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Far-Ultraviolet Observations of the Galactic NRC Publications Archive Archives des publications du CNRC Far-Ultraviolet Observations of the Galactic Supersoft Binary RX J0019.8+2156 (QR Andromedae) Hutchings, J.B.; Crampton, D.; Cowley, A.P.; Schmidtke, P.C.; Fullerton, A.W. This publication could be one of several versions: author’s original, accepted manuscript or the publisher’s version. / La version de cette publication peut être l’une des suivantes : la version prépublication de l’auteur, la version acceptée du manuscrit ou la version de l’éditeur. For the publisher’s version, please access the DOI link below./ Pour consulter la version de l’éditeur, utilisez le lien DOI ci-dessous. Publisher’s version / Version de l'éditeur: https://doi.org/10.1086/322114 The Astronomical Journal, 122, 3, pp. 1572-1577, 2001 NRC Publications Record / Notice d'Archives des publications de CNRC: https://nrc-publications.canada.ca/eng/view/object/?id=06dd086f-351d-4c62-94e5-fd8e1e4187a3 https://publications-cnrc.canada.ca/fra/voir/objet/?id=06dd086f-351d-4c62-94e5-fd8e1e4187a3 Access and use of this website and the material on it are subject to the Terms and Conditions set forth at https://nrc-publications.canada.ca/eng/copyright READ THESE TERMS AND CONDITIONS CAREFULLY BEFORE USING THIS WEBSITE. L’accès à ce site Web et l’utilisation de son contenu sont assujettis aux conditions présentées dans le site https://publications-cnrc.canada.ca/fra/droits LISEZ CES CONDITIONS ATTENTIVEMENT AVANT D’UTILISER CE SITE WEB. Questions? Contact the NRC Publications Archive team at [email protected]. If you wish to email the authors directly, please see the first page of the publication for their contact information. Vous avez des questions? Nous pouvons vous aider. Pour communiquer directement avec un auteur, consultez la première page de la revue dans laquelle son article a été publié afin de trouver ses coordonnées. Si vous n’arrivez pas à les repérer, communiquez avec nous à [email protected]. THE ASTRONOMICAL JOURNAL, 122:1572È1577, 2001 September ( 2001. The American Astronomical Society. All rights reserved. Printed in U.S.A. FAR-ULTRAVIOLET OBSERVATIONS OF THE GALACTIC SUPERSOFT BINARY RX J0019.8]2156 (QR ANDROMEDAE)1 J. B. HUTCHINGS,2 D. CRAMPTON,2 A. P. COWLEY,3 P. C. SCHMIDTKE,3 AND A. W. FULLERTON4,5 Received 2001 April 23; accepted 2001 May 30 ABSTRACT Far-Ultraviolet Spectroscopic Explorer spectra were obtained of the supersoft X-ray binary RX J0019.8]2156 (QR And) during 16 consecutive spacecraft orbits, covering the binary orbit (P \ 15.85 hr) with about 0.2 phase overlap. The spectrum is dominated by strongH absorption (column density 2 D1020 gcm~2), which appears at the velocity di†erent from other interstellar absorption lines and may be partially circumbinary. This absorption makes study of spectral features from the binary system diffi- cult. The only well-detected emission lines are He II j1085 and O VI j1032 (the other line of the O VI doublet, at 1037A ,H is largely obscured by strong absorption). The O VI shows a P Cygni proÐle that 2 varies in velocity and strength with binary phase. We compare this with similar changes seen in Balmer line proÐles. We extract the far-ultraviolet (FUV) light curve and compare it with the optical light curve. There is an eclipse in both wavelength regions, but the FUV minimum lasts much longer, well beyond the visible light egress. The FUV results are discussed in connection with the binary model and mass Ñows within the system. Key words: binaries: close È ISM: jets and outÑows È stars: individual (RX J0019.8]2156\QR And) È ultraviolet emission È X-rays 1. INTRODUCTION Like several other supersoft X-ray binaries, QR And also shows bipolar emission-line jets (velocity about ^800 km RX J0019.8]2156 (hereafter called by its variable star s~1)inHeII (j4686) and the lower Balmer lines (e.g., Becker designation, QR And) is one of the few identiÐed Galactic et al. 1998; Cowley et al. 1998; Deufel et al. 1999). These jet supersoft X-ray binaries, although numerous examples have features come and go on timescales of weeks to months. been found in the Magellanic Clouds and M31 (see Greiner Since the Balmer outÑow is phase dependent (and persist- 1996). The system was Ðrst noted in the ROSAT All-Sky ent?), this is likely a constant disk Ñow that is not strongly Survey and described by Beuermann et al. (1995). They related to the jet activity. found this 12th magnitude system shows D0.5 mag eclipses There has been some disagreement about the appropriate and radial velocity variations that Ðt an orbital period of model for QR And, with various authors deriving