-008 -.398+-009 .104 6 31
43639.336 -.558+-006 -.452+-004 .106 3 42
43640.326 -.576+-003 -.412+-005 .164 3 41
43647.389 -.618+-005 -.464+-005 .154 4 51
44605.360 -.592+-004 -.532+-005 .060 4 30
44613.476 -.612+-003 -.510+-001 .102 4 23
44614.317 -.601+-001 -.514+-007 .087 3 32
44619.292 -.606+-007 -.500+-007 .106 4 33
44621.374 -.603+-001 -.504+-005 .099 4 24
44633.493 -.595+-003 -.505+-005 .090 4 28
44637.476 -.603+-002 -.511+-004 .092 4 27
44642.494 -.574+-002 -.469+-002 .105 4 31
44661.428 -.536+-005 -.452+-005 .084 5 29
45218.496 -.632+-005 -.665+-003 -.033 5 51
45221.507 -.696+-006 -.642+-003 .054 5 49
45223.519 -.707+-007 -.624+-009 .083 5 47
45224.511 -.667+-009 -.560+-005 .107 5 48
45225.552 -.630+-007 -.516+-007 .114 5 43
45226.526 -.590+-005 -.459+-007 .131 5 46
45251.545 -.464+-002 -.312+-008 .152 2 35
45259.526 -.529+-001 -.481+-002 .048 5 34
45260.540 -.565+-007 -.522+-007 .043 4 33
* observation made at Piszkéstető mountain station
Table 4
Photoelectric U observations of RU Cam
(variable - BD +70°448)
J. D. DeltaU n J. D. DeltaU n
39536.591 -.292+-009 5 39617.358 -.313+-008 3
39538.572 -.318+-005 3 39618.359 -.370+-006 4
39546.304 -.468+-005 5 39623.371 -.365+-014 4
39547.319 -.470+-004 5 39639.381 -.306+-019 3
39562.484 -.337+-005 4 39664.420 -.326+-011 4
39564.292 -.420+-006 6 40449.513 -.714+-011 4
39570.304 -.577+-006 6 40807.471 -.437+-006 3
39585.346 -.465+-010 3 41634.484 -.545+-003 5
39588.322 -.691+-013 3 41637.604 -.506+-006 5
39590.324 -.650+-002 4 41650.430 -.574+-006 5
39598.346 -.345+-012 4 41679.275* -.530+-016 4
39600.326 -.287+-011 3 41680.248* -.469+-010 4
39604.361 -.336+-003 3 41682.277* -.413 1
39610.392 -.624+-009 4 42452.283* -.644+-009 4
39611.361 -.649+-011 4 42453.262* -.654+-016 4
* observation made at Piszkéstető mountain station