Spectral types of 80 early-type stars of variable radial velocity

Bidelman, W. P.; Ratcliff, S. J.; Svolopoulos, S. N.

doi:10.1086/132242

Cited by 10 publications

(6 citation statements)

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“…Abt (1985) gave the spectral type A2 Vn λ Boo, but Bidelman, Ratcliff, & Svolopoulos (1988) did not note peculiarity in their spectral type of A3 Vn and Paunzen et al (2001) recorded a spectral type A3 Van, i.e. not λ Boo although they were specifically looking for λ Boo stars.…”

Section: Notes On Members Of the λ Boo Classmentioning

confidence: 99%

An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue

Murphy

Corbally²,

Gray

et al. 2015

Publ. Astron. Soc. Aust.

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The literature on the λ Boo stars has grown to become somewhat heterogenous, as different authors have applied different criteria across the UV, optical and infrared regions to determine the membership status of λ Boo candidates. We aim to clear up the confusion by consulting the literature on 212 objects that have been considered as λ Boo candidates, and subsequently evaluating the evidence in favour of their admission to the λ Boo class. We obtained new spectra of ∼90 of these candidates and classified them on the MK system to aid in the membership evaluations. The re-evaluation of the 212 objects resulted in 64 members and 103 non-members of the λ Boo class, with a further 45 stars for which membership status is unclear. We suggest observations for each of the stars in the latter category that will allow them to be confidently included or rejected from the class. Our reclassification facilitates homogenous analysis on group members, and represents the largest collection of confirmed λ Boo stars known. c 0000 RAS

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Section: Notes On Members Of the λ Boo Classmentioning

confidence: 99%

An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue

Murphy

Corbally²,

Gray

et al. 2015

Publ. Astron. Soc. Aust.

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“…HD 81 104 duplicity has been detected by Bidelman et al (1988); they classified this star as A3Vn SB2.…”

Section: Binaries With Composite Spectramentioning

confidence: 99%

The heterogeneous class ofλBootis stars

Gerbaldi

Faraggiana²,

Lai³

2003

A&A

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Abstract. We demonstrate that it is arduous to define the λ Boo stars as a class of objects exhibiting uniform abundance peculiarities which would be generated by a mechanism altering the structure of their atmospheric layers. We collected the stars classified as λ Boo up to now and discuss their properties, in particular the important percentage of confirmed binaries producing composite spectra (including our adaptive optics observations) and of misclassified objects. The unexplained RV variables (and thus suspected binaries), the known SB for which we lack information on the companion, the stars with an UV flux inconsistent with their classification, and the fast rotating stars for which no accurate abundance analysis can be performed, are also reviewed.

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“…• 245, SAO 36891, HIP 4983) is a little studied bright B2IV-V (Guetter 1968) or B3III (Bidelman et al 1988) star. Božić & Harmanec (1998) discovered light and colour variations of this star, having repetitive brightenings accompanied by a reddening of the (B − V) index and a Send offprint requests to: H. Božić, e-mail: hbozic@geodet.geof.hr…”

Section: Introduction Hd 6226 (Bd+46mentioning

confidence: 99%

Properties and nature of Be stars

Božić

Harmanec

Yang

et al. 2004

A&A

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Abstract. Photometric and spectroscopic monitoring of the B star HD 6226 resulted in the finding that this object is a new bright Be star with a clear positive correlation between the brightness and emission-line strength. The emission-line episodes are relatively short and seem to repeat frequently which makes this star an ideal target for studying the causes of the Be phenomenon. The general character of the light variations, the low v sin i = 70 km s .61507 over the whole time interval covered by the observations, the velocities of the broad outer wings of the same lines varying in anti-phase and with a lower amplitude. This periodicity could not be found in the radial-velocity variations of the sharp core of Hα. There is some indication of variability on a time scale of 24-29 days but our data are insufficient to prove that conclusively. A comparison of the line spectrum obtained outside emission episodes with synthetic spectra, standard dereddening of UBV magnitudes and Hipparcos parallax all agree with the conclusion that HD 6226 is a star with the following basic properties: T eff = 17 000 K, log g = 3.0 [cgs], mass of 5 M and radius of 11 R . The strong emission-line episodes may appear regularly, in a cycle of 630 days but with different durations of individual cycles. HD 6226 is probably one of the first B stars for which the Be nature was predicted on the basis of the character of its light and colour changes.

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Spectral types of 80 early-type stars of variable radial velocity

Abstract: MK spectral types are given for 80 normal early-type stars of variable radial velocity determined from spectrograms taken with the Lick Observatory 0.9-m refractor during the years 1957-58.

Cited by 10 publications

References 0 publications

An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue

An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue

The heterogeneous class ofλBootis stars

Properties and nature of Be stars

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