Physical properties and catalog of EW-type eclipsing binaries observed by LAMOST

Qian, S.‐B.; He, J.-J.; Zhang, Jia; Zhu, L.-Y.; Shi, Xiang-Dong; Zhao, En-Guang; Xiao, Zhi Yu

doi:10.1088/1674-4527/17/8/87

Cited by 139 publications

(139 citation statements)

References 41 publications

Supporting

Mentioning

130

Contrasting

Order By: Relevance

“…No high resolution classification spectrum is available for IL Cnc, however an estimate from (B-V ) and (V-I C ) color indices generated from the new LCs herein and those reported by four other surveys (USNO-B1, 2MASS, SDSS-DR9 and UCAC4) cataloged in VizieR (Lasker et al 1996) suggests that it is an early K type system. This assignment is supported by a recent publication (Qian et al 2017) in which low resolution (R ≈ 1800) spectra were obtained from over 7900 stars; therein IL Cnc is classified as a main sequence K3 system. Nonetheless, additional high resolution spectroscopic data may be required to unequivocally classify this system.…”

supporting

confidence: 61%

See 1 more Smart Citation

Multicolor light curves and Period Analysis of IL Cnc

Alton¹

2018

IBVS

View full text Add to dashboard Cite

The spectral type and orbital period were estimated from multicolor (B, V and Ic) Rinner et al. (2003) based on unfiltered ccd data. Photometric data were also collected from this system during the ROTSE-I survey (NSVS; Woźniak et al. 2004) and later captured by the ASAS Survey (Pojmański et al. 2005). Sparsely sampled light curve data acquired over the time span between 1999 and 2005 were folded by period analysis. This report describes the results from the first multicolor (BVI C ) ccd-based photometric study conducted on this variable target. The analysis of eclipse time differences (ETD) calculated from times-of-minima published in the literature and new data presented herein has resulted in an improved ephemeris for IL Cnc.Time-series images were taken (90-sec) in 2014 with an SBIG ST-8XME CCD camera mounted at the Cassegrain focus of a 0.28-m catadioptric telescope. This f/6.4 instrument located in UnderOak Observatory (UO; NJ, USA) produces an image scale of 2.06 ′′ /px (bin=2×2) and a field-of-view (FOV) of 17.5 ′ ×26.3 ′ . Image acquisition (raw lights, darks, and flats) at UO was performed as described elsewhere (Alton 2016) and produced at least 282 values in each bandpass (B,V and I C ). Similarly at Desert Bloom Observatory (DBO; AZ, USA), an SBIG STT-1603ME CCD camera mounted at the Cassegrain focus of a 0.4-m catadioptric telescope was used for imaging IL Cnc in 2018. This f/6.8 instrument produces an image scale of 1.36 ′′ /px (bin=2×2) and a FOV of 11.5 ′ ×17.2 ′ . At DBO, image acquisition (75-sec) was performed using MaxIm DL Version 6.13 (Diffraction Limited) or TheSkyX Pro Version 10.5.0 (Software Bisque). This most recent imaging campaign produced at least 235 individual photometric values in each bandpass. Both ccd cameras were equipped with B, V and I C filters manufactured to match the Johnson-Cousins-Bessell prescription. Calibration and registration of all images collected at UO and DBO were performed with AIP4Win v2.4.0 (Berry and Burnell 2005). Instrumental readings were reduced to catalog-based magnitudes using the reference MPOSC3 star fields (Warner 2007) built into MPO Canopus v10.7.1.3 (Minor Planet Observer). The 2014 and 2018 light curves (LC) used an identical ensemble of five non-varying comparison stars in the same FOV. The identity, J2000 coordinates and color index (B − V ) of these stars are listed in Table 1. Only data from images taken above 30• altitude (airmass <2.0) were accepted in order to minimize error due to differential refraction and color extinction.

