/ftp/cats/A+A/311/484



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J/A+A/311/484       CH Cyg 1991-1995 UBV-JHKLM photometry (Munari+, 1996)
The following files can be converted to FITS (extension .fit .fit.Z .fgz)
	table1 table2
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Query from: http://vizier.cds.unistra.fr/cgi-bin/VizieR?-source=J/A+A/311/484
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drwxr-xr-x 9 cats archive 171 Jan 29 2012 [Up] drwxr-xr-x 2 cats archive 274 Jan 12 2023 [TAR file] -rw-r--r-- 1 cats archive 466 Dec 19 2022 .message -r--r--r-- 1 cats archive 4868 Jul 26 1996 ReadMe -rw-r--r-- 1 cats archive 213 Sep 19 2007 +footg5.gif -rw-r--r-- 1 cats archive 2047 Mar 5 2008 +footg8.gif -r--r--r-- 1 cats archive 1492 Apr 2 1996 table1 -r--r--r-- 1 cats archive 2684 Feb 5 1996 table1.tex -r--r--r-- 1 cats archive 1283 Apr 2 1996 table2 -r--r--r-- 1 cats archive 2094 Feb 5 1996 table2.tex
Beginning of ReadMe : J/A+A/311/484 CH Cyg 1991-1995 UBV-JHKLM photometry (Munari+, 1996) ================================================================================ UBV-JHKLM photometry of CH Cygni over 1978-1995: dust properties and doubts on the triple star model. Munari U., Yudin B.F., Kolotilov E.A., Tomov T.V. <Astron. Astrophys. 311, 484 (1996)> =1996A&A...311..484M (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Photometry, UBVRIJKLMNH Keywords: binaries: symbiotic - individual stars: CH Cyg - infrared stars Abstract: We present new UBV-JHKLM photoelectric photometry of the symbiotic binary CH Cyg covering the period 1991-1995, which extend our monitoring started in 1978. The large and highly homogeneous set of data that we have accumulated in the last eighteen years is reviewed and discussed. By July 1995 the outbursting component has returned to the same conditions which characterized the previous minimum in 1988-1989. In J, H, K CH Cyg shows a long term modulation that can be fitted with a sinusoid of 32 year period. It may be a dust obscuration event similar to those known to undergo in symbiotic Miras. The cool giant exhibits in the infrared a variability of large amplitude, best described as chaotic-like. The only detectable periodicity is 1980 days. The photometric properties of the cool giant denounce a clear partnership with the spheroidal component of the Galaxy. This lowers the estimated distance to  120pc and the cool giant mass to  1.0M_sun_. Several episodes of dust condensation in the wind of the giant are identified. One is in full progress at the time of writing. The dust condensation temperature is found to be  1,000K. The condensed dust grains absorb selectively in the infrared but are large enough to absorb neutrally in the UBV wavelength region. There is no evidence for dust condensing in an hypothetical wind or ejected material from the outbursting white dwarf. The recently proposed triple-star model for CH Cyg is confronted with photometric observations. Several serious discrepancies are outlined and individually discussed. We believe that, without additional evidences and careful modelling, the triple star model cannot survive the comparison with the photometric observations. The low amplitude (2.6km/s) and periodic (756 days) radial velocity variations apparently do not trace an orbital motion. They may be due to one of the many superimposed pulsation modes of the highly variable M giant. Objects: --------------------------------------------------------- RA (2000) DE Name --------------------------------------------------------- 19 24 33.0 +50 14 30 CH Cyg = HD 182917 = BD+49 2999 ---------------------------------------------------------