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Claret, A.; Dzitko, H.; Engelmann, J.; Starck, Jean-Luc

doi:10.1023/a:1008080015656

Cited by 9 publications

(7 citation statements)

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“…Our photometric solutions suggest that the coverage of cool starspots on the surface of the secondary component is about 5% (2010) and 11% (2011). Usually, late-type stars with a deeper convective envelope and faster rotation will, in turn, produce a strong magnetic field (Claret. 2000;Zhang et al 2014).…”

Section: Discussionmentioning

confidence: 99%

“…The possible effective temperature for the primary component (star 1), T 1 = 4290 K, was fixed according to aver-age color index. The same value of gravity-darkening coefficients is taken, i.e., g 1 = g 2 = 0.32 (Claret 2000), and the bolometric albedos for both components were set as A 1 = A 2 = 0.5 (Ruciński 1969). The orbital eccentricity e = 0, since when the orbital period is less than 1 day, close binary orbits become circularized (Zahn 1989).…”

Section: Photometric Solutions With W-d Programmentioning

confidence: 99%

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NSVS 01286630: a detached binary with a close-in companion

Zhang

Qian

Liao

et al. 2018

Res. Astron. Astrophys.

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New photometric observations of NSVS 01286630 were performed and two sets of four-color (B, V , R c , I c ) light curves (LCs) were obtained. Using the 2013 version of the Wilson-Devinney (W − D) code, we analyzed these data. The photometric solutions reveal that NSVS 01286630 is an active detached eclipsing binary (EB) with a high orbit inclination(nearly 90 • ). Remarkably, the temperature of the primary component (the hotter star) is higher than the secondary one, but, the value of mass ratio q( M2 M1 ) for NSVS 0128663 is more than 1, which can be explained that the surface of the secondary component of NSVS 01286630is covered with big cool-star-spots. Based on our new CCD mid-eclipse times and the data published until now, the variations of the mid-eclipse times were reanalyzed in detail using a weighted least-squares method. It is discovered that the (O − C) diagram of the system shows a cyclic oscillation with a period of 3.61 yr and an amplitude of 0.001 days. The cyclic variation may be caused by the light travel time effect (LTTE) due to the presence of a third companion, whose mass we calculated is M 3 sin(i 3 )=0.11 M ⊙ . The third body may affect the orbital evolution of the central binary system by transferring the angular momentum.

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Section: Discussionmentioning

confidence: 99%

Section: Photometric Solutions With W-d Programmentioning

confidence: 99%

NSVS 01286630: a detached binary with a close-in companion

Zhang

Qian

Liao

et al. 2018

Res. Astron. Astrophys.

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“…For glitches producing single fast increases and decreases of the signal, a simple median filtering produces a fairly good deglitching. The ISOCAM glitch rate is one per second, and each glitch on average has an impact on eight pixels (Claret et al 1999). However, 5 to 20% of the total number of readouts, depending on the integration time and the strength of the selection criterion, are affected by memory effects, which can produce false detections.…”

Section: A Brief Discussion Of the Problemmentioning

confidence: 99%

Faint source detection in ISOCAM images

Starck

Aussel

Elbaz

et al. 1999

Astron. Astrophys. Suppl. Ser.

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Abstract. We present a tool adapted to the detection of faint mid-infrared sources within ISOCAM mosaics. This tool is based on a wavelet analysis which allows us to discriminate sources from cosmic ray impacts at the very limit of the instrument, four orders of magnitudes below IRAS. It is called PRETI for Pattern REcognition Technique for ISOCAM data, because glitches with transient behaviors are isolated in the wavelet space, i.e. frequency space, where they present peculiar signatures in the form of patterns automatically identified and then reconstructed. We have tested PRETI with Monte-Carlo simulations of fake ISOCAM data. These simulations allowed us to define the fraction of remaining false sources due to cosmic rays, the sensitivity and completeness limits as well as the photometric accuracy as a function of the observation parameters.Although the main scientific applications of this technique have appeared or will appear in separated papers, we present here an application to the ISOCAM-Hubble Deep Field image. This work completes and confirms the results already published .

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“…The light curves are modeled based on the small planet approximation and a four-coefficient limb-darkening law is used (Mandel & Agol 2002). The four limb-darkening coefficients are derived through interpolation of the coefficient tables of Claret (2000Claret ( , 2004. The best fitting values and uncertainties are inferred from the posterior probability distributions of the system parameters.…”

Section: The Stellar Parameters Of Wasp-32mentioning

confidence: 99%

Long-term transit timing monitoring and homogenous study of WASP-32

Sun

Wang

et al. 2015

Res. Astron. Astrophys.

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We report new photometric observations of the transiting exoplanetary system WASP-32 made by using CCD cameras at Yunnan Observatories and Ho Koon Nature Education cum Astronomical Centre, China from 2010 to 2012. Following our usual procedure, the observed data are corrected for systematic errors according to the coarse decorrelation and SYSREM algorithms so as to enhance the signal of the transit events. Combined with radial velocity data presented in the literature, our newly observed data and earlier photometric data in the literature are simultaneously analyzed to derive the physical parameters describing the system by employing the Markov chain Monte Carlo technique. The derived parameters are consistent with the result published in the original paper about WASP-32b, but the uncertainties of the new parameters are smaller than those in the original paper. Moreover, our modeling result supports a circular orbit for WASP-32b. Through the analysis of all available mid-transit times, we have refined the orbital period of WASP-32b; no evident transit timing variation is found in these transit events.

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Cited by 9 publications

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NSVS 01286630: a detached binary with a close-in companion

NSVS 01286630: a detached binary with a close-in companion

Faint source detection in ISOCAM images

Long-term transit timing monitoring and homogenous study of WASP-32

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