HD 207651: A Triple System with Scuti and Ellipsoidal Variations But No Doradus Pulsations

Henry, Gregory W.; Fekel, Francis C.; Henry, Stephen M.

doi:10.1086/381928

Cited by 22 publications

(30 citation statements)

References 18 publications

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“…demonstrated that the observed location of the Doradus variables agrees well with the theoretical instability strip of Warner et al (2003). Since the Doradus and the Scuti instability strips overlap, Henry et al (2004) continued the efforts of Handler & Shobbrook (2002) to find examples of stars pulsating intrinsically with both Doradus and Scuti frequencies. They concluded that the growing number of confirmed Doradus variables that also lie within the Scuti instability strip but do not exhibit additional Scuti variability makes it unlikely that the two types of pulsation can coexist in the same star.…”

Section: Introductionmentioning

confidence: 54%

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Eleven New γ Doradus Stars

2005

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We present new high-dispersion spectroscopic and precise photometric observations to identify 11 new Doradus variables. Seven of these new Doradus stars appear to be single, three are primaries of single-lined binaries, and one has two distant visual companions; none are double-lined or close visual binaries. Several of the stars show spectroscopic line-profile and low-amplitude radial velocity variability indicative of pulsation. All 11 stars are photometrically variable with amplitudes between 8 and 93 mmag in Johnson B and periods between 0.398 and 2.454 days. One star is monoperiodic; the rest have between two and five independent periods. The variability at all periods approximates a sinusoid, although three of the stars exhibit cycle-to-cycle variation in the level of maximum brightness, similar to the Blazhko effect observed in some RR Lyrae stars. We provide a new tabulation of all 54 Doradus stars confirmed to date and list some of their properties. All are dwarfs or subgiants and lie within a well-defined region of the H-R diagram that overlaps the cool edge of the Scuti instability strip. Four of the new Doradus variables from this paper also lie within the Scuti instability strip but do not exhibit the additional higher frequency variability typical of Scuti stars. The variability type of several of these stars given in the General Catalog of Variable Stars and in SIMBAD should now be revised.

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Section: Introductionmentioning

confidence: 54%

“…This work continues a series of papers in which we have examined the spectroscopic and photometric characteristics of candidate Doradus stars (most recently, , 2005Henry et al 2004). Early summaries of this new class of variable stars can be found in Kaye et al (1999a) and .…”

Section: Introductionmentioning

confidence: 62%

Eleven New γ Doradus Stars

2005

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“…In several studies, V1464 Aql was classified as a spectroscopic binary system, RR Lyr (RRc), an eclipsing binary, possibly contact (EC) or semi-detached system (ESD) (Duerbeck 1997;Pourbaix et al 2004;Pribulla & Rucinski 2006; PASA, 30, e016 (2013) doi:10.1017/pasa.2012.016 Aerts et al (2002). c Henry et al (2004). d Chapellier et al (2004).…”

Section: Resultsmentioning

confidence: 99%

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

Dal

Sipahi

2013

Publ. Astron. Soc. Aust.

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Taking into account the results obtained from the models and analyses of the BVRI light curves, we discuss the nature of V1464 Aql. The analyses indicated that the mass ratio of the system is q = 0.71 ± 0.02, while the inclination of the system (i) is 38°.45 ± 0°.22. Taking the primary component's temperature as 7 420 ± 192 K, we found that the temperature of the secondary is 6 232 ± 161 K. The mass of the primary component was found to be 1.74 ± 0.05 M ࣻ , while it is 1.23 ± 0.01 M ࣻ for the secondary. The primary component's radius was found to be 2.10 ± 0.05 R ࣻ , while it was found as 1.80 ± 0.01 R ࣻ for the secondary. Revealing that the system should not exhibit any eclipses, we demonstrated that the main variation with large amplitude should be caused due to the ellipsoidal effect. Indeed, the Fourier analysis also supported the result. For the first time in the literature, we revealed that the primary component is a δ Scuti star. The period of pulsation was found to be 58.482 ± 0.002, 58.482 ± 0.001, 60.966 ± 0.002, and 60.964 ± 0.003 min in BVRI bands, respectively. We plotted V1464 Aql in the log(P orb )-log (P pulse ) plane. Using more than 160 binaries, whose one or both components are pulsating, we derived a new linear fit in the log (P orb )-log (P pulse ) plane for each type of binary. Using the linear fit of each group, we obtained new calibrations between log (P orb ) and log (P pulse ) for different types of pulsating stars. In addition, a calibration has been obtained for the first time for the pulsating stars with spectral types O and B. V1464 Aql seems to be located near the other ellipsoidal and close binaries. Thus, we listed V1464 Aql as a new candidate for the ellipsoidal variables with a δ Scuti component.

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“…But Henry et al (2004) found that a long-term period component of HD 207651, 1.3598 cycle day À1 = 0.73540 days, did not result from a Doradus type term but from the ellipticity effect. From the spectroscopic observations an eclipsing period was twice the long-term period seen in the photometry.…”

Section: Singg Le-radial Mode Sx Phoenicis Stars With Longg -Term Varmentioning

confidence: 93%

SX Phoenicis Stars in the Globular Cluster NGC 5466

Jeon

Lee

2004

Astron J

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Through time-series CCD photometry of the globular cluster NGC 5466, we have detected nine SX Phoenicis stars, including three new ones. All the SX Phoenicis stars are located in the blue straggler region in the colormagnitude diagram of NGC 5466. Five of them clearly show double-radial mode features, the periods of which are consistent with the theoretical ratio of the first-overtone mode to the fundamental mode (P 1H /P F ). Normally, it has not been easy to secure a P-L relation for the SX Phoenicis stars because their pulsational mode has been difficult to determine. The existence of five SX Phoenicis stars in NGC 5466 with double-radial modes allows us to reliably derive a P-L relation for the fundamental mode of SX Phoenicis stars. Using seven SX Phoenicis stars, including fiincluding fi ve stars with double-radial modes, we derive a P-L relation for the fundamental mode in NGC 5466, hV i ¼ À3:25(AE0:46) log P þ 14:70(AE0:06); ( ¼ AE0:04), corresponding to hM V i ¼ À3:25(AE0:46) log P À 1:30(AE0:06) for an adopted distance modulus of (m À M ) 0 ¼ 16:00 and zero reddening.

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HD 207651: A Triple System with Scuti and Ellipsoidal Variations But No Doradus Pulsations

Cited by 22 publications

References 18 publications

Eleven New γ Doradus Stars

Eleven New γ Doradus Stars

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

SX Phoenicis Stars in the Globular Cluster NGC 5466

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