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Yerkes Observatory Received August 20, I960 8IB .3 .5. THE SPECTRUM OF RHO CASSIOPEIAE. I* Wallace R. Beardsley! Yerkes Observatory 196lApJS. Received August 20, I960; revised September 16, 1960 ABSTRACT This paper constitutes an analysis of an extensive series of spectrograms of p Cassiopeiae taken by several observers principally with the 82-inch telescope of the McDonald Observatory both during and after the deep minimum in light of 1946. Identification measures by Tai and Thackeray before the minimum have been combined with detailed measures by the writer during and after the minimum, to form a catalogue of the spectral lines as seen on plates of medium dispersion. A group of 23 selected zero-volt lines were analyzed for radial-velocity and intensity changes. Although no change in radial velocity was detected, marked changes in intensity did occur. The hydrogen lines in p Cas in 1936 were found to be as strong as, or even stronger than, in ô CMa. Weakness of the hydrogen lines as early as 1939 may be evidence of spectral change leading up to the 1946 minimum. Evidence is cited for an over- lying shell in which the TiO is formed. Unlike RV Tauri stars, the spectral type from line ratios at minimum light was also M3. The spectral type after minimum varied progressively from K5p to G5p, even reaching F8p during the “flare-up” of 1950. The behavior of emission in the hydrogen and Ca I X 4227 lines is discussed, as well as the presence of a sharp absorption core in Ca I. This core also was probably due to an overlying shell. I. INTRODUCTION h m 0 / TTfou irregular variable p Cas (HD 224014, qiqoo ^ 23 49 4, Ô1900 = +56 57 , mv ^ 4.1-6.2, Sp. F8 lap) is of particular interest as a result of an unprecedented light- minimum that occurred in 1946, accompanied by marked and extraordinary spectral changes. This paper presents a study of the spectrum before, during, and after this deep minimum. The star was discovered to be variable in light by Miss Louise Wells (Pickering 1901) ; the irregular variable classification was assigned by Cannon and Pickering (1907) on the basis of 59 observations in 1903-1905. Previously the star had been recognized as being reddish in color, first appearing so to Schmidt (1872) as color 6?5 (yellow). A discussion of the characteristics of the spectrum on low dispersion has been published by Payne-Gaposchkin and Mayall (1946), who classified 31 Harvard objective-prism plates taken between 1885 and 1946. Their results indicate that the spectrum varied from F8 to K5. Prior to the unprecedented light-minimum of 1946 the spectrum was F8, and, at the time, p Cas was selected as being representative of the spectral class of F8 la supergiants (Morgan, Keenan, and Kellman 1943). The general spectral characteristics of an F8 la supergiant comprise very strong lines of ionized metals— i.e., Fen, Tin, Sen, Y n, and Cm—as well as strong hydrogen lines and fairly strong neutral iron lines. The profiles of these lines also imply considerable turbulence. Color observations of p Cas by a number of observers have also indicated color varia- bility (Guthnick 1914; Guthnick and Hügeler 1920; and Guthnick and Pavel 1920). A photoelectric six-color observation (on August 23, 1941 [JD 2430230]) by Stebbins and Whitford (1945) when the spectrum was F8-G0 implies considerable interstellar red- dening. Conversion of this observation to the B — V system gives B — V = +1.37. Additional photoelectric observations of p Cas should be made to investigate changes in color of the star. The visual light-curve from 1904 to 1934 has been published by Hassenstein (1934), * Contributions from the McDonald Observatory, University of Texas, No. 337. t Now at the Allegheny Observatory, University of Pittsburgh. 381 © American Astronomical Society • Provided by the NASA Astrophysics Data System 8IB .3 .5. 382 WALLACE R. BEARDSLEY while the photographic light-curve from 1904 to 1946 has been published by Payne- Gaposchkin and Mayall (1946). The light-curve was characterized by alternate in- 196lApJS. creases and decreases in intensity with no apparent plateaus. Immediately apparent in both light-curves is the irregularity of period of variation and of amplitude. Also apparent in both light-curves is the existence of three separate modes (see Fig. 2 in Hassenstein 1934), the first lasting until about September, 1911 (JT> 2419300), the second then con- tinuing to about September, 1922 (JD 2423300), the third then continuing to the deep light-minimum of 1946. A íísemiregularity,,, however, appears to exist for each of the three modes, the mean period for the first mode being about 450 days, for the second mode about 200 days, and for the third mode about 300 days. It will be shown later (see Sec. Ill) that the spectral type F8 la was apparently associated with the third mode. Figure 1 presents the light-curve of p Cas for the period October, 1943, to September, 1954. Both visual and photographic observations are represented, as well as the dates of the spectroscopic observations discussed in this paper. The visual curve comprises dots, which represent A.A.V.S.O. 10-day means [before JD 2433600 the A.A.V.S.O. observations are those of Oravec and Ashbrook (Campbell 1946,1948; Mayall 1950 ff.)], and + signs, which represent visual observations by Parenago (1947). The photo- graphic curve is comprised of circles which represent photoelectric observations of Kos- tylev (1947), and X signs which represent photographic observations by S. Gaposchkin (Payne-Gaposchkin and Mayall 1946; Gaposchkin 1947) reduced to Kostylev’s scale. The visual curve covers the entire period 1943-1954, the photographic curve covers only JULIAN DATE > Fig. 1.—A plot of visual and photographic magnitudes of p Cas for the interval October, 1943, to September, 1954; . = A.A.V.S.O. 10-day visual means (before JD 2433600 the A.A.V.S.O. observa- tions are those of Oravec and Ashbrook); + = visual observations by Parenago; o = photoelectric observations by Kostylev; X = photographic observations by S. Gaposchkin reduced to the Kostylev scale. The dates and dispersions of the spectrograms discussed by the writer are indicated: X, Yerkes classification spectrograph dispersion 125 A/mm at Hy; F/2 and CG McDonald Cassegrain spectro- graph dispersions 76 and 26 A/mm at H7, respectively. The date 11-2/19-47 refers to a series of 12 spectrograms by Greenstein taken within that interval. © American Astronomical Society • Provided by the NASA Astrophysics Data System 8IB .3 .5. RHO CASSIOPEIAE 383 the portion 1943-1947. If we say the normal magnitudes of p Cas are mv = 4.8 and wPg = 5.4, it is apparent that p Cas became appreciably redder during the 1946 light- 196lApJS. minimum. From wPg — mv = +0.6 on about July 15,1945 (JD 2431652), the color index increased rapidly to +1.3 on about December 15, 1945 (JD 2431805), which was near the middle of the decline in brightness, and then decreased slowly and more or less uni- formly to approximately +0.7 on about May 1, 1947 (JD 2432307), near the middle of the incline in brightness. An increase in color index to about +1.0 occurred for observations thereafter through November, 1947 (JD 2432500). A “phase lag” is ap- parent in the relative shapes of the minimum, the visual light-curve being decidedly asymmetrical, while the photographic light-curve appears nearly symmetrical. It is interesting that the previously mentioned £ — F of +1.37 by Stebbins and Whitford was also obtained during the decline to a minimum, although it was a much shallower minimum [see the light-curve by S. Gaposchkin (Payne-Gaposchkin and Mayall 1946)]. II. THE SPECTRUM OE p CAS, 1939-1950 Commencing with the discovery of the unprecedented light-minimum by Popper (1946), an extensive series of observations was undertaken by W. P. Bidelman, D. M. Popper, J. L. Greenstein, and others, principally with the 500-mm camera of the Casse- grain spectrograph of the 82-inch telescope of the McDonald Observatory. The dispersion was 18 A/mm at 4000 A, 26 A/mm at H7, 41 A/mm at H0, and 79 A/mm at the D lines. Because of the surprising spectral changes (F8 la to Ma) that took place, a de- tailed analysis of the spectrum should be of value. Accordingly, three plates in the series—one taken during minimum (CG 5171, November 22, 1946) by W. P. Bidelman, one taken just after minimum (CG 6222-3, November 5, 1947) by J. L. Greenstein, and one taken well after minimum (CG 8626, November 5, 1950) by G. Münch—have been carefully measured. In addition to these measures, there are available measures of the spectrum of p Cas in 1939 made by Tai and Thackeray (1948), with approximately the same dispersion, and deposited in the archives of the Royal Astronomical Society. The writer is very grateful to Dr. A. D. Thackeray for permission to utilize these measures and to Dr. R. H. Garstang for transcribing them. The catalogue of spectral changes is presented in Table 1. The arrangement consists of four sets of columns, one set each for the plates taken in 1939, 1946, 1947, and 1950. Each set comprises three columns in the following order: (1) wave length, X, corrected for a preliminary radial velocity based on several strong Fe 1 lines in the spectrum with accompanying comparison lines; (2) visually estimated intensity; and (3) identification, based on the Revised Multiplet Table oí Moore (1945). The preliminary velocities (km/sec) were —42.6 (1939), —45.7 (1946), —40.9 (1947), and —53.0 (1950). One should approach with caution the question of the significance of these velocity differences.
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