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 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:
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RA (2000) DE Designation(s)
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16 08 46.2 +44 56 06 phi Her = V* phi Her
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File Summary:
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FileName Lrecl Records Explanations
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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)
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See also:
J/A+A/367/597 : ups Her, phi Her + HR 7018 abundances (Adelman+, 2001)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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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
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Note (1): The adopted abundance from HgIIλ3984 is from
Woolf & Lambert (1999ApJ...521..414W 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 1989A&A...209..391B for V II;
Biemont (1981ApJ...248..867B 1981ApJ...248..867B) for Zr II
DW = Dworetsky (1980A&A....84..350D 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 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 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).
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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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)
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Note (1): The Hg II value adopted for this study is that of Woolf & Lambert
(1999ApJ...521..414W 1999ApJ...521..414W), the Nd and Pr abundances are from Dolk et al.
(2002A&A...385..111D 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).
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 10-Dec-2008