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J/BaltA/14/51    Elemental abundances of 4 Lac and nu Cep    (Yuce+, 2005)

Elemental abundances of 4 Lacertae and ν Cephei Yuce K. <Baltic Astron., 14, 51 (2005)> =2005BaltA..14...51Y
ADC_Keywords: Stars, supergiant ; Equivalent widths ; Abundances, peculiar Keywords: stars: supergiants, abundances, atmosphere - stars: individual: 4 Lac, nu Cep Abstract: Elemental abundance analysis based on high S/N and high resolution Dominion Astrophysical Observatory spectrograms have been performed for two early type supergiants: 4 Lac (B9 Iab) and ν Cep (A2 Ia). Lines as weak as of order 5mÅ are employed in this study. The projected rotational velocities of these stars are 14 and 26km/s, respectively. Both stars show similar radial velocity amplitudes, macroturbulent velocities and the same general elemental abundance trends. Their He, CNO and light element abundances are solar or overabundant while the iron peak and heavy element abundances are solar or underabundant. Detailed LTE model atmosphere abundance analysis shows that 4 Lac has nuclearly processed matter in its photosphere while ν Cep does not. Description: 4 Lac and ν Cep are two early type supergiants. Table A1 contains the elemental abundances for the stars. It is grouped by atomic species with the lines listed by multiplet and within multiplets by numerical order. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 22 24 31.0 +49 28 35 4 Lac = HD 212593 21 45 26.9 +61 07 15 nu Cep = HD 207260 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file abund.dat 33 25 Atomic abundances tablea1.dat 55 383 Elemental abundances of 4 Lac and ν Cep tablea1.tex 74 571 LaTeX version of tablea1.dat and abund.dat
See also: J/A+A/406/975 : Elemental abundances of four A-B stars (Kocer+, 2003) J/A+A/406/987 : Elemental abundances of three CP stars (Pintado+, 2003) J/A+A/394/187 : γ Ser + 101 Her elemental abundances (Caliskan+, 2002) J/A+A/367/597 : ups Her, phi Her + HR 7018 abundances (Adelman+, 2001) J/A+A/367/859 : α Scl and HD 170973 abundances (Lopez-Garcia+, 2001) J/A+A/371/1078 : Elemental abundance of 4 normal B & A stars (Adelman+, 2001) J/MNRAS/316/514 : 28 And + 99 Her elemental abundances (Adelman+, 2000) J/A+A/354/899 : Elemental abundance analyses IV. (Adelman+, 2000) J/A+AS/137/227 : HD 133029 & HD 192913 abundances (Lopez-Garcia+ 1999) J/A+AS/129/563 : Abundances of HR 4487, 14 Hyd and 3 Cen A (Pintado+ 1998) J/A+AS/125/219 : Abundances of mu Lep, 7 Sex, HR 4817 + 28 Her (Adelman+ 1997) J/A+AS/107/353 : HD 43819 & HD 147550 abundances (Lopez-Garcia+, 1994) Byte-by-byte Description of file: abund.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Ion Ion 8- 9 A2 --- Element Element (identical to bytes 1-2) 12- 16 F5.2 --- log(Nel/Ntot)1 ? 4 Lac derived abundance of Element (1) 18- 21 F4.2 --- e_log(Nel/Ntot)1 ? rms uncertainty on log(Nel/Ntot)1 23- 28 F6.2 --- log(Nel/Ntot)2 ? nu Cep derived abundance of Element (1) 30- 33 F4.2 --- e_log(Nel/Ntot)2 ? rms uncertainty on log(Nel/Ntot)2
Note (1): Ratio of number of atoms to the total number of atoms per unit volume
Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Ion Ion 8- 13 A6 --- Mult Multiplet number (1) 15- 21 F7.2 0.1nm Lambda Laboratory wavelength 23- 27 F5.2 --- log(gf) log gf value 29- 30 A2 --- r_log(gf) loggf value reference (3) 32- 36 F5.1 0.1pm EW1 ? Equivalent width for 4 Lacertae 38- 42 F5.2 --- log(El/Ntot)1 ? Derived abundance for 4 Lacertae (2) 44- 48 F5.1 0.1pm EW2 ? Equivalent width for ν Cep 50- 55 F6.2 --- log(El/Ntot)2 ? Derived abundance for nu Cep (2)
Note (1): Multiplet number from Moore 1945 if first line of multiplet; if not from Moore an initial indicating the paper Note (2): Derived abundance in relative number of atoms per unit volume Note (3): gf value references are as follows: BG = Biemont et al. (1989A&A...209..391B) for V II, Biemont et al. (1981ApJ...248..867B) for Zr II FW = Fuhr & Wiese (1990, in Lide, D. R. ed, CRC Handbook of Chemistry and Physics, CRC Press, Cleveland, OH) and Fuhr & Wiese (1998, In ed. D. R. Lide, CRC Handbook of Chemistry and Physics, 79th ed., CRC Press Inc., Boca Raton) GB = Grevesse et al. (1981, Upper Main Sequence CP Stars, 23rd. Liege Astrophys. Coll., 211) HL = Hannaford et al. (1982ApJ...261..736H); KG = Kurucz (guess-1995, In: Adelman S.J., Wiese W.L. (eds.) Astrophysical Applications of Powerful New Databases. ASP Conference Series, p. 205) KP = Kurucz & Peytremann (1975, SAO Special Report No. 362, part. 1) KX = Kurucz & Bell (1995, Kurucz CD-Rom No. 23) LA = Lanz & Artru (1985PhyS...32..115L) LD = Lawler & Dakin (1989, JOSA B, 6, 1457) MF = Fuhr, Martin & Wiese, 1988, and Martin, Fuhr & Wiese, 1988, Cat. VI/72 SG = Schulz-Gulde (1969, JQSRT, 9, 13) WF = Wiese, Fuhr & Deters (1996, Atomic transition probabilities of carbon, nitrogen, and oxygen : a critical data compilation. Edited by W.L. Wiese, J.R. Fuhr, and T.M. Deters. Washington, DC) WM = Wiese & Martin (1980, NSRDS-NBS 68. Part 2, US Government Printing Office, Washington, DC); WS = Wiese, Smith & Glennon (1966, NSRDS-NBS 4, US Governement Printing Office, Washington) and Wiese, Smith & Miles (1969, NSRDS-NBS, D.C.: US Department of Commerce, National Bureau of Standards)
Acknowledgements: Kutluay Yuce, kyuce(at)astro1.science.ankara.edu.tr
(End) Patricia Vannier CDS 07-Mar-2005
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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