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J/ApJ/655/1046      Abundances of φ Her                    (Zavala+, 2007)

The mercury-manganese binary star φ Herculis: detection and properties of the secondary and revision of the elemental abundances of the primary. Zavala R.T., Adelman S.J., Hummel C.A., Gulliver A.F., Caliskan H., Armstrong J.T., Hutter D.J., Johnston K.J., Pauls T.A. <Astrophys. J., 655, 1046-1057 (2007)> =2007ApJ...655.1046Z
ADC_Keywords: Binaries, spectroscopic ; Abundances, peculiar ; Equivalent widths Keywords: astrometry - binaries: spectroscopic - stars: abundances - stars: chemically peculiar - stars: individual (phi Herculis AB) Abstract: Observations of the mercury-manganese star phi Her with the Navy Prototype Optical Interferometer (NPOI) conclusively reveal the previously unseen companion in this single-lined binary system. The NPOI data were used to predict a spectral type of A8 V for the secondary star phi Her B. This prediction was subsequently confirmed by spectroscopic observations obtained at the Dominion Astrophysical Observatory. phi Her B is rotating at 50±3km/s, in contrast to the 8 km/s lines of phi Her A. Recognizing the lines from the secondary permits one to separate them from those of the primary. The abundance analysis of phi Her A shows an abundance pattern similar to those of other HgMn stars, with Al being very under-abundant and Sc, Cr, Mn, Zn, Ga, Sr, Y, Zr, Ba, Ce, and Hg being very overabundant. Description: phi Her was observed with the NPOI in 25 different epochs from 1997 April 19 to 2005 June 16. Objects: ---------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------- 16 08 46.2 +44 56 06 phi Her = V* phi Her ---------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 70 25 Astrometric solutions for φ Her table7.dat 36 196 Abundances of φ Her including new lines table8.dat 39 33 Comparison of derived and solar abundances (log N/H)
See also: J/A+A/367/597 : ups Her, phi Her + HR 7018 abundances (Adelman+, 2001) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 A3 --- ObsM UT Month of NPOI observation 5- 6 I2 d ObsD UT Day of NPOI observation 8- 16 F9.4 yr ObsY Julian Year of NPOI observation 18- 22 F5.2 mas rho Fitted binary separation 24- 29 F6.2 deg theta Fitted binary position angle 31- 34 F4.2 mas errMaj Semimajor axis of error ellipse 36- 39 F4.2 mas errMin Semiminor axis of error ellipse 41- 45 F5.1 deg errPA Position angle of error ellipse 47- 51 F5.2 mas Crho Calculated binary separation 53- 58 F6.2 deg Ctheta Calculated binary position angle 60- 64 F5.2 mas (O-C)rho Binary separation (O-C) value 66- 70 F5.2 deg (O-C)theta Binary position angle (O-C) value
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Ion Species name (1) 7- 9 A3 --- Mult Muliplet identification (2) 11- 18 F8.3 0.1nm lambda ? Laboratory wavelength in Angstroms 19- 23 F5.2 [-] log(gf) ? Log of the gf value 25- 26 A2 --- r_log(gf) Reference for log(gf) (3) 28- 30 I3 0.1pm EW ? Observed equivalent width in milliAngstroms 32- 36 F5.2 [-] logN/NT ? Log of the derived number abundance
Note (1): The adopted abundance from HgIIλ3984 is from Woolf & Lambert (1999ApJ...521..414W). Note (2): The multiplet numbers are from Moore (1945, A Multiplet Table of Astrophysical Interest (Princeton: Princeton Univ. Obs.) except that I indicates Mn II lines from Iglesias & Velasco (1964, Publ. Inst. Opt. Madrid, No. 23) and J indicates Fe II lines from Johansson (1978, Phys. Scr., 18, 217 ). Note (3): The gf value references (including those for older lines): BG = Biemont et al. (1989A&A...209..391B for V II; Biemont (1981ApJ...248..867B) for Zr II DW = Dworetsky (1980A&A....84..350D) GB = Grevesse et al. (1981, in Proc. 23rd Liege Astrophys. Colloq., Upper Main Sequence Stars , 211) HL = Hannaford et al. (1982ApJ...261..736H) KX = Kurucz & Bell (1995, CD-ROM 23, Atomic Data for Opacity Calculations) LA = Lanz & Artru (1985, Phys. Scr., 32, 115) LD = Lawler & Dakin (1989, J. Opt. Soc. Am. B, 6, 1457) MF = Fuhr et al. (1988) and Martin et al. (1988), Cat. VI/72 MC = Magazzu & Cowley (1986ApJ...308..254M) N4 = Fuhr & Wiese (2006, J. Phys. Chem. Ref. Data, 35, 1669) WF = Wiese, Fuhr & Deters (1996, J. Phys. Chem. Ref. Data Monogr. Vol. 7) WM = Wiese & Martin (1980, Wavelengths and Transition Probabilities for Atoms and Atomic Ions, Part 2) WS = Wiese, Smith & Glennon (1966, Atomic Transition Probabilities, Hydrogen through Neon (NSRDS-NBS 4) and Wiese, Smith & Miles (1969, Atomic Transition Probabilities, Vol. 2, Sodium through Calcium, NSRDS-NBS 22).
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Ion Species name (1) 8- 12 F5.2 [-] AAbd ? Adelman et al. (2001, Cat. J/A+A/367/597) φ Her A abundance 14- 17 F4.2 [-] e_AAbd ? Uncertainty in AAbd 19- 23 F5.2 [-] ATP This paper's φ Her A abundance 25- 28 F4.2 [-] e_ATP ? Uncertainty in ATP (2) 30- 32 I3 --- n_ATP ? Number of lines used in ATP 34- 39 F6.2 [-] Sun Solar abundance (3)
Note (1): The Hg II value adopted for this study is that of Woolf & Lambert (1999ApJ...521..414W), the Nd and Pr abundances are from Dolk et al. (2002A&A...385..111D). Note (2): When more than one line is detected the error is the standard deviation of the mean. No error is quoted when only one line is present. Note (3): From Grevesse, Noels & Sauval (1996, in ASP Conf. Ser. 99, 117).
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 10-Dec-2008
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