Disentangling component spectra of , a spectroscopic binary with a pulsating primary

Uytterhoeven, K.; Briquet, Maryline; Aerts, C.; Telting, J. H.; Harmanec, P.; Lefever, K.; Cuypers, J.

doi:10.1051/0004-6361:20041444

Cited by 32 publications

(28 citation statements)

References 38 publications

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“…However, its photometric amplitudes with respect to wavelength (Table 1) are also consistent with pulsation. On the other hand, the frequency reported by Uytterhoeven et al (2005) is somewhat lower than the one detected in our and the space photometry. In fact, it corresponds to one of the aliases (0.244 d −1 ) mentioned before.…”

Section: κ Scocontrasting

confidence: 88%

“…The dominant pulsation mode of the primary component has been spectroscopically identified as either (l, m) = (2, −1) or (1, −1) (Uytterhoeven et al 2005). Our results point towards the latter possibility, which is also more Fig.…”

Section: κ Scosupporting

confidence: 60%

“…Uytterhoeven et al (2005) spectroscopically determined Notes. The formal errors on the frequencies are ±0.001 d −1 ; on the amplitudes they are ±0.5 mmag in v and y and ±0.6 mmag in u.…”

Section: κ Scomentioning

confidence: 99%

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Time-resolved multicolour photometry of bright B-type variable stars in Scorpius

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Schwarzenberg‐Czerny

2013

A&A

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Context. The first two of a total of six nano-satellites that will constitute the BRITE-Constellation space photometry mission have recently been launched successfully. Aims. In preparation for this project, we carried out time-resolved colour photometry in a field that is an excellent candidate for BRITE measurements from space. Methods. We acquired 117 h of Strömgren uvy data during 19 nights. Our targets comprised the β Cephei stars κ and λ Sco, the eclipsing binary μ 1 Sco, and the variable super/hypergiant ζ 1 Sco. Results. For κ Sco, a photometric mode identification in combination with results from the spectroscopic literature suggests a dominant (l, m) = (1, −1) β Cephei-type pulsation mode of the primary star. The longer period of the star may be a rotational variation or a g-mode pulsation. For λ Sco, we recover the known dominant β Cephei pulsation, a longer-period variation, and observed part of an eclipse. Lack of ultraviolet data precludes mode identification for this star. We noticed that the spectroscopic orbital ephemeris of the closer pair in this triple system is inconsistent with eclipse timings and propose a refined value for the orbital period of the closer pair of 5.95189 ± 0.00003 d. We also argue that the components of the λ Sco system are some 30% more massive than previously thought. The binary light curve solution of μ 1 Sco requires inclusion of the irradiation effect to explain the u light curve, and the system could show additional low amplitude variations on top of the orbital light changes. ζ 1 Sco shows long-term variability on a time scale of at least two weeks that we prefer to interpret in terms of a variable wind or strange mode pulsations.

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Section: κ Scocontrasting

confidence: 88%

Section: κ Scosupporting

confidence: 60%

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Time-resolved multicolour photometry of bright B-type variable stars in Scorpius

Handler

Schwarzenberg‐Czerny

2013

A&A

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“…The star rotates at about half its critical velocity and shows clear evidence of rotational modulation in addition to its pulsational variability in both the photometry and the spectroscopy. The list of B-type stars with a detected mixture of rotational and pulsational variability with similar frequencies and amplitudes is growing and occurs across all effective temperatures of this spectral type (e.g., Uytterhoeven et al 2005;Degroote et al 2011;Thoul et al 2012). This is not surprising given the co-existence of chemically peculiar Bp and SPB stars in the same part of the HR diagram (e.g., Briquet et al 2007).…”

Section: Discussionmentioning

confidence: 99%

Gravito-inertial and pressure modes detected in the B3 IV CoRoT target HD 43317

Pápics

Briquet

Baglin

et al. 2012

A&A

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115

146

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Context. OB stars are important building blocks of the Universe, but we have only a limited sample of them well understood enough from an asteroseismological point of view to provide feedback on the current evolutionary models. Our study adds one special case to this sample, with more observational constraints than for most of these stars. Aims. Our goal is to analyse and interpret the pulsational behaviour of the B3 IV star HD 43317 using the CoRoT light curve along with the ground-based spectroscopy gathered by the HARPS instrument. This way we continue our efforts to map the β Cep and SPB instability strips. Methods. We used different techniques to reveal the abundances and fundamental stellar parameters from the newly-obtained highresolution spectra. We used various time-series analysis tools to explore the nature of variations present in the light curve. We calculated the moments and used the pixel-by-pixel method to look for line profile variations in the high-resolution spectra. Results. We find that HD 43317 is a single fast rotator (v rot ≈ 50% v crit ) and hybrid SPB/β Cep-type pulsator with Solar metal abundances. We interpret the variations in photometry and spectroscopy as a result of rotational modulation connected to surface inhomogeneities, combined with the presence of both g and p mode pulsations. We detect a series of ten consecutive frequencies with an almost constant period spacing of 6339 s as well as a second shorter sequence consisting of seven frequencies with a spacing of 6380 s. The dominant frequencies fall in the regime of gravito-inertial modes.

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“…Per see Harmanec 1999, κ Sco see Uytterhoeven et al 2005a) that the bump-like LPV are due to stellar-surface structure with magnetic origin. Whereas there is much indirect evidence for the presence of magnetic fields in some massive early-type stars (see e.g.…”

Section: Origin Of the Observed Lpvmentioning

confidence: 98%

A high-resolution spectroscopy survey ofβ Cephei pulsations in bright stars

Telting¹,

Schrijvers

Ilyin

et al. 2006

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We present a study of absorption line-profile variations in early-B type near-main-sequence stars without emission lines. We have surveyed a total of 171 bright stars using the Nordic Optical Telescope (NOTSA), William Herschel Telescope (ING) and Coudé Auxiliary Telescope (ESO). Our sample contains 75% of all O9.5−B2.5 III-V non-emission-line stars brighter than 5.5 mag. We obtained high signal-to-noise, high-resolution spectra of the SiIII λ4560 triplet -for 125 stars of our sample we obtained more than one spectrum -and examined these for pulsational-like line-profile variations and/or structure. We conclude that about half of our sample stars show evidence for line-profile variations (LPV). We find evidence for LPV in about 65% of our sample stars brighter than V = 5.5. For stars with rotational broadening V sin i ∼ 100 km s −1 , we find evidence for LPV in about 75% of the cases. We argue that it is likely that these LPV are of pulsational origin, and that hence more than half of the solar-neighbourhood O9.5-B2.5 III−V stars is pulsating in modes that can be detected with high-resolution spectroscopy. We detected LPV in 64 stars previously unknown to be pulsators, and label these stars as new β Cep candidates. We conclude that there is no obvious difference in incidence of (pulsational) LPV for early-B type near-main-sequence stars in binaries or in OB associations, with respect to single field stars.

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Disentangling component spectra of , a spectroscopic binary with a pulsating primary

Cited by 32 publications

References 38 publications

Time-resolved multicolour photometry of bright B-type variable stars in Scorpius

Time-resolved multicolour photometry of bright B-type variable stars in Scorpius

Gravito-inertial and pressure modes detected in the B3 IV CoRoT target HD 43317

A high-resolution spectroscopy survey ofβ Cephei pulsations in bright stars

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