A study of the bright stars. I. A catalogue of spectral classifications.

Cowley, A. P.; Cowley, C. R.; Jaschek, M.; Jaschek, C.

doi:10.1086/110819

Cited by 261 publications

(204 citation statements)

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“…This represents an increase of 0.9 dex over the value of 3.9 obtained by Cameron (1973) Cowley et al 1969). An interesting problem arises in connection with the determination of vanadium abundances in HR 465(b) and HR 8216.…”

Section: Vanadium Abundancesmentioning

confidence: 46%

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Vanadium abundances in early A stars

Cowley¹,

Elste²,

Urbanski³

1978

PASP

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Vanadium-to-hydrogen ratios have been determined for o Peg, HR 6127, HR 465 (rare earth minimum), and HR 8216. With respect to the solar system, vanadium is overabundant in the first two stars, possibly normal in the third, and underabundant in the fourth. The range in the V/H ratio in these four stars is between one and two orders of magnitude. An intercomparison of the four spectra shows that the strong V n lines occur in the stars with weaker Cr and Fe spectra. The vanadium anomaly is thus suggestive of the well-known calcium anomaly in peculiar A stars, but we believe that vanadium and calcium abundances are not closely correlated.

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Section: Vanadium Abundancesmentioning

confidence: 46%

“…The calcium deficiency in 73 Dra (cf. Sadakane 1976), has long been recognized; its Kline type (Cowley et al 1969) is A0. In HR 8216, however, Sargent, Strom, and Strom (1969) find calcium to be normal, or overabundant.…”

Section: Discussionmentioning

confidence: 99%

Vanadium abundances in early A stars

Cowley¹,

Elste²,

Urbanski³

1978

PASP

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“…(1) Reed (2005); (2) Niemczura (2003); (3) (2002); (7) Cucchiaro et al (1980); (8) Hohle, Neuhäuser & Schutz (2010); (9) Fitzpatrick & Massa (2007); (10) Cowley et al (1969); (11) Warren & Hesser (1977); (12) Lefever et al (2010); (13) Koen & Eyer (2002); (14) Kilambi (1975); (15) Houk & Cowley (1975); (16) Gudennavar et al (2012); (17) Abt, Levato & Grosso (2002); (18) Vogt et al (1998); (23) Grillo et al (1922); (24) Tobin (1985); (25) Turner (1973); (26) Wegner (2003); (27) Vleeming (1974); (28) obtained from models from left-bottom edges with neglected overshooting, respectively. Therefore, based on the differences between the cases with and without overshooting, we can estimate the error in mass in Table 1 to be at least a few tenths of a solar mass, and the error in the critical rotation frequency in Table 2 to be at least 0.25 d −1 .…”

Section: ±0003 ±1mentioning

confidence: 99%

Identification of pulsational modes in rotating slowly pulsating B-type stars

Szewczuk

Daszyńska‐Daszkiewicz

2015

Monthly Notices of the Royal Astronomical Society

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Knowledge of the geometry of pulsational modes is a prerequisite for seismic modelling of stars. In the case of slowly pulsating B-type (SPB) pulsators, the simple zero-rotation approach so far used for mode identification is usually not valid because pulsational frequencies are often of the order of the rotational frequency. Moreover, this approach allows us to determine only the spherical harmonic degree, , while the azimuthal order, m, is beyond its reach. On the other hand, because of the density of oscillation spectra of SPB stars, knowledge of m is indispensable if one wants to assign the radial order, n, to the observed frequency peaks. Including the effects of rotation via the traditional approximation, we perform identification of the mode angular numbers ( , m) for 31 SPB stars with available multicolour time series photometry. Simultaneously, constraints on the rotational velocity, V rot , and the inclination angle, i, are determined assuming uniform rotation and a constant value of V rot sin i. Dependence of the results on the adopted model is tested using HD 21071 as an example. Despite some model uncertainties and limitations of the method, our studies show the correct approach to identifying the low-frequency oscillation modes.

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“…Bertaud (1959) classified it as AOp-EuCr, Cowley et al (1969) as B9p-Eu(Cr? ), Osawa (1965) as Hg and Zverko (1974) as Mntype.…”

Section: Introductionmentioning

confidence: 99%

Spectrum Analysis of the Binary Star 53 Aur with a CP3 Component

Zverko

Budaj

Zboril

et al. 1993

International Astronomical Union Colloquium

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The CP-star 53 Aur (HD 47152, HR 2425) has been assigned in the literature different types of peculiarity. Bertaud (1959) classified it as A0p-EuCr, Cowley et al. (1969) as B9p-Eu(Cr?), Osawa (1965) as Hg and Zverko (1974) as Mn -type. MacAlister (1978) discovered its binary nature and Tokovinin (1986) first determined its orbit with a period of 13.7 y. Subsequent interferometric observations by Baize (1989) yielded new orbital elements with a period of 25.816 y, total mass of 5.8 M⊙ and magnitude difference of two B9 components 0.3 mag. Adelman (1982) performed spectrophotometry and fitted the Balmer jump with Teff=10 500 K, while the Paschen continuum with Teff=9 500 K, log g=4 in both cases. Palmer (1965) estimated the projected rotational velocity to 325 km s−1 from the width of the Ca II-K line, while Wolff and Preston (1975) obtained 33 km s−1 from the Mg II 448.1 nm line. In this work we analyze high-dispersion spectra obtained in two distant orbital phases, namely in 1975 and in 1992 to distinguish the components of the system.

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A study of the bright stars. I. A catalogue of spectral classifications.

Cited by 261 publications

References 0 publications

Vanadium abundances in early A stars

Vanadium abundances in early A stars

Identification of pulsational modes in rotating slowly pulsating B-type stars

Spectrum Analysis of the Binary Star 53 Aur with a CP3 Component

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