Other
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...20510213s&link_type=abstract
American Astronomical Society Meeting 205, #102.13; Bulletin of the American Astronomical Society, Vol. 36, p.1513
Other
1
Scientific paper
Using MACHO and OGLE-II data, we are investigating the long-term optical light curves of Be-star companions to X-ray pulsars in the Magellanic Clouds. Here we present new results for two SMC X-ray pulsars: RXJ0049.1-7250 (P(pulse)=74.7 s) and XMMUJ005517.7-723853 (P(pulse)=701.6 s). RXJ0049.1-7250, identified with Star 1 of Stevens et al. (MNRAS, 309, 421, 1999), has a mean V 16.9. We find a strong periodicity at P=33.3 days, which is likely the orbital period, in good agreement with the relation between orbital and pulse periods first recognized by Corbet (A&A, 141, 91, 1984). The folded OGLE-II light curve shows an I amplitude of 0.03 mag. In addition, we find quasi-periodic variations (QPV) of the type discussed by Schmidtke et al. (AJ, 127, 3388, 2004) with periods in the range of 2.39 - 2.40 days, changing slightly in different orbits. The MACHO light curve of XMMUJ005517.7-723853 (=RXJ0055.2-7238) clearly shows short-term variability around mean V 15.9. Analysis of the photometric data reveals a pronounced period at P=0.28 days, much shorter than expected for either an orbital or rotational period of the Be star. The folded light curve shows approximately sinusoidal variations with amplitudes V 0.03 and R 0.02 mag. We suggest that this short period may be due to non-radial pulsations of the type seen in some single Be stars (e.g. Balona & James, MNRAS, 332, 714, 2002). The data, with the 0.28-day variation removed, show a possible long-term period of 413 days, but further analysis is needed to confirm it. The folded light curve using this long period shows 0.01 mag outbursts in R, very similar to the behavior found in other Be/X-ray systems.
Cowley Anne Pyne
Schmidtke Paul C.
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