- ID:
- ivo://CDS.VizieR/J/ApJ/877/75
- Title:
- BVRI photom. of DV Psc and known short-period EBs
- Short Name:
- J/ApJ/877/75
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using 27 sets of new multiband photometry light curves acquired from our long-term photometric campaign carried out in the last 5yr and high-resolution spectroscopic data from seven nights, we analyzed the physical mechanisms of period variation, starspot cycle, optical flares, and chromospheric activities of the eclipsing binary DV Psc. Our updated O-C diagram covering a period of approximately 20yr shows an oscillation in its orbital period. This variations might be caused by a third body with an orbital period of 14.58+/-0.28yr. There are two active regions of starspots at longitude belts of about 90{deg} and 270{deg}. We obtained its starspot cycles with periods of 3.60+/-0.03yr and 3.42+/-0.02yr at about 90{deg} and 270{deg}, respectively. Moreover, the magnitude difference of Max.I-Max.II shows cyclic oscillation of 5.15+/-0.01yr. During our decade long photometric campaign, we observed DV Psc a total of 326.4hr, detected 18 outbursts (12 of them have never been reported) with flare energies in the range of (6.62-1106.85)x10^24^J. The slope of the relationship between the phase of the max flare and spots is 0.842 +/-0.083, implying a correlation between spots and flares. We discovered evidence for a correlation between the rotation period and the activity cycle for the short-period eclipsing binaries. Our high-resolution spectroscopic observations of DV Psc show obvious emissions above continuum in the H{alpha} line and small self-reversal emissions of the CaII IRT lines.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/AJ/151/124
- Title:
- BVR photometry of IZ Mon and AR Dra
- Short Name:
- J/AJ/151/124
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present multi-color photometric observations for two neglected near-contact binaries, IZ Mon (P=0.77980^d^) and AR Dra (P=0.67584^d^). By the aid of the updated W-D analysis code, the photometric solutions were deduced from the multi-color light curves (LCs). IZ Mon is a semi-detached binary with a mass ratio of q=0.388(+/-0.002) , while AR Dra is a detached star with a mass ratio of q=0.652(+/-0.002). The asymmetric LCs of IZ Mon were modeled by a hot spot on the secondary's surface, which may be attributed to mass transfer from the primary. Based on all collected eclipse times for two systems, we constructed their timing residual curves. The orbital period for IZ Mon may be continuously decreasing at a rate of dP/dt=-2.06(+/-0.04)days/yr, which may result from mass and angular momentum loss from the central system. For AR Dra, there exists a cyclic variation with a period of P_3_=104.9(+/-2.9)yr due to light-time orbit effect via the presence of the third body, whose mass is more than 0.28(+/-0.02)M_{Sun}_. Finally, two near-contact binaries, IZ Mon and AR Dra, will evolve into contact binaries.
- ID:
- ivo://CDS.VizieR/J/MNRAS/465/4968
- Title:
- Cataclysmic variables observations
- Short Name:
- J/MNRAS/465/4968
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new time-resolved photometry of 74 cataclysmic variables (CVs), 47 of which are eclipsing. Thirteen of these eclipsing systems are newly discovered. For all 47 eclipsing systems, we show high cadence (1-20s) light curves obtained with the high-speed cameras ULTRACAM and ULTRASPEC. We provide new or refined ephemerides, and supply mid-eclipse times for all observed eclipses. We assess the potential for light-curve modelling of all 47 eclipsing systems to determine their system parameters, finding 20 systems that appear to be suitable for future study. Systems of particular interest include V713 Cep, in which we observed a temporary switching-off of accretion; and ASASSN-14mv and CSS111019:233313-155744, which both have orbital periods well below the CV period minimum. The short orbital periods and light-curve shapes suggest that they may be double degenerate (AM CVn) systems or CVs with evolved donor stars.
- ID:
- ivo://CDS.VizieR/J/ApJS/213/9
- Title:
- Catalina Surveys periodic variable stars
- Short Name:
- J/ApJS/213/9
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present ~47000 periodic variables found during the analysis of 5.4 million variable star candidates within a 20000deg^2^ region covered by the Catalina Surveys Data Release-1 (CSDR1). Combining these variables with type ab RR Lyrae from our previous work, we produce an online catalog containing periods, amplitudes, and classifications for ~61000 periodic variables. By cross-matching these variables with those from prior surveys, we find that >90% of the ~8000 known periodic variables in the survey region are recovered. For these sources, we find excellent agreement between our catalog and prior values of luminosity, period, and amplitude as well as classification. We investigate the rate of confusion between objects classified as contact binaries and type c RR Lyrae (RRc's) based on periods, colors, amplitudes, metallicities, radial velocities, and surface gravities. We find that no more than a few percent of the variables in these classes are misidentified. By deriving distances for this clean sample of ~5500 RRc's, we trace the path of the Sagittarius tidal streams within the Galactic halo. Selecting 146 outer-halo RRc's with SDSS radial velocities, we confirm the presence of a coherent halo structure that is inconsistent with current N-body simulations of the Sagittarius tidal stream. We also find numerous long-period variables that are very likely associated within the Sagittarius tidal stream system. Based on the examination of 31000 contact binary light curves we find evidence for two subgroups exhibiting irregular light curves. One subgroup presents significant variations in mean brightness that are likely due to chromospheric activity. The other subgroup shows stable modulations over more than a thousand days and thereby provides evidence that the O'Connell effect is not due to stellar spots.
