The Spectrum of Singly Ionized Phosphorus, P II

Svendenius, Nils; Magnusson, Carl-Erik; Zetterberg, Per Olof

doi:10.1088/0031-8949/27/5/005

Cited by 31 publications

(16 citation statements)

References 8 publications

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“…These data (air wavelength λ id , ionic species, log gf , the energy of the lower and upper levels of the transition, and the combination of configurations comprising the multiplet) are all extracted from the line list data of Kurucz (1995), with the exception of all data for P II (Svendenius et al 1983), wavelengths for the Mn II ( 6 S)4d e 5 D−( 6 S)4f 5 F multiplet lines (Johansson et al 1995), and several energy level assignments for Fe II (Johansson, private communication). The last column in both tables provides the absorption line depth (Depth) computed by the SYNTHE program for the line center, on a scale where the normalized continuum level has a value of 1.000.…”

Section: Line List Descriptionmentioning

confidence: 99%

Emission lines in the optical spectrum of 3 Cen A

Wahlgren

Hubrig²

2004

A&A

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Abstract. Previously, weak emission lines had been detected at red wavelengths in the spectra of a limited sample of mid to late B type main sequence stars. A fuller description of the occurrence and origins of these lines has yet to be forwarded, in part due to the lack of observations detailing the spectral transitions involved. To address this deficiency, we present a line list of weak emission features found in the optical and near infrared spectral region of the chemically peculiar He-weak star 3 Cen A (HD 120709). Nearly 350 features, mostly associated with allowed transitions from high-excitation states of first ions, are catalogued along with identifications. Prominent among the emission lines are the spectra P II, Mn II, Fe II, Ni II and Cu II. Emission lines from Ca II, Si II and Hg II are also evident. Abundances are determined for several elements from synthetic spectrum fitting, with anomalies detected for the ions O I/II, P II/III and Si II/III. The LTE synthetic spectrum fitting also revealed that the low excitation 4s−4p transitions of Fe II predict an abundance that is greater than that determined from higher excitation 4d−4f transitions. Several of these latter transitions have upper energy levels that are found to be associated with emission lines. We also present empirical considerations for the excitation processes leading to the weak emission lines.

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Section: Line List Descriptionmentioning

confidence: 99%

Emission lines in the optical spectrum of 3 Cen A

Wahlgren

Hubrig²

2004

A&A

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“…The stellar lines were identified with the general references A Multiplet Table of Astrophysical Interest (Moore 1945) and Wavelengths and Transition Probabilities for Atoms and Atomic Ions, Part 1 (Reader & Corliss 1980) as well as Svendenius et al (1983) for P II, Pettersson (1983) for S II, Huldt et al (1982) for Ti II, Catalan et al (1964) for Mn I, Iglesias & Velasco (1964) for Mn II, Nave et al (1994) for Fe I, and Dworetsky (1971), Johansson (1978), Guthrie (1985), and Adelman (1987) for Fe II, and Isberg & Litzen (1985) for Ga II.…”

Section: The Spectramentioning

confidence: 99%

Elemental abundance analyses with DAO spectrograms

Adelman

Gulliver

Rayle

2001

A&A

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Abstract. Elemental abundances analyses are performed for the Mercury-Manganese stars υ Her, φ Her, and HR 7018 consistent with previous studies of this series using spectrograms obtained with Reticon and CCD detectors. Comparisons of the first two analyses with those performed using coadded photographic plates show the general consistency of the derived elemental abundances. For υ Her and for φ Her, abundances were newly found for O, and for Al, V, Zn, and Ce, respectively. HR 7018 is discovered to be a single-lined spectroscopic binary. Its Sc abundance is the smallest of any class member with derived abundances and its Sr abundance the largest of any known HgMn star. A correlation analysis of the most complete abundance sets for 20 HgMn stars shows that the abundances of some elements are correlated with one another and some are functions of the stellar effective temperature.

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“…The stellar lines were identified with the general references A Multiplet Table of Astrophysical Interest (Moore 1945) and Wavelengths and Transition Probabilities for Atoms and Atomic Ions, Part 1 (Reader & Corliss 1980) as well as the more specialized references for P II (Svendenius et al 1983), S II (Pettersson 1983), Ti II (Huldt et al 1982), Mn II (Iglesias & Velasco 1964), and Fe II (Johansson 1978). Baschek (1973) discussed the analyses of α Scl independently carried out by Schmitt (1972Schmitt ( , 1973 and Vilhu (1972).…”

Section: Observational Materials and Line Identificationsmentioning

confidence: 99%

Elemental abundance studies of CP stars

López-García

Adelman

Pintado

2001

A&A

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Abstract. Fine analyses of the magnetic CP stars α Scl and HD 170973 are presented using ATLAS9 model atmospheres which have same bulk metallicity as the deduced abundances. The light elements are mostly solar except for silicon, and all the heavier elements except nickel in HD 170973, which is solar, are greatly overabundant. The iron peak elements are typically 10 times overabundant, Sr is of order of 1000 times solar, Y and Zr are of order of 100 times solar. The rare earths are 1000 or more times overabundant.

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The Spectrum of Singly Ionized Phosphorus, P II

Cited by 31 publications

References 8 publications

Emission lines in the optical spectrum of 3 Cen A

Emission lines in the optical spectrum of 3 Cen A

Elemental abundance analyses with DAO spectrograms

Elemental abundance studies of CP stars

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