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J/other/Ser/180.71      Masses of visual binaries   (Cvetkovic+, 2010)
On the component masses of visual binaries.
    Cvetkovic Z., Ninkovic S.
   <Serbian Astron. Journal, 180, 71-80 (2010)>
   =2010SerAJ.180...71C
ADC_Keywords: Stars, double and multiple ; Stars, masses

Keywords: binaries: visual - stars: fundamental parameters


Abstract:
    In the Sixth Catalog of Orbits of Visual Binary Stars we found those
    belonging to the Main Sequence to form a sample containing 432 visual
    binaries. Their total masses were obtained dynamically, i.e. they were
    calculated using the orbital elements and the new Hipparcos
    parallaxes. For the same pairs the total mass was also found
    astrophysically - by applying the mass-luminosity relation. The
    apparent magnitudes of the components were found in two different
    ways: by deriving them from total magnitudes and magnitude
    differences, and by taking their values directly from a catalogue. The
    results for these two approaches show no essential discrepancy. The
    values of total masses obtained dynamically have a large dispersion
    involving even completely unrealistic values. This is a clear
    indication that the input data are not sufficiently reliable.
    Nevertheless, in a large number of cases the agreement between total
    masses obtained by us in two different ways is quite satisfactory
    indicating that i) for many visual binaries, as a rule not too distant
    and with high-quality orbital elements, the dynamical total masses can
    be reliable; ii) the mass-luminosity relation yields quite
    satisfactory estimates for the component masses when they belong to
    the Main Sequence and iii) a correlation between the relative parallax
    error and orbit grade exists.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table1.dat        96      431   Input data on binaries
table2.dat        68      364   Determined magnitudes and spectral types for
                              binary stars from subsample of 364 ones
table3.dat        80      431   Calculated masses for binary stars of the whole
                              sample


See also:
    I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)
    I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
    V/39  : 4th Catalog of Orbits of Visual Binaries (Worley+, 1983)
    http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/orb6 :
            6th Catalog of Orbits of Visual Binaries Home Page


Byte-by-byte Description of file: table1.dat

   Bytes Format Units   Label    Explanations

   1- 10  A10   ---     WDS      WDS number, HHMMm+DDMM
  12- 22  A11   ---     Name     Star name
  24- 29  I6    ---     HIP      HIP number
  31- 35  F5.2  mag     mt       ?=- Integrated magnitude of the pair
  37- 41  F5.3  mag     Dmag     ?=- magnitude difference
  43- 47  F5.2  mag     m1       Magnitude of A component
  49- 53  F5.2  mag     m2       ?=- Magnitude of B component
  55- 60  F6.2  mas     plx      New parallax (van Leeuwen, 2007, Cat. I/311)
  61- 62  A2    ---     u_plx    [??] Uncertainty flag on plx
  64- 70  F7.2  yr      Per      Period (1)
  72- 77  F6.3  s       a        Semimajor axis of orbit (1)
      79  I1    ---     G        [1/5] Grade of orbit, 1 is best (1)
  81- 87  F7.2  yr      Per2     ? Second period from second grade
  90- 94  F5.3  s       a2       ? Second orbit semimajor axis from second grade
      96  I1    ---     G2       [2/5]? Second grade of orbit

Note (1): From Sixth Catalog of Orbits of Visual Binary Stars,
     http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/orb6


Byte-by-byte Description of file: table2.dat

   Bytes Format Units   Label     Explanations

   1-  6  I6    ---     HIP       HIP number
   8- 12  F5.2  mag     m1.I      ? Apparent magnitude of component A
                                    according to Approach I
  14- 18  F5.2  mag     m2.I      ? Apparent magnitude of component B
                                    according to Approach II
  20- 24  F5.2  mag     Mag1.I    ? Absolute magnitude of component A
                                    according to Approach I
  26- 30  F5.2  mag     Mag2.I    Absolute magnitude of component B
                                    according to Approach I
  32- 36  F5.2  mag     m1.II     ? Apparent magnitude of component A
                                    according to Approach I
  38- 42  F5.2  mag     m2.II     ? Apparent magnitude of component B
                                    according to Approach II
  44- 48  F5.2  mag     Mag1.II   ? Absolute magnitude of component A
                                    according to Approach II
  50- 54  F5.2  mag     Mag2.II   ? Absolute magnitude of component B
                                    according to Approach II
  56- 57  A2    ---     Sp1       Spectral type of component A
  59- 60  A2    ---     Sp2       Spectral type of component B
  62- 68  A7    ---     SpType    WDS spectral type


Byte-by-byte Description of file: table3.dat

   Bytes Format Units   Label    Explanations

   1-  6  I6    ---     HIP      HIP number
       8  I1    ---     G        Grade of orbit (1 is the best)
  10- 15  F6.2  mas     plx      Parallax
  17- 21  F5.2  mas     e_plx    rms uncertainty on plx
  23- 29  A7    ---     SpType   WDS spectral type
  31- 35  F5.2  Msun    M1.I     ? Mass of primary according to Approach I
  37- 41  F5.2  Msun    M2.I     ? Mass of secondary according to Approach I
  43- 47  F5.2  Msun    Mt.I     ? Mass of the pair according to Approach I
  49- 53  F5.2  Msun    M1.II    ? Mass of primary according to Approach II
  55- 59  F5.2  Msun    M2.II    ? Mass of secondary according to Approach II
  61- 65  F5.2  Msun    Mt.II    ? Mass of the pair according to Approach II
  67- 71  F5.2  Msun    Mdyn     ? Dynamical mass of the pair
      72  A1    ---     n_Mdyn   [>] > when dynamical mass exceeds 100M☉
  74- 75  A2    ---     Rem      [*m ] Large discrepancies (1)
  77- 80  F4.2  Msun    Mdyn2    ? Second dynamical mass of the pair

Note (1): Notes as follows:
   * = large discrepancy between astrophysical and dynamical total masses
   m = multiple star


History:
    From electronic version of the journal
(End)                                      Patricia Vannier [CDS]    04-Apr-2011