- ID:
- ivo://CDS.VizieR/J/other/NewA/31.65
- Title:
- BVRcIc light curves of LU Lac
- Short Name:
- J/other/NewA/31.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- LU Lac is a neglected W UMa binary star in photometric investigations. In this paper, we present BVRI CCD photometric light curves obtained on one night in 2012. The first photometric solutions of this system are computed by using the Wilson-Devinney code. It is shown that LU Lac is a marginal contact W-type system with a degree of contact factor of f=8.9%, a mass ratio of q=2.085 and a high inclination of i=82.20{deg}. From the first analyses of orbital period changes, we found the period variation of the system includes an oscillation (A3=0.0125-days and T3=51.92-years). The cyclic change may be attributed to the light-travel time effect through the presence of a third body.
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- ID:
- ivo://CDS.VizieR/J/AJ/152/219
- Title:
- BV(RI)c light curves of DD Indi
- Short Name:
- J/AJ/152/219
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Observations and a 2015 Wilson-Devinney Program analysis are undertaken for the first precision observations of DD Indi. DD Indi is of solar-type (T_1_~5750K) and was determined to be a shallow-contact eclipsing binary. It was observed from 2013 June through September at Cerro Tololo InterAmerican Observatory in remote mode. The 24 inch Boller and Chivens reflector, now under management by The Southeastern Association for Resarch in Astronomy (SARA) was used. Five new eclipse timings were obtained, for three primary and two secondary eclipses. Seven more eclipse timings were calculated from All Sky Automated Survey data. A possibly increasing period was found from all available eclipse timings with a 5+/-2x10^-11^xE^2^ quadratic term. A BVR_c_I_c_ simultaneous synthetic light-curve analysis reveals that the system has a mass ratio of ~0.46, a ~140K component temperature difference, and two weak cool spots. The Roche Lobe fill-out of this W-type binary is only ~11%, and an inclination of ~86{deg} was determined. A time of constant light of ~16 minutes is measured around phase zero. More detail is included in this report.
- ID:
- ivo://CDS.VizieR/J/AJ/152/199
- Title:
- BV(RI)c light curves of FF Vul
- Short Name:
- J/AJ/152/199
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- High-precision BVR_c_I_c_ light curves of FF Vul were taken during the fall of 2015 with the Dark Sky Observatory 0.81m reflector of Appalachian State University, and the SARA north 0.91m reflector at KPNO. FF Vul is an eclipsing binary with a period of 0.44 day. A Wilson-Devinney solution shows that the binary is a near-contact, semidetached binary, i.e., with a V1010 Oph-type configuration. Five eclipse timings (three primary and two secondary) were calculated. A quadratic ephemeris was determined indicating that the period is decreasing. A near-equatorial hot spot was modeled on the cooler, secondary star, possibly caused by matter impacting from the primary component via the inner Lagrangian point. The component temperature difference is more than 1500K. The solution confirms a total secondary eclipse of 23 minutes duration. As expected in binaries of this type, there is a magnetic spot region.
- ID:
- ivo://CDS.VizieR/J/AJ/152/227
- Title:
- BV(RI)c light curves of NSVS 5066754
- Short Name:
- J/AJ/152/227
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- BVR_c_I_c_ light curves of NSVS 5066754 were taken on 2014 May at Dark Sky Observatory in North Carolina. This variable is a solar-type eclipsing binary (T1~5750K) with a period of only 0.3751689(1) days. It appeared to be one of the shortest periods in Shaw's list of near-contact binaries. The Binary Maker fits and our Wilson-Devinney solutions show that the binary could have both semidetached and marginal contact binary configurations. Five new times of minimum light were calculated, along with two minima determined from archived All Sky Automated Survey observations. From these minima and the discovery epoch, a quadratic ephemeris was determined. Thus, a magnetic braking scenario is possible. Both semidetached and contact models were explored. A marginal contact solution had the best sum of square residuals. It gave a mass ratio of ~0.5, and a component temperature difference of ~360K, albeit somewhat large for a contact binary. Two substantial cool spots were determined in this solution with 37{deg} and 28{deg} radii and t-factors or 0.94 and 0.78 respectively. The fill-out is very shallow, ~106%. It may have recently achieved contact.
- ID:
- ivo://CDS.VizieR/J/AJ/145/14
- Title:
- BV(RI)c light curves of V1043 Cas
- Short Name:
- J/AJ/145/14
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Complete Bessel BVR_c_I_c_ light curves of V1043 Cassiopeia [2MASS J00371195+5301324, Mis V1292, USNO-A2.0 1425-00875743, {alpha}(2000)=00^h^37^m^11.95^s^, {delta}(2000)=+53{deg}01'32.5"] are analyzed. The system is a member of the small group of pre-contact W UMa binaries (PCWBs). Its light curve has the appearance of an Algol (EA) light curve, however it is made up of dwarf solar type components in a detached mode with a period of only 0.6616days. The analysis includes a period study, an improved ephemeris, a mass ratio search, and a simultaneous BVR_c_I_c_ Wilson-Devinney solution. We document about 20 other PCWBs given in the literature. Several have RS CVn-like properties.