quite 15.85 hr. Archival photographic plates show the orbital di†erent values for the orbital inclination and hence the period has been stable for over 40 years (Greiner & Wenzel stellar masses. Beuermann et al. (1995) concluded that the 1995), although there are irregular changes of a few tenths inclination must be quite low (i D 20¡), based partially on of a magnitude in the overall brightness level of the system the assumptions that the masses are similar and consistent (e.g., Cowley et al. 1998; Deufel et al. 1999). with a white dwarf. On the other hand, Meyer-Hofmeister The system is at Galactic latitude [40¡ and hence shows et al. (1998) analyzed the light curve and presented models little evidence of interstellar reddening, with mean that indicate an inclination near i \ 55¡, while Tomov et al. U[B D [0.7 (Beuermann et al. 1995) and quite weak (1998) suggested an even larger value (i D 79¡), also based II I interstellar lines of Ca and Na (McGrath et al. 2001). on the light curve. The adopted inclination is important This, with the mean absolute magnitude of supersoft binary since it ultimately conÐnes the range of possible masses and systems, places its distance at D2 kpc, so it lies well out of hence the model and evolution of the system. From an the Galactic plane. analysis of the emission-line velocities and those of the II Optical spectra show very strong emission lines of He bipolar jets, Becker et al. (1998) found that the jet lines show II (virtually all the He lines in the Multiplet Table are the same velocity amplitude and phasing as He II 4686 A identiÐed). Balmer absorption lines are present through and hence concluded that the He II lines must reveal the about half the orbital cycle and indicate a strong outÑow of motion of the compact star where the jets originate. material with velocities of about [200 to [600 km s~1. Further, from analysis of the outÑow line proÐles they found that the orbital inclination must lie in the range ÈÈÈÈÈÈÈÈÈÈÈÈÈÈÈ 35¡ \ i \ 60¡. For the purpose of our discussion below, we 1 Based on observations made with the NASA-CNES-CSA Far Ultra- have adopted these conclusions of Becker et al. and assume violet Spectroscopic Explorer. FUSE is operated for NASA by Johns a model similar to that discussed by Meyer-Hofmeister Hopkins University under NASA contract NAS 5-3298 et al. 2 Herzberg Institute of Astrophysics, National Research Council of O VI emission (jj3811, 3835, and 5290) is found in all Canada, Victoria, BC V9E 2E7, Canada; john.hutchings=nrc.ca, david.crampton=nrc.ca. supersoft X-ray binaries and is potentially interesting as its 3 Department of Physics and Astronomy, Arizona State University, high ionization may indicate an origin close to the accretion Box 871504, Tempe, AZ 85287-1504; anne.cowley=asu.edu, disk center. However, study of these lines is compromised paul.schmidtke=asu.edu. by blends with He II at 3813 and 3834A and with [Fe XIV] 4 Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, Victoria, BC V8W 3P6, Canada. at 5303A. This suggested that it would be particularly inter- 5 Department of Physics and Astronomy, Johns Hopkins University, esting to observe the supersoft systems in the far-ultraviolet 3400 North Charles Street, Baltimore, MD 21286; awf=pha.jhu.edu. with the Far-Ultraviolet Spectroscopic Explorer (FUSE) 1572 SUPERSOFT BINARY RX J0019.8]2156 1573 TABLE 1 FUSE OBSERVATIONS OF RX J0019.8]2156 Photometric HJD (mid) Exposure Orbit Phasea 2,451,700] (s) 1 ............. 0.475 52.922 2481 2 ............. 0.584 52.993 2191 3 ............. 0.694 53.066 1871 4 ............. 0.799 53.135 1590 5 ............. 0.907 53.206 1310 6 ............. 0.966 53.246 418 7 ............. 0.013 53.277 1160 8 ............. 0.075 53.318 850 9 ............. 0.120 53.347 920 10............ 0.184 53.389 1220 11............ 0.227 53.418 701 12............ 0.293 53.461 1721 13............ 0.327 53.478 1320 IG Top two plots FUSE 14............ 0.414 53.541 3461 F . 1.È : Average spectrum of QR And with dif- ferent amounts of smoothing and airglow removal; bottom two plots, for 15............ 0.519 53.610 3461 comparison, theH model absorption with two di†erent smoothings. 16............ 0.622 53.679 3301 2 a Ephemeris:T \ HJD 2,449,987.8459(16) ] 0.6604645(14) 0 H model from our grid that Ðts it most closely. The H E days (McGrath et al. 2001). 2 2 absorption strength in the FUSE wavelength range is since the O VI resonance lines (1032 and 1037A ) lie within loosely correlated with E(B[V ) and was compared with its wavelength range. several B0 stars with E(B[V ) ranging from 0.15 to 0.5 mag, OBSERVATIONS which had been observed with FUSE.
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