Multiband photometric re-classification of ROTSE-I<i>δ</i>Scuti type stars

Jin, Ho; Kim, S.-L.; Kwon, S. G.; Youn, Jae-Hyuck; Lee, C.-U.; Lee, D.-J.; Kim, Kyoung-Sook

doi:10.1051/0004-6361:20030500

Cited by 18 publications

(4 citation statements)

References 13 publications

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“…Secondly, we combined the newly determined times of maximum light with those provided by earlier studies (Eggen 1955;Broglia & Masani 1957;Spinrad 1959;Broglia 1961;Heiser & Hardie 1964;Fitch et al 1966;Gieren et al 1974;Langford 1976;Szeidl & Mahdy 1981;Joner & McNamara 1983;Jiang 1985;Peniche et al 1985;Hamdy et al 1986;Kim & Joner 1994;Agerer et al 1999;Agerer & Hubscher 2000Derekas et al 2003;Jin et al 2003;Hubscher 2005;Hubscher et al 2006;Klingenberg et al 2006;Zhou 2006;Ward et al 2008).…”

Section: Times Of Maximum Light and O − C Diagramunclassified

Pulsations of the High-AmplitudeδScuti star YZ Bootis

Yang

Esamdin

et al. 2018

Res. Astron. Astrophys.

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We present a study on the pulsations of the high-amplitude δ Scuti star YZ Boo based on photometric observations in Johnson V and R bands with both the Nanshan 1-m telescope of Xinjiang Astronomical Observatory (XAO) and the Xinglong 85-cm telescope of National Astronomical Observatories, Chinese Academy of Sciences (NAOC). The Fourier analysis of the light curves reveals the fundamental radial mode and its five harmonics, with the fourth and the fifth newly detected. 39 new times of light maximum are determined from the light curves, and combined with those in the literature, we construct the O−C diagram and derive a new ephemeris and the determination of a new value of the updated period 0.104091579(2). Besides, the O − C diagram reveals an increasing period change rate of YZ Boo. Theoretical models are calculated and constrained with the observationally determined parameters of YZ Boo. The mass and age of YZ Boo are hence derived as M = 1.61 ± 0.05 M ⊙ and age = (1.44 ± 0.14) × 10 9 yr, respectively. With both the frequency of the fundamental radial mode and the period change rate, YZ Boo is located at the post-main-sequence stage.

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Section: Times Of Maximum Light and O − C Diagramunclassified

Pulsations of the High-AmplitudeδScuti star YZ Bootis

Yang

Esamdin

et al. 2018

Res. Astron. Astrophys.

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“…V2367 Cyg (KIC 9408694) was discovered in a ROTSE survey (Akerlof et al 2000) and confirmed as a HADS star by Jin et al (2003) and Pigulski et al (2009). The star was included in the Kepler commissioning run (Quarter 0 = Q0) and data were obtained for a duration of 9.73 d with continuous short‐cadence (SC) 1‐min exposures.…”

Section: Introductionmentioning

confidence: 97%

Kepler observations of the high-amplitude δ Scuti star V2367 Cyg

Balona

Lenz

Antoci

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We analyse Kepler observations of the high‐amplitude δ Scuti (HADS) star V2367 Cyg (KIC 9408694). The variations are dominated by a mode with frequency f1= 5.6611 d−1. Two other independent modes with f2= 7.1490 d−1 and f3= 7.7756 d−1 have amplitudes an order of magnitude smaller than f1. Nearly all the light variation is due to these three modes and their combination frequencies, but several hundred other frequencies of very low amplitude are also present. The amplitudes of the principal modes may vary slightly with time. The star has twice the projected rotational velocity of any other HADS star, which makes it unusual. We find a correlation between the phases of the combination frequencies and their pulsation frequencies, which is not understood. Since modes of highest amplitude in HADS stars are normally radial modes, we assumed that this would also be true in this star. However, attempts to model the observed frequencies as radial modes without mode interaction were not successful. For a star with such a relatively high rotational velocity, it is important to consider the effect of mode interaction. Indeed, when this was done, we were able to obtain a model in which a good match with f1 and f2 is obtained, with f1 being the fundamental radial mode.

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“…Thus, it is very difficult to identify the accurate type of variable stars based only on their single filter light curves. Hence at least two filters should be employed to see the change of the amplitude at different wavelength bands for accurate classification (Jin et al 2003(Jin et al , 2004.…”

Section: Detection and Classification Of Vari-able Starsmentioning

confidence: 99%

Detection of Variable Stars in the Open Cluster M11 Using Difference Image Analysis Pipeline

Lee¹,

Koo²,

Lee³

et al. 2010

Journal of Astronomy and Space Sciences

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We developed a photometric pipeline to be used for a wide field survey. This pipeline employs the difference image analysis (DIA) method appropriate for the photometry of star dense field such as the Galactic bulge. To verify the performance of pipeline, the observed dataset of the open cluster M11 was re-processed. One hundred seventy eight variable stars were newly discovered by analyzing the light curves of which photometric accuracy was improved through the DIA. The total number of variable stars in the M11 observation region is 335, including 157 variable stars discovered by previous studies. We present the catalogue and light curves for the 178 variable stars. This study shows that the photometric pipeline using the DIA is very useful in the detection of variable stars in a cluster.

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Multiband photometric re-classification of ROTSE-IδScuti type stars

Cited by 18 publications

References 13 publications

Pulsations of the High-AmplitudeδScuti star YZ Bootis

Pulsations of the High-AmplitudeδScuti star YZ Bootis

Kepler observations of the high-amplitude δ Scuti star V2367 Cyg

Detection of Variable Stars in the Open Cluster M11 Using Difference Image Analysis Pipeline

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