- ID:
- ivo://CDS.VizieR/J/AJ/147/3
- Title:
- BV(RI)c light curves of V2421 Cyg
- Short Name:
- J/AJ/147/3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the first precision BVRI light curves, synthetic light curve solutions, and a period study for the high amplitude solar type binary, V2421 Cygni. The light curves have the appearance of an Algol (EA) type; however, it is made up of dwarf solar type components in a detached mode with a period of only 0.6331 days with an amplitude of about a full magnitude, i.e., it is a precontact W UMa binary. Flare-like disruptions occur in the light curves following the primary and secondary eclipses possibly due to the line-of-sight track of a gas stream. An associated stream spot and splash spot cause bright equatorial spots on the stellar surface of the primary star. The more massive star is the gainer, making this system a classic, albeit dwarf, Algol.
- ID:
- ivo://CDS.VizieR/J/AJ/149/30
- Title:
- BVRI differential photometry of V1001 Cas in 2012
- Short Name:
- J/AJ/149/30
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A 2012 follow up to the analysis of 2009 observations is presented for the very short period (~0.43days) precontact W UMa binary (PCWB) V1001 Cassiopeia. Its short period, similar to the majority of W UMa binaries, and its distinct EA light curve make it a very rare and interesting system for continuing photometric investigation. Previous photometric VRI standard magnitudes give a K4 spectral type. Our solutions of light curves separated by some three years give approximately the same physical parameters. However, the spots have radically changed in temperature, area, and position. While only one dark spot was used to model the first curves, two hot spots are now needed. This affects the overall shape of the light curve, especially in the secondary eclipses in B and V. Additional eclipse timings now show that the orbital period is changing. We conclude that spots are very active on this solar-type dwarf system and that it may mimic its larger cousins, the RS CVn binaries. The conclusion is that analysis now needs to be directed at the continuous time evolution of PCWBs.
- ID:
- ivo://CDS.VizieR/J/ApJ/788/41
- Title:
- BVRI light curve of OGLE LMC-ECL-11893
- Short Name:
- J/ApJ/788/41
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the serendipitous discovery of a disk-eclipse system OGLE-LMC-ECL-11893. The eclipse occurs with a period of 468 days, a duration of about 15 days, and a deep (up to {Delta}m_I_~1.5), peculiar, and asymmetric profile. A possible origin of such an eclipse profile involves a circumstellar disk. The presence of the disk is confirmed by the H-alpha line profile from the follow-up spectroscopic observations, and the star is identified as Be/Ae type. Unlike the previously known disk-eclipse candidates, the eclipses of OGLE-LMC-ECL-11893 retain the same shape throughout the span of ~17yr (13 orbital periods), indicating no measurable orbital precession of the disk.
- ID:
- ivo://CDS.VizieR/J/A+A/542/A78
- Title:
- BVRI light curves and RV curves of 65 UMa
- Short Name:
- J/A+A/542/A78
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The study of stellar multiple systems provides us with important information about the stellar formation processes and can help us to estimate the multiplicity fraction in the Galaxy. 65 UMa belongs to a rather small group of stellar systems of higher multiplicity, whose inner and outer orbits are well-known. This allows us to study the long-term stability and evolution of the orbits in these systems. We obtained new photometric and spectroscopic data that when combined with interferometric data enables us to analyze the system 65 UMa and determine its basic physical properties.
- ID:
- ivo://CDS.VizieR/J/A+A/539/A129
- Title:
- BVRI light curves of 3 eclipsing binaries
- Short Name:
- J/A+A/539/A129
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We aim to derive the absolute parameters of the components of AD And, AL Cam, and V338 Her, interpret their orbital period changes and discuss their evolutionary status. New and complete multi-filter light curves of the eclipsing binaries AD And, AL Cam, and V338 Her were obtained and analysed with modern methods. Using all reliably observed times of minimum light, we examined orbital period irregularities using the least squares method. In addition, we acquired new spectroscopic observations during the secondary eclipses for AL Cam and V338 Her. For AL Cam and V338 Her, we derive reliable spectral types for their primary stars. Statistical checks of orbital period analysis for all systems are very reassuring in the cases of V338 Her and AD And, although less so for AL Cam. The LIght-Time Effect (LITE) results are checked by inclusion of a third light option in the photometric analyses. Light curve solutions provide the means to calculate the absolute parameters of the components of the systems and reliably estimate their present evolutionary status. AL Cam and V338 Her are confirmed as classical Algols of relatively low mass in similar configurations. Unlike AL Cam, however, V338 Her is still transferring matter between its components, raising interest in the determinability of the evolutionary histories of Algols. AD And is found to be a detached system in which both close stars are of age 10^9^yr and is probably a "non-classical" young triple, at an interesting stage of its dynamical evolution.
