J/A+A/311/523 Photometry of W UMa (Maceroni+, 1996)
The properties of W Ursae Majoris contact binaries: new results and old problems
Maceroni C., van't Veer F.
<Astron. Astrophys. 311, 523 (1996)>
=1996A&A...311..523M 1996A&A...311..523M (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Magnitudes ; Spectral types ; Reddening
Keywords: binaries: close - star: evolution - stars: mass loss
Abstract:
The physical properties of W UMa binary systems are revisited on the
basis of the observational data published in the last decade and of
the recent theoretical studies on angular-momentum-loss-driven secular
evolution. The absolute elements (masses, radii, luminosities) are
derived by an inference method and a calibration based on the
available high quality spectroscopic orbits. The derived age
(8Gy) agrees with the estimate of Guinan and Bradstreet from space
motions. The analysis of the resulting physical parameters shows
little correlation between the standard classification in A and W
subtype (first proposed by Binnendijk (1970) and only related to the
light curve morphology) and the evolutionary status and origin of the
systems. Most A-subtype systems seem to have no evolutionary link with
W-subtype ones. The relation between total mass and mass ratio for the
"bona fide" sample also suggests that mass loss from the system may
play an important role.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1 59 78 Basic observational data of W UMa binaries
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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- 2 I2 --- No Sequential number (1)
5- 12 A8 --- Name Star name
15- 20 F6.4 d Per Orbital period
23- 27 F5.2 mag MaxMag Maximum magnitude
30- 34 F5.2 mag MinMag Minimum magnitude
37 A1 --- MagType [VPB] Type of magnitudes
40- 46 A7 --- Sp Spectral type(s)
49- 52 F4.2 mag B-V ? B-V color index
55- 58 F4.2 mag E(B-V) ? Reddening
59 A1 --- u_E(B-V) Uncertainty flag on E(B-V)
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Notes (1): Systems denoted by sequential numbers from 1 to 48 are
classified as W-subtype, the others as A-subtype (Binnendijk L, 1970,
Vistas in Astr. 12, 217). Within each sub-type systems are ordered
according to increasing orbital period.
The values presented derive from the papers on individual systems
listed in the original paper (Table 2), or from the General Catalogue
of Variable Stars 4th ed. (Khopolov P.N. et al. 1985, Nauka Publ. Co.,
Moscow, Catalogue II/195) and the Eight Catalogue of the orbital
elements of spectroscopic binary systems (Batten A.H., Fletcher J.M,
MacCarthy D.G., 1989 Publ. D.A.O. vol XVII, Catalogue V/64).
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Courtesy: Carla Maceroni
(End) Patricia Bauer [CDS] 09-Apr-1996