2005
DOI: 10.1086/427713
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Chromospherically Active Stars. XXIV. The Giant, Single-lined Binaries HD 37824, HD 181809, and HD 217188

Abstract: We have obtained spectroscopy and photometry of three chromospherically active, single-lined spectroscopic binaries, HD 37824 (V1149 Ori), HD 181809 (V4138 Sgr), and HD 217188 (AZ Psc). HD 37824 has a circular orbit with a period of 53.57 days. Its primary is a K0 III star, while the secondary is likely a G or K dwarf. HD 181809 has an orbit with a period of 13.04667 days and a low eccentricity of 0.040. The primary has a spectral type of K0 III-IV, and its secondary is probably an M dwarf. The orbit of HD 217… Show more

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Cited by 30 publications
(33 citation statements)
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“…V1149 Ori has an orbital period of P orb = 53.57465 d (Fekel et al 1987) and a variable rotational photometric period with a mean value of P pho = 53.12 d (Fekel & Henry 2005). If granted the spectral classification by Cutispoto (1995), the observed photometric variability can be completely attributed to the giant component.…”
Section: V1149 Ori (Hd 37824)mentioning
confidence: 98%
“…V1149 Ori has an orbital period of P orb = 53.57465 d (Fekel et al 1987) and a variable rotational photometric period with a mean value of P pho = 53.12 d (Fekel & Henry 2005). If granted the spectral classification by Cutispoto (1995), the observed photometric variability can be completely attributed to the giant component.…”
Section: V1149 Ori (Hd 37824)mentioning
confidence: 98%
“…Fekel & Henry 2005, P orb , t 0 , e, Sp-type of component A). Note the MLC dip at about f orb =0.75 in Figures 6(c), (e), and (g), which will be discussed later in Section 6.1.4.…”
Section: Mlc Of V711 Taumentioning
confidence: 99%
“…1b: filled circles). More detailed information of the operation of the T3 0.4 m APT and the data reduction procedures can be found, e.g., in Henry (1999) and Fekel & Henry (2005).…”
Section: Observationsmentioning
confidence: 99%