Symbiotic Nova PU Vul - 33 Years of Observations

2012 ◽  
Vol 21 (1-2) ◽  
Author(s):  
S. Shugarov ◽  
D. Chochol ◽  
E. Kolotilov
Keyword(s):  
Binary System ◽  
Light Curves ◽  
Secondary Minimum ◽  
Pulsation Period ◽  
Primary Minimum ◽  
Cool Component ◽  
Period Analysis ◽  
Binary Orbit ◽  
Orbit Period

AbstractWe present UBVRI light curves of the symbiotic nova PU Vul after its outburst in 1978. Three observed eclipses of the hot component by the cool one were used to determine the ephemeris of the binary system as JD (Min I) = 2444550(15) + 4897(10) × E days. the 194-day shift of the secondary minimum from its expected positions in 2001 suggests the eccentricity of the binary orbit. Period analysis of the VRI photometry improved the pulsation period of the cool AGB variable in the system to P = 217.7 days. Pulsation of the cool component is detected only in the phases around the primary minimum, when the visible hemisphere of the AGB star is not influenced by the interaction with the hot component.

scholarly journals UBV Photometry of the Massive Eclipsing Binary TT Aur

2001 ◽  
Vol 18 (2) ◽  
pp. 151-157 ◽  
Author(s):  
S. Özdemir ◽  
H. Ak ◽  
M. Tanriver ◽  
H. Gülseçen ◽  
S. Gülseçen ◽  
...  
Keyword(s):  
Binary System ◽  
Primary Component ◽  
Light Curves ◽  
National Observatory ◽  
Simultaneous Solution ◽  
Primary Minimum ◽  
Circumstellar Material ◽  
System Parameters ◽  
Ubv Photometry ◽  
Excess Absorption

AbstractUBV observations of the massive binary system TT Aur were carried out mainly at theTurkish National Observatory (TUG). These observations, together with IUE spectra and times of eclipse minima collected from the literature, were used to study the system parameters.Simultaneous solution of the light curves by the Wilson-Devinney code allows a semi-detached configuration with a slightly larger Roche-lobe filling secondary. This picture is supported by other evidence. The shoulders of the primary minimum suggest some excess absorption, in keeping with circumstellar material in the form of a disk-like structure around the primary component. The deeper primary minimum in the U filter may indicate a hotter region on the secondary-facing hemisphere of the primary.The period variation of the system can also be related to the possible existence of a third component in a circular orbit around the system.An alternative detached representation is also considered using optimal curve-fitting techniques. We appeal for further observations to help resolve some outstanding issues in this interesting massive binary.

scholarly journals The newly discovered Be/X-ray binary Swift J004516.6–734703 in the SMC: witnessing the emergence of a circumstellar disc

2020 ◽  
Vol 499 (1) ◽  
pp. L41-L46
Author(s):  
J A Kennea ◽  
M J Coe ◽  
P A Evans ◽  
I M Monageng ◽  
L J Townsend ◽  
...  
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Light Curves ◽  
Type I ◽  
Pulsation Period ◽  
X Ray ◽  
Tidal Interaction ◽  
Long Period ◽  
Periodicity Analysis ◽  
Ir Light

ABSTRACT We report on the discovery of Swift J004516.6–734703, a Be/X-ray binary system by the Swift SMC Survey, S-CUBED. Swift J004516.6–734703, or SXP 146.6, was found to be exhibiting a bright (∼1037 erg s−1) X-ray outburst on 2020 June 18. The historical UV and IR light-curves from OGLE and Swift/UVOT showed that after a long period of steady brightness, it experienced a significant brightening beginning around 2019 March. This IR/UV rise is likely the signature of the formation of a circumstellar disc, confirmed by the presence of strong an H α line in SALT spectroscopy, that was not previously present. Periodicity analysis of the OGLE data reveals a plausible 426 d binary period, and in X-ray a pulsation period of 146.6 s is detected. The onset of X-ray emission from Swift J004516.6–734703 is likely the signature of a Type-I outburst from the first periastron passage of the neutron star companion through the newly formed circumstellar disc. We note that the formation of the circumstellar disc began at the predicted time of the previous periastron passage, suggesting its formation was spurred by tidal interaction with the neutron star.

