/ftp/cats/J_other/PASP/121/104



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J/PASP/121/104      BVRI differential photometry of GW Gem  (Lee+, 2009)
The following files can be converted to FITS (extension .fit or fit.gz)
	table1.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/PASP/121/104
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drwxr-xr-x 14 cats archive 253 Jan 29 2012 [Up] drwxr-xr-x 2 cats archive 213 Jan 13 2023 [TAR file] -rw-r--r-- 1 cats archive 461 Dec 19 2022 .message -r--r--r-- 1 cats archive 4063 Jun 3 2009 ReadMe -r--r--r-- 1 cats archive 44599 Apr 26 2009 table1.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/PASP/121/104 BVRI differential photometry of GW Gem (Lee+, 2009) ================================================================================ Photometric properties of the near-contact binary GW Geminorum. Lee J.W., Kim S.-L., Lee C.-U., Kim H.-I., Park J.-H., Park S.-R., Koch R.H. <Publ. Astron. Soc. Pac., 121, 104-110 (2009)> =2009PASP..121..104L ================================================================================ ADC_Keywords: Stars, double and multiple ; Photometry, CCD ; Photometry, UBVRI Abstract: New multiband CCD photometry is presented for the eclipsing binary GW Gem; the RI light curves are the first ever compiled. Four new minimum timings have been determined. Our analysis of eclipse timings observed during the past 79 years indicates a continuous period increase at a fractional rate of +(1.2+/-0.1)x10^10^, in excellent agreement with the value +1.1x10^-10^ calculated from the Wilson-Devinney binary code. The new light curves display an inverse O'Connell effect increasing toward longer wavelengths. Hot- and cool-spot models are developed to describe these variations but we prefer a cool spot on the secondary star. Our light-curve synthesis reveals that GW Gem is in a semidetached, but near-contact, configuration. It appears to consist of a near-main-sequence primary star with a spectral type of about A7 and an evolved early K-type secondary star that completely fills its inner Roche lobe. Mass transfer from the secondary to the primary component is responsible for the observed secular period change. Description: Our CCD photometry of GW Gem was performed on 13 nights during the period 2007 December 20-2008 March 1 in order to obtain multicolor light curves. The observations were taken with a SITe 2K CCD camera and a BVRI filter set attached to the 61-cm reflector at Sobaeksan Optical Astronomy Observatory (SOAO) in Korea. Objects: -------------------------------------------------------------------- RA (2000) DE Designation(s) -------------------------------------------------------------------- 07 52 29.0 +27 09 16 GW Gem = V* GW Gem 07 53 05.5 +27 16 55 2MASS J07530545+2716551 = UCAC2 41361532 --------------------------------------------------------------------