- ID:
- ivo://CDS.VizieR/V/121
- Title:
- Catalog of DMS-type eclipsing binaries
- Short Name:
- V/121
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The catalogue contains information about 113 detached main-sequence (DMS) type detached binaries with known photometric and geometric elements.
- ID:
- ivo://CDS.VizieR/V/120
- Title:
- Catalog of early-type contact binaries
- Short Name:
- V/120
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- For the first time the early type contact systems were identified as an individual class in M.A. Svechnikov's Catalogue [1] in 1969, which contains 8 systems of this type. The Catalogue of Coch R.H., Plavec M. and Wood F.B. [2] contains 37 systems of the early spectral type. According to Svechnikov's classification [3] a primary component (more massive and hotter) of a CE-system (contact system of early spectral class) has a spectral class earlier than F0-F2 and an orbital period of more than 0.5 day. Usually the spectral class of a primary is earlier than the spectral class of a secondary. Both components fill their Roche-lobes on 90-100%. The following Catalogue of Svechnikov M.A. and Bessonova L.A. [4] contains 38 CE-systems. In 1986 Bondarenko I.I. [5] published the Catalogue of the CE-stars, which contained 83 systems. Physical characteristics of the CE-stars presented in the list of catalogues abovementioned, were obtained by different authors by using different methods of calculation. We propose the Catalogue of the CE-systems with homogeneous absolute physical characteristics, that allows to define accurately general features of this class of binary stars. The comparing of physical characteristics of the CE-systems with other classes` characteristics of binary stars can show the possible evolutionary stages of the CE-systems. The foundation of absolute elements of the CE-systems are the photometric observations (on the whole, the latest multicolour photoelectric, in a few cases photographic and visual observations). The accuracy of modern photometric observations is high, and generally they are processed with the help of reliable computer methods both classical and synthetical methods). But reliable spectral observations (the ray speed curves) are very scarce, especially for both components). We have preferred the spectral class of a primary (usually it is more bright), supposing, that it's spectral class was defined accurately, and photometric and geometrical elements from light curves. All stars from our Catalogue were classified preliminarily as CE-stars by Svechnikov M.A., Istomin L.F. and Grehova O.A. [6]. We have supposed both components fill their Roche-lobes and by using the diagram (q-r[critical]) of Plavec-Kratochvile [7] mass ratio was obtained. The absolute elements were obtained by the approximated method of Svechnikov, which was modernized for CE-stars. Our Catalogue consist of three parts: photometric, geometrical and absolute elements of CE-systems. All stars were divided approximately into two groups: massive (m1>3 solar masses for primary) and less-massive stars (m1<3 solar masses for primary). A Catalogue has a Supplement.
- ID:
- ivo://CDS.VizieR/V/118
- Title:
- Catalog of eclipsing binaries parameters
- Short Name:
- V/118
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalogue contains information about 44 binaries with known photometric orbit elements and unknown spectroscopic one.
- ID:
- ivo://CDS.VizieR/J/other/A+AT/23.213
- Title:
- Catalog of massive close binaries
- Short Name:
- J/other/A+AT/23.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalogue contains compilations of observable data for 176 massive close binaries with components earlier than approximately B5 of the main sequence are presented.
- ID:
- ivo://CDS.VizieR/J/AJ/147/119
- Title:
- Catalog of sources in the Kepler field of view
- Short Name:
- J/AJ/147/119
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Kepler mission has to date found almost 6000 planetary transit-like signals, utilizing three years of data for over 170000 stars at extremely high photometric precision. Due to its design, contamination from eclipsing binaries, variable stars, and other transiting planets results in a significant number of these signals being false positives (FPs). This directly affects the determination of the occurrence rate of Earth-like planets in our Galaxy, as well as other planet population statistics. In order to detect as many of these FPs as possible, we perform ephemeris matching among all transiting planet, eclipsing binary, and variable star sources. We find that 685 Kepler Objects of Interest (KOIs)--12% of all those analyzed--are FPs as a result of contamination, due to 409 unique parent sources. Of these, 118 have not previously been identified by other methods. We estimate that ~35% of KOIs are FPs due to contamination, when performing a first-order correction for observational bias. Comparing single-planet candidate KOIs to multi-planet candidate KOIs, we find an observed FP fraction due to contamination of 16% and 2.4% respectively, bolstering the existing evidence that multi-planet KOIs are significantly less likely to be FPs. We also analyze the parameter distributions of the ephemeris matches and derive a simple model for the most common type of contamination in the Kepler field. We find that the ephemeris matching technique is able to identify low signal-to-noise FPs that are difficult to identify with other vetting techniques. We expect FP KOIs to become more frequent when analyzing more quarters of Kepler data, and note that many of them will not be able to be identified based on Kepler data alone.
- ID:
- ivo://CDS.VizieR/J/A+A/417/263
- Title:
- Catalogue of Algol type binary stars
- Short Name:
- J/A+A/417/263
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A catalogue of (411) Algol-type (semi-detached) binary stars is presented in the form of five separate tables of information. The catalogue has developed from an earlier version (Budding, 1984, Cat. <V/46>) by including more recent information and an improved layout. A sixth table lists (1872) candidate Algols, about which fewer details are known at present. Some issues relating to the classification and interpretation of Algol-like binaries are also discussed.
