J/PAZh/28/653 Pulsation Modes of Cepheid (Sachkov, 2002)
Two Period-Radius Relations for Classical Cepheids:
Determining the Pulsation Mode and the Distance Scale
Sachkov M.E.
<Pis'ma Astron. Zh. 28, 653 (2002)>
=2002PAZh...28..653S 2002PAZh...28..653S
=2002AstL...28..589S 2002AstL...28..589S
ADC_Keywords: Stars, variable
Abstract:
A catalog of pulsation mode and radii for 64 classical Cepheids based
on the 1995-2001 radial velocities observations with the correlation
spectrometer.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
objects.dat 57 64 Objects positions
table1.dat 44 13 First overtone Cepheid radii
table2.dat 44 51 Fundamental mode Cepheid radii
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Byte-by-byte Description of file: objects.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Star Name of the star system
12- 26 A15 --- OName Other star name
29- 30 I2 h RAh Right ascension (J2000)
32- 33 I2 min RAm Right ascension (J2000)
35- 41 F7.4 s RAs Right ascension (J2000)
43 A1 --- DE- [-+] Declination sign
44- 45 I2 deg DEd Declination (J2000)
47- 48 I2 arcmin DEm Declination (J2000)
50- 55 F6.3 arcsec DEs Declination (J2000)
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Star Star name in GCVS
11-16 F6.4 [d] logP1 Logarithm of first-overtone period
18-20 I3 solRad Rad Cepheid Radius in solar units
22-23 I2 solRad e_Rad Uncertainty in Rad
25-29 F5.2 --- delPhi Phase shift
31-34 F4.2 --- e_delPhi Uncertainty in delPhi
36-39 F4.2 mag AmpV Amplitude in V-band
41-44 F4.2 --- Mm Parameter of light curve in GCVS (G1)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Star Star name in GCVS
11-16 F6.4 [d] logP0 Logarithm of fundamental-mode period
18-20 I3 solRad Rad Cepheid Radius in solar units
22-23 I2 solRad e_Rad Uncertainty in Rad
25-29 F5.2 --- delPhi Phase shift
31-34 F4.2 --- e_delPhi Uncertainty in delPhi
36-39 F4.2 mag AmpV Amplitude in V-band
41-44 F4.2 --- Mm Parameter of light curve in GCVS (G1)
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Global Notes:
Note (G1): Duration of brightness rise from minimum to maximum
in fractions of the period.
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(End) Mikhail Sachkov, Veta Avedisova (INASAN) 14-Nov-2002