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J/A+A/311/484       CH Cyg 1991-1995 UBV-JHKLM photometry (Munari+, 1996)
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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)
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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:
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         RA  (2000)  DE      Name
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     19 24 33.0  +50 14 30   CH Cyg = HD 182917 = BD+49 2999
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File Summary:
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  FileName      Lrecl  Records   Explanations
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ReadMe             80        .   This file
table1             25       58   1991-1995 CH Cyg UBV photoelectric photometry
table1.tex         73       64   LaTeX version of table1
table2             36       35   1991-1995 CH Cyg JHKLM photoelectric photometry
table2.tex         75       51   LaTeX version of table2
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Byte-by-byte Description of file: table1
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   Bytes Format Units   Label     Explanations
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   1-  7  I7    d       JD        Julian date
   9- 13  F5.2  mag     Umag      U magnitude
  15- 19  F5.2  mag     Bmag      B magnitude
  21- 24  F4.2  mag     Vmag      V magnitude
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Byte-by-byte Description of file: table2
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   Bytes Format Units   Label     Explanations
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   1-  7  I7    d       JD        Julian date
   9- 12  F4.2  mag     Jmag      J magnitude
  14- 18  F5.2  mag     Hmag      ? H magnitude
  20- 24  F5.2  mag     Kmag      ? K magnitude
  26- 30  F5.2  mag     Lmag      ? L magnitude
  32- 36  F5.2  mag     Mmag      ? M magnitude
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(End)                                         Patricia Bauer [CDS]   02-Apr-1996