show abstract

supporting

confidence: 61%

“…Photometric data were also collected from this system during the ROTSE-I survey (NSVS; Woźniak et al 2004) and later captured by the ASAS Survey (Pojmański et al 2005). Sparsely sampled light curve data acquired over the time span between 1999 and 2005 were folded by period analysis.…”

mentioning

confidence: 99%

Multicolor light curves and Period Analysis of IL Cnc

Alton¹

2018

IBVS

View full text Add to dashboard Cite

show abstract

“…However, we have not detected third light (l 3 ) through photometric analysis, which implies that the tertiary may be a compact object such as a white dwarf or a neutron star. Qian et al (2017 proposed that a compact tertiary component may even contaminate the inner binary during the early evolutionary stage of a multiple star system, which can explain the formation of a contact binary with a very high metallicity.…”

Section: Discussionmentioning

confidence: 99%

The W-subtype active contact binary PZ UMa with a possible more massive tertiary component

Xiao

Soonthornthum

2019

Publications of the Astronomical Society of Japan

Self Cite

View full text Add to dashboard Cite

Two sets of multiple-color (B, V, R c , I c ) light curves of PZ UMa were observed in dependently with the 2.4 meter telescope at the Thai National Observatory and the 1 meter telescope at Yunnan Observatories. The light curves were analyzed with the Wilson-Devinney program and the two sets of light curves produced consistent results, which show that PZ UMa is a W-subtype contact binary with an extreme mass ratio (M 1 /M 2 = 0.18). The basic physical parameters of PZ UMa were determined to beThe orbital period analysis of PZ UMa revealed a 13.22 year periodicity, which implies that there may be a tertiary component orbiting around the binary system. The mass and orbital radius of the tertiary component were calculated to be M 3 = 0.88M ⊙ and a 3 = 3.67AU, if the orbit was coplanar with the central binary system. It is interesting that the minimum mass of the tertiary was calculated to be M 3min = 0.84M ⊙ , which means the tertiary component is even larger than the primary star and the secondary one of PZ UMa. PZ UMa is a late-type contact binary with stellar activity. The O'Connell effect appeared on its light curves when it was observed on April 2016. However, the O'Connell effect reversed when the target was observed again on December 2016. The changes of the O'Connell effect in such a short time-scale strongly support the occurrence of rapidly changing magnetic activity on this W UMa binary.

show abstract

“…The following were the adjustable parameters: the orbital inclination, i; the mean effective temperature of star 2, T 2 ; the monochromatic luminosity of star 1 in each band, L 1 and the dimensionless potential of star 1, Ω 1 . According to the LAMOST data, the effective temperature of primary component was adopted to be T 1 =6180 K (Qian et al 2017). From Figure 1, we could find out that the new determined light curves are EW-type light curves; these two minimums are nearly symmetric and no spotted solution is needed.…”

Section: Light Curve Analysis Using the W-d Codementioning

confidence: 99%

First Photometric Investigation of the Neglected EW-type Binary System V502 Her

Zhao¹,

Qian²,

Liao³

et al. 2018

PASP

View full text Add to dashboard Cite

V502 Her is a neglected EW-type binary, which has been known for more than 60 years. The first multi-color CCD photometric light curve and spectroscopic observations of contact binary V502 Her was obtained. Based on the LAMOST data, its spectrum can be found to be F5. Together with solutions of light curves by using the Wilson-Devinney code, it infers that V502 Her is an A-type W UMa contact binary system with the mass ratio of q=0.313 and the filling factor of f=38.1%. According to all minimum times from the literature and our observations, the orbital period was analyzed and a long-term increase with a periodic change (P 3 = 26.8 years) was computed. The orbital period increase may be caused by the mass transfer from a less-massive component to the more massive one, which indicates that V502 Her is in the thermal relaxation oscillation (TRO) controller stage, while the light-travel time effect (LTTE) through the presence of a cool third body may lead to the periodic variation.

show abstract

Physical properties and catalog of EW-type eclipsing binaries observed by LAMOST

Cited by 139 publications

References 41 publications

Multicolor light curves and Period Analysis of IL Cnc

Multicolor light curves and Period Analysis of IL Cnc

The W-subtype active contact binary PZ UMa with a possible more massive tertiary component

First Photometric Investigation of the Neglected EW-type Binary System V502 Her

Contact Info

Product

Resources

About