scholarly journals BVRI Light Curves and Period Analysis of the Beta Lyrae System XX Leonis

2006 ◽  
Vol 2 (S240) ◽  
pp. 551-554
Author(s):  
P. Zasche ◽  
P. Svoboda ◽  
M. Wolf
Keyword(s):  
Binary System ◽  
Primary Component ◽  
Light Curves ◽  
Minimum Mass ◽  
Mass Ratio ◽  
Third Body ◽  
Photometric Analysis ◽  
Period Analysis ◽  
The Third ◽  
Ccd Detector

AbstractThe contact eclipsing binary system XX Leonis (p = 0.97 days, Sp A9) has been analysed using the PHOEBE programme, based on the Wilson–Devinney code. The BVRI light curves were obtained during spring 2006 using the 20-cm telescope and ST-7 CCD detector. The effective temperature of the primary component determined from the photometric analysis is T = (7342 ± 14) K, the inclination of the orbit is i = (84.83 ± 0.29)° and the photometric mass ratio q = (0.40 ± 0.01). The third-body hypothesis was also suggested; based on a period analysis using 57 minimum times this gave a period for the third body of p3 = (59.66 ± 0.05) yr, an amplitude of A = (0.036 ± 0.028) day and zero eccentricity, which yields as a minimum mass M3,min = (0.91 ± 0.01) M⊙.

scholarly journals New Data on the Eclipsing Binary V1848 Ori and Improved Orbital and Light Curve Solutions

2020 ◽  
Vol 29 (1) ◽  
pp. 72-80 ◽  
Author(s):  
Fatemeh Davoudi ◽  
Atila Poro ◽  
Fahri Alicavus ◽  
Afshin Halavati ◽  
Saeed Doostmohammadi ◽  
...  
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Mass Function ◽  
Light Curves ◽  
Complete Analysis ◽  
Physical Parameters ◽  
Mass Ratio ◽  
Third Body ◽  
Eclipsing Binary

AbstractNew observations of the eclipsing binary system V1848 Ori were carried out using the V filter resulting in a determination of new times of minima and new ephemeris were obtained. We presented the first complete analysis of the system’s orbital period behavior and analysis of O-C diagram done by the GA and MCMC approaches in OCFit code. The O-C diagram demonstrates a sinusoidal trend in the data; this trend suggests a cyclic change caused by the LITE effect with a period of 10.57 years and an amplitude of 7.182 minutes. It appears that there is a third body with mass function of f (m3) = 0.0058 M⊙ in this binary system. The light curves were analyzed using the Wilson-Devinney code to determine some geometrical and physical parameters of the system. These results show that V1848 Ori is a contact W UMa binary system with the mass ratio of q = 0.76 and a weak fillout factor of 5.8%. The O’Connell effect was not seen in the light curve and there is no need to add spot.

The Massive Binary System RY Sct – New Solution of the Light Curves

Astrophysics ◽  
2020 ◽  
Vol 63 (2) ◽  
pp. 243-251
Author(s):  
N. Kochiashvili ◽  
I. Kochiashvili ◽  
R. Natsvlishvili ◽  
S. Beradze ◽  
M. Vardosanidze
Keyword(s):  
Binary System ◽  
Light Curves

scholarly journals Interpreting the Evolving Clumpy Shell Structure of IRC +10216 in Terms of Time Dependent Dust Shell Models

2003 ◽  
Vol 209 ◽  
pp. 127-128
Author(s):  
J. M. Winters ◽  
T. Blöcker ◽  
K.-H. Hofmann ◽  
G. Weigelt
Keyword(s):  
Time Scale ◽  
High Spatial Resolution ◽  
Light Curves ◽  
Infrared Light ◽  
Pulsation Period ◽  
Line Profiles ◽  
Dust Shell ◽  
Time Intervals ◽  
Stellar Pulsation ◽  
Shell Models

