2017
DOI: 10.1051/0004-6361/201629897
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First observation of Hα redshifted emission in RR Lyr

Abstract: Context. The so-called Hα third emission occurs around pulsation phase ϕ = 0.30. It has been observed for the first time in 2011 in some RR Lyrae stars. The emission intensity is very weak, and its profile is a tiny persistent hump in the red side-line profile. Aims. We report the first observation of the Hα third emission in RR Lyr itself (HD 182989), the brightest RR Lyrae star in the sky. Methods. New spectra were collected in 2013−2014 with the AURELIE spectrograph (resolving power R = 22 700, T152, Observ… Show more

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Cited by 10 publications
(20 citation statements)
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“…The maximum intensity of the Hα third emission should correspond to the maximum of the compression. For our observations made during the night of 2014-09-14 (Gillet et al 2017), the maximum compression probably occurs around the pulsation phase ϕ = 0.357. Thus, the most intense part of the compression occurs after the beginning of the infalling motion of the sodium layer.…”
Section: Phase 5 (0320-0455): a Two-step Infalling Motionmentioning
confidence: 62%
See 3 more Smart Citations
“…The maximum intensity of the Hα third emission should correspond to the maximum of the compression. For our observations made during the night of 2014-09-14 (Gillet et al 2017), the maximum compression probably occurs around the pulsation phase ϕ = 0.357. Thus, the most intense part of the compression occurs after the beginning of the infalling motion of the sodium layer.…”
Section: Phase 5 (0320-0455): a Two-step Infalling Motionmentioning
confidence: 62%
“…The maximum velocity of the shock is variable from one Blazhko maximum to another. For example, by August 13, 2014, the Hα profile was observed (Gillet et al 2017) very close to a Blazhko maximum (ψ = 0.04). It shows that the shock velocity decreases rapidly from 156 km s −1 at ϕ = 0.903 to 101 km s −1 at ϕ = 0.941.…”
Section: Shock Wave Velocity Evolutionmentioning
confidence: 96%
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“…The first, dubbed the "third apparition" (Preston 2011), is identified by a weak red-shifted Hα emission wing visible during about one third of the pulsation cycle following maximum light. Ad hoc explanations of this apparition have been advanced by Chadid & Preston (2013) and Gillet et al (2017Gillet et al ( , 2019. A second shock, identified by violet-shifted Hα emission during the "bump" preceding minimum light (Gillet & Crowe 1988), is discussed at length in the foregoing references.…”
Section: Introductionmentioning
confidence: 99%