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V/85 Stellar Mass Catalogue (Belikov 1995)
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Stellar Mass Catalogue. Preliminary Version
Belikov A.N.
<Bull. Inf. CDS 47, 9 (1995)>
=1995BICDS..47....9B
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ADC_Keywords: Stars, masses
Description:
The catalogue includes binary stars for which dynamical masses of
components has been published in 1969 - 1988. It doesn't contain other
compilation catalogues that were published in this two decades and uses
original data papers only. It collects masses defined by direct,
dynamical methods only (without use of mass-luminosity, mass-radius,
mass-spectrum and similar relations).
The work was supervised by Dr O. Malkov.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 99 360 The catalogue
refs.dat 114 246 References
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Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Name Principal name of the system
14- 25 A12 --- OtherID Secondary identifier of the system
27- 33 F7.4 solMass M1 Mass of primary component
35- 40 F6.4 solMass e_M1 ? Mean error on M1
42- 48 F7.4 solMass M2 Mass of secondary component
50- 55 F6.4 solMass e_M2 ? Mean error on M2
57- 58 A2 --- Method Method of mass determination (1)
60- 61 A2 --- Note explained in note (5)
63- 72 A10 --- AAAref Reference from AAA (2)
74- 78 A5 --- System Type of system (3)
80- 99 A20 --- Sp Spectral types of the two stars (4)
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Note (1): Methods of mass determination:
S - methods for double lined spectroscopic binaries:
The inclination of the system are derived from :
S0 resolved light curve;
S1 visual orbit;
S2 speckle-interferometry;
S3 polarimetry.
V - methods for visual binaries:
Photographic magnitude difference
V0 is known;
V1 is assumed to be zero;
V2 is calculated from visual magnitudes and spectra;
V3 is calculated from visual magnitudes and difference
visual and photographic photocentric semimajor axes;
V4 is known from speckle - interferometry;
V5 is calculated from J,H,K magnitude differences.
R - methods for resolved spectroscopic binaries:
R0 orbital parallax used.
R1 trigonometric parallax used.
Note (2): number of the paper in Astronomy and Astrophysics Abstracts,
made of Volume . Section . Paper number
The references are explained in file "refs.dat"
Note (3): Types of system abbreviations, the colon (:) indicates
an uncertainty:
Al Algol-type star
c contact system
ce evolved contact system
d detached system
dn dwarf nova
fl flare star
nc near contact system
p.RS precursor of the RS CVn-type system
R R CMa-type star
RS RS CVn-type star
S W Ser-type star
sd semidetached system
W W UMa-type star
WA W UMa-type star,type A
WB W UMa-type star,type B
WR binary system with Wolf-Raet star
WW W UMa-type star,type W
Note (4): Spectra abbreviations:
e. early
m. middle
l. late
? unknown spectrum
(Sp) questionable spectrum
+ division of primary and secondary component spectra
; division of composed spectrum of system and component's spectra
- uncertainty in spectral class
/ uncertainty in luminosity class
Note (5): Individual Notes:
a authors calculated all needed parameters, but didn't
calculate final masses.
b the trigonometric parallax used too.
c authors used dynamic parallax to calculate sum of mass, but
the system has trigonometric parallax the same. Authors calculated
all needed parameters, but didn't calculate final masses.
d authors used dynamic parallax to calculate sum of mass but
the system has trigonometric parallax the same.
1 the second of this pair is the intrinsic variable star .
2 to determine mass ratio authors used self-determined
radial velocities.
3 with mass ratio from Wilson & Devinney , ApJ 182, 539, 1973
4 the final stage of the B-type W UMa configuration
5 used orbit from Lippincott S.L., 1981, PASP 93, 376
6 used orbit from Russell & Gatewood, 1983, PASP 96, 429
7 a system between Roche-lobe filling stage of case C
(post-helium flash) mass transfer
8 1) the primary is near filling its Roche lobe;
2) intrinsic activity is detected;
3) a member of NGC 752.
9 the secondary is intrinsic variable of delta Scuti type.
10 these system is a member of open cluster NGC 6231 of the Sco OB1
association.
11 sp.elements from Struve & Gratton, 1948, ApJ 108, 497
12 sp.elements from Struve & Zetergi, 1959, ApJ 130, 789
13 sp.elements from King & Hilditch , 1984, MNRAS 209, 645
14 this system is passing through a transition state from a
semidetached configuration, reached via case A mass transfer
episode to become an evolved and deep-contact A-type W UMa system.
15 UV Cet is B - component of L726-8(A+B).
16 using sp.elements by Harper W.E., Pearce J.A., Petrie R.M.,
Mckellar A., JRASC 29, 411, 1935
17 using sp.elements by Popper D.M., ApJ 166, 366, 1971
18 primary component is the beta-Cepheid star.
19 Algol-type eclipsing binary with an evolved and less-massive
secondary component (must be filling it's Roche lobe)
20 this system has more than two stars (from anomalous large
total mass) maybe.
21 the secondary has evolved G9 spectrum.
22 the system has third component of A7V spectrum.
23 the system has third component.
24 the system has third component of K5 spectrum.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- AAAref Reference as in "catalog.dat"
12-114 A103 --- Text of reference
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Historical Notes:
The decimal points have been added where necessary.
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(End) Francois Ochsenbein [CDS] 19-Jul-1995