Properties and nature of Be stars

Koubský, P.; Hummel, C. A.; Harmanec, P.; Tycner, C.; Leeuwen, F. van; Yang, S.; Šlechta, M.; Božić, H.; Zavala, R. T.; Ruždjak, Domagoj; Sudar, D.

doi:10.1051/0004-6361/201014477

Cited by 16 publications

(20 citation statements)

References 32 publications

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“…Notes on Individual Stars HD 4180. Koubský et al (2010) present a single-lined spectroscopic orbit for HD 4180 plus interferometric observations from NPOI of the resolved system A,B. The components of this binary system are too close for speckle resolution, and the object appeared single in observations by Mason et al (1997).…”

Section: Facilities: Chara Arraymentioning

confidence: 93%

“…The components of this binary system are too close for speckle resolution, and the object appeared single in observations by Mason et al (1997). Grundstrom (2007) observed spectral features corresponding to two similar late-B or early-A stars that showed Doppler shifts on a timescale of approximately 4 days, and these probably form in the close (Ba, Bb) system that was suspected by Koubský et al (2010). We have estimated the K-band magnitude difference using the magnitude difference from NPOI △R = 2.9 mag , the estimated spectral types from Koubský et al (2010), the near-IR color calibration from Wegner (1994), and the flux excess E ⋆ (V ⋆ − K) = 0.13 mag from Touhami et al (2011).…”

Section: Facilities: Chara Arraymentioning

confidence: 99%

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A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS

Touhami

Gies

Schaefer

et al. 2013

ApJ

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We report on a high angular resolution survey of circumstellar disks around 24 northern sky Be stars. The K-band continuum survey was made using the CHARA Array long baseline interferometer (baselines of 30 -331 m). The interferometric visibilities were corrected for the flux contribution of stellar companions in those cases where the Be star is a member of a known binary or multiple system. For those targets with good (u, v) coverage, we used a four-parameter Gaussian elliptical disk model to fit the visibilities and to determine the axial ratio, position angle, K-band photospheric flux contribution, and angular diameter of the disk's major axis. For the other targets with relatively limited (u, v) coverage, we constrained the axial ratio, inclination angle, and/or disk position

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Section: Facilities: Chara Arraymentioning

confidence: 93%

Section: Facilities: Chara Arraymentioning

confidence: 99%

A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS

Touhami

Gies

Schaefer

et al. 2013

ApJ

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“…This method works very well for objects with symmetrical profiles (see e.g. Božić et al 1996;Koubský et al 2010;or Nemravová et al 2012). The basic reasons that the measurements of strong Hα emission should give the most realistic estimate of the radial velocity of a Be primary can be found in Ruždjak et al (2009).…”

Section: Spectroscopic Observations and Their Reductionsmentioning

confidence: 97%

o Puppis: another Be+sdO binary?

Koubský

Kotková

Votruba

et al. 2012

A&A

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The spectrum of the Be star o Pup is shown to vary periodically with a period of 28.9 days. A radial-velocity variable He i 6678 Å emission component suggests that the star is the same type as φ Per, 59 Cyg, and FY CMa, i.e. binaries consisting of a Be star and a hot companion that illuminates the Be star disk (also called φ Per-type binaries or Be+sdO binaries). The range of radial-velocity variations of the stronger emission component in the helium line observed in o Pup is about 270 km s −1 , a value in good agreement with the range derived for φ Per-type binaries. The radial velocity curves defined by the prominent emission peak in He i 6678 Å line and Hα + Paschen emission move in anti-phase. We suggest that o Pup is generically similar to φ Per-type systems and may represent the fourth case of a Be star with a hot subdwarf companion.

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“…The NPOI is a six-element optical long-baseline interferometer that has been described in detail by Armstrong et al (1998). The interferometric observations obtained during our δ Sco campaign have utilized all six operational stations resulting in baseline lengths from 18 to 80 m. The raw interferometric data were obtained and reduced using steps outlined in Hummel et al (2003), Benson et al (2003), and Koubský et al (2010). The calibrator star used was ζ Oph (HR 6175, O9V) with an estimated diameter of 0.85 mas based on the R − I color (Mozurkewich et al 1991).…”

Section: Observations and Reductionsmentioning

confidence: 99%

THE REVISED ORBIT OF THE δ Sco SYSTEM

Tycner¹,

Ames²,

Zavala³

et al. 2011

ApJ

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In anticipation of the possible collision between a circumstellar disk and the secondary star in the highly eccentric binary system δ Scorpii, high angular resolution interferometric observations have been acquired aimed at revising the binary parameters. The Navy Prototype Optical Interferometer (NPOI) was used to spatially resolve the binary components in 2000 and over a period between 2005 and 2010. The interferometric observations are used to obtain the angular separations and orientations of the two stellar components at all epochs for which data has been obtained, including 2005 and 2006, for which based on previous studies there was some uncertainty as to if the signature of binarity can be clearly detected. The results of this study represent the most complete and accurate coverage of the binary orbit of this system to date and allow for the revised timing of the upcoming periastron passage that will occur in 2011 to be obtained.

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Properties and nature of Be stars

Cited by 16 publications

References 32 publications

A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS

A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS

o Puppis: another Be+sdO binary?

THE REVISED ORBIT OF THE δ Sco SYSTEM

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