The prototypical dust-enshrouded carbon Mira IRC +10216 is known to exhibit intrinsic changes on a time scale of the order of only a few years as revealed, e.g., by CO infrared line profiles (Winters et al. 2000a), its infrared light curves, and by high spatial resolution monitoring in the infrared (Osterbart et al. 2000; Tuthill et al. 2000). In particular, the infrared light curves indicate a possible periodicity on a ≈ 20 yr time scale, i.e. that a recurrent phenomenon might lead to the observed variations. Such multi-periodicity time scales of several (≈ 10) stellar pulsation periods are predicted by consistent hydrodynamical models which include a proper treatment of dust formation (e.g. Winters et al. 2000b). In these models discrete dust layers form in time intervals which are several times longer than the typical pulsation period of an AGB star (Fleischer, Gauger, & Sedlmayr 1995; Höfner, Feuchtinger, & Dorfi 1995).

scholarly journals Variability of the Light Curves of the Close Binary GR Tauri

2002 ◽  
Vol 187 ◽  
pp. 337-338
Author(s):  
A. Yamasaki ◽  
M. Takeda ◽  
T. Yamauchi ◽  
G. Takada ◽  
S. Hattori
Keyword(s):  
Binary System ◽  
The State ◽  
Light Curves ◽  
Close Binary ◽  
Eclipsing Binary ◽  
Short Period ◽  
Contact Binary

AbstractVariability of the light curves of the short-period eclipsing binary system GR Tau (, almost-contact binary) is studied. It is found that GR Tau experienced both the state which is characterized by asymmetric light curves and the state characterized by symmetrical light curves.

scholarly journals δ Sct-Type Pulsators in Eclipsing Binary Systems: the Case of RZ Cas

2002 ◽  
Vol 185 ◽  
pp. 102-103
Author(s):  
E. Rodríguez ◽  
V. Costa ◽  
M.J. López-González ◽  
J.M. García ◽  
S.L. Kim ◽  
...  
Keyword(s):  
Binary System ◽  
Binary Systems ◽  
Hot Spot ◽  
Primary Component ◽  
Roche Lobe ◽  
Light Curves ◽  
Eclipsing Binary ◽  
Preliminary Results ◽  
The Impact

AbstractRZ Cas is an Algol-type eclipsing binary system where the primary component was recently discovered as a δ Set pulsator. A three-continent multisite photometric campaign was carried out during 1999. Preliminary results are reported here indicating a semi-detached system where the secondary fills its Roche lobe. The light curves also suggest a hot spot on the surface of the primary component as a consequence of the impact of the mass stream from the secondary. The pulsational behaviour can be well described with only one frequency.

scholarly journals The Symbiotic Binary System AG Pegasi

1980 ◽  
Vol 88 ◽  
pp. 535-542 ◽  
Author(s):  
Charles D. Keyes ◽  
Mirek J. Plavec
Keyword(s):  
Binary System ◽  
Emission Lines ◽  
Complete Coverage ◽  
Cool Component ◽  
Relative Contribution ◽  
Photometric Observations

A complete coverage of the spectrum of AG Peg has been obtained between wavelengths 1200 − 7000 A by us, and can be supplemented by IR photometric observations by others. Our IUE observations yield a lower value of E(B-V), about 0.12. The two stellar components are easily recognized, but their characteristics are still rather uncertain.The cool component may be a normal M1.7 III giant, but the temperature and luminosity of the hot star remain largely indeterminate. Firstly, there are no good models for a hot subdwarf, and secondly, it is difficult to determine the relative contribution of the star itself and the surrounding hydrogen cloud.The emission lines observed in the UV have double or triple structure, indicating two or three distinct emitting regions.

scholarly journals The Star Spot Model and the Observations of SZ Piscium

1980 ◽  
Vol 88 ◽  
pp. 415-418
Author(s):  
Shyam M. Jakate
Keyword(s):  
Secondary Minimum ◽  
Primary Minimum ◽  
Photometric Observations ◽  
Spot Model ◽  
Spot Activity

Details of photometric observations during the totalities of the primary and secