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Publications of the Astronomical Society of the Pacific 101: 999-1003, November 1989

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Publications of the Astronomical Society of the Pacific 101: 999-1003, November 1989 Publications of the Astronomical Society of the Pacific 101: 999-1003, November 1989 RECENT PHOTOMETRIC BEHAVIOR OF THE UNUSUAL Be STAR HD 45677 = FS CANIS MAJORIS ELAINE M.HALBEDEL* Corralitos Observatory, P.O. Box 16314, Las Cruces, New Mexico 88004 Received 1989 June 15, revised 1989 August 16 ABSTRACT Four years of recent photometry for the unusual Be star HD 45677 = FS CMa is presented. The star is shown to vary actively during the time period observed. A quasi-periodicity of296.5 days has been found for the recent data but does not entirely satisfy historical magnitudes. The feasibility of several models (binarity with a semiregular late-type variable or an infrared object versus motions in the circumstellar shell of a single star) is discussed. A spectrum centered on Ha is presented. Key words: Be star-photometry-circumstellar matter 1. Introduction cool companion is still in the process of formation. Low The star HD 45677 = FS Canis Majoris is an unusual et al. (1970) also suggest a cool companion and that FS member of the class of Be stars. It has been suggested to CMa may be a protostar approaching the main sequence be an object intermediate between a Be star and a plane- and its companion an infrared object like Becklin's object. tary nebula or a symbiotic object. Its spectrum is quite However, another suggestion postulates that the infrared excess is a feature derived from thermal emission from the peculiar, having shown strong Ρ Cygni-type emission at circumstellar dust grains which have a temperature of the Balmer lines of hydrogen and also emission lines of 600 K-1800 Κ (Allen 1971), since there has been no evi- [Fe II], [Ni π], [Cr π], [S ll], and [Ο i]. That it possesses dence of periodicity whatsoever in the radial-velocity an extended thick shell of gas and dust of considerable variations over the past 50 years (Dyck and Milkey 1972). density is inferred from the appearance of the nebular They model the infrared excess by H_ free-free emission lines of [O l] at 6300 and 6363 and of [S ll] at 4068 λλ λ in the metal ionization region. Neither SiO maser radia- (Merrill and Burwell 1933). tion (Dickinson et al. 1978) nor OH emission (Lepine and First noted to have emission at Ha in 1898 (Merrill Rieu 1974) have been detected. In the ultraviolet the 1952), there has never been a time that FS CMa has been spectrum shows an interstellar band at 0.22 μιη and other without hydrogen emission. These line profiles have been lines which suggest high-temperature condensates (Mer- observed to be variable in nature sometimes on the order rill 1979). The infrared spectrum is rich in unidentified of hours (e.g.. Swings (1973) records the disappearance of lines and resembles that of η Carinae and LHa 101 an absorption component of Ηδ in 2 hours). The spectrum (Thackeray and Velasco 1976). Polarization of light has is rich in emission lines both permitted and forbidden. been observed suggesting that the dust grains in the Spectrum variations have been observed in the lines of circumstellar shell are solid dielectric grains with r ~ 0.2 Mg π, He I, and Ca π (Swings et al. 1980). μ (Zellner and Serkowski 1972). The star is not a member FS CMa possesses a strong infrared excess. Indeed, the of a large OB association. infrared produces most of the observed energy flux. Sev- Spectral classification of the underlying star of FS CMa eral models have attempted to account for this by invok- is difficult because of the prevalence of emission lines in ing a cool companion. Ciatti, D'Odorico, and Mammano the spectrum. Previous types have been BQ [ ] (Ciatti (1974) suggest that this companion may be a very late- et al. 1974), BOp (Rufener 1981), B1 (Kilkenny 1978), B2e type giant or supergiant (perhaps representative of the (Merrill 1928), B2q (Allen 1973), B2 IVep sh (Buscombe phase of evolution following long-period variability) or a 1977), B2 IVe (Feinstein et al 1976), B2 IVpe (Kilkenny carbon star. Since there is no radio emission observed and 1981), B3pe (Mendoza 1958), and B3 V (Low et al. 1970). there is an absence of some nebular lines (both of which The estimated υ sin i of 200 km s-1 should be considered would denote a small Η π region), it is possible that the provisional. * Visiting Astronomer, Kitt Peak National Observatory, National Op- 2. The Photometric History of FS CMa tical Astronomy Observatories, operated by the Association of Universi- ties for Research in Astronomy, Inc., under contract with the National Spectroscopy suggests that the extended region sur- Science Foundation. rounding FS CMa is capable of changes on both long and 999 © Astronomical Society of the Pacific · Provided by the NASA Astrophysics Data System 1000 ELAINE M. HALBEDEL short time scales. Therefore, it is no surprise that the star B9) and HD 45629 (V - 7.091; {Β-V) = -0.032; B8). is also a photometric variable. Swings and Swings (1972) These magnitudes were derived from all-sky photometry have examined the light curve of this object from the at the Kitt Peak telescope. Only HD 45629 had previ- Harvard plate collection from 1899 to 1963. They found ously published magnitudes: V = 7.10 and (Β—V) = that the amplitude of photometric variation during this —0.04 (Nicolet 1978), in good agreement with the values time has always been less than 0.3 magnitude, with no observed. There was excellent consistency in colors be- trend toward periodicity. Feinstein et al. (1976) have tween the Corralitos and Kitt Peak systems, with there produced the most intensive study of the photometry of being a magnitude difference of0.003 in AV and Δ (ß — V) this star. They found that in 1972 JJBV photometry between the two. This was not considered large enough to showed day-to-day variations of about 0.02 magnitude as correct. The average standard errors in AV and Δ (ß — V) well as large variations of > 0.10 over longer time inter- for the standard stars were found to be 0.025 and 0.024, vals. The star may vary in V as much as 0.5 magnitude respectively. over a year's time, as much as 0.1 in a week or less, and < A total of 47 V and {Β —V) magnitudes were obtained 0.02 in the course of a single night. A variation in V or y is for FS CMa over a time period of JD2446391-7595 (1985 usually accompanied by a change in (B — V), (b—y), or q November 22 to 1989 March 10), or four observing sea- of opposite sign. No periodicities were observed for these sons. Table 1 details the observations while Figure 1 changes. It is suggested that the small brightness in- shows them graphically. It can be seen immediately that creases between 1899 and 1969 proceed from individual FS CMa has been photometrically active during the past mass-loss events, but that the slow and steady decline of four years. The optical brightness has slowly increased in 0.9 V magnitude between 1958-71 may be due to a cloud V magnitude, followed by a decline, with considerable of material passing through the dust cloud region and the scatter. Curiously, counter to the previous behavior line of sight. Walker (1977) used high-speed photometry chronicled by Feinstein et al. (1976), the mean {Β—V) to show that there was no flickering present. does not seem to have changed, though once again there Swings et al. (1980) have examined the correlation of is considerable scatter. A maximum range of 0.431 in V spectrum and photometric changes. They find that the and 0.098 in (β — V) was observed, both within the histor- photometric data and some spectrum features are well ical ranges previously observed. correlated (or anticorrelated) at certain epochs, but that Though previous searches for periodicities in the pho- this trend does not continue. In 1977 they found that tometry of F S CMa have given negative results, it was there was an anticorrelation between H7 and Ηδ absorp- thought useful to perform a periodicity search using the tion cores and U, B,V, and (U~B). At this time He I and discrete Fourier transform method of Deeming (1975) on Mg π also became more intense. When (U—B), {Β —V), the body of data reported herein. The results were some- and V decreased (suggesting that the effect of the dust what unexpected. A range of periods from 0.85 to 601 patches in the shell decreased), the red emission of the days was searched, and two possible periods were indi- Balmer lines increased. However, in 1979 there were few cated: 296.5 and 166.3 days. The first of these was the positive or negative correlations with the spectra, except better of the two in terms of strength of the power spec- that the strengths of the Ca π and M g π absorption lines trum. A third, almost exactly a day, was considered to be were correlated among themselves and with u, υ, {μ—υ), an artifact of the spacing of the observations at a single and C\. observing site. Figure 2 shows this quasi-periodicity plot- There would seem to be some evidence that the in- ted by phase. Of course, it is distinctly possible that other frared colors in the 1.6-3.5 μ region may be variable periods (particularly of short duration) may exist for this (Feinstein et al. 1976).
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