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A New SU UMa-Type Dwarf Nova, QW Serpentis (= TmzV46)
We report on the results of the QW Ser campaign, which has beencontinued from 2000 to 2003 by the VSNET collaboration team. Four longoutbursts and many short ones were caught during this period. Ourintensive photometric observations revealed superhumps with a period of0.07700(± 0.00004) d during all four superoutbursts, proving theSU UMa nature of this star. The recurrence cycles of the normaloutbursts and the superoutbursts were measured to be 50 days and240(± 30) days, respectively. The change rate of the superhumpperiod was -5.8 × 10-5. The distance and the X-rayluminosity in the range of 0.5-2.4keV are estimated to be 380(±60)pc and log LX = 31.0 ± 0.1 erg s-1.These properties have typical values for an SU UMa-type dwarf nova withthis superhump period.
| Speckle Interferometry at the US Naval Observatory. V.
The results of 1544 speckle interferometric observations of 637 binarystars, ranging in separation from 0.25" to 5.25", are tabulated. Theseobservations were obtained using the 66 cm refractor at the US NavalObservatory in Washington, DC, with an intensified CCD detector. This isthe fifth in a series of papers presenting measures obtained with thissystem and covers the period 1998 January 1 through December 31. Randomerrors for all measures are estimated to be 17.6 mas in separation and0.55d/ρ in position angle, where ρ is the separation inarcseconds.
| Speckle Interferometry at the US Naval Observatory. III.
Position angles and separations resulting from 2578 speckleinterferometric observations of 590 binary stars are tabulated. This isthe third in a series of papers presenting measures obtained using the66 cm refractor at the US Naval Observatory in Washington, DC, andcovers the period from 1995 June through 1996 December. Program starsrange in separation from 0.2" to 4.3", with a limiting magnitude ofV=11. Random errors are estimated to be 17.0 mas in separation and0.56d/rho in position angle, where rho is the separation in arcseconds.These are the first results acquired using an improved intensified CCDdetector. The new detector, in concert with an intensity-filteringtechnique applied in software, has permitted a 1 mag increase in dynamicrange, to 3.5 mag, for pairs separated by about 2". The instrumentationand calibration are briefly described, with an emphasis on thecharacteristics of the new detector. The software filter used toincrease the dynamic range is also described.
| Binary star measurements made at Nice with the 50-cm reflector
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1989A&AS...77..125L&db_key=AST
| Micrometer measures of doubles stars. III.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1963AJ.....68...57V&db_key=AST
| Mesures d'étoiles doubles effectuées au réfracteur de 38 cm. de l'Observatoire de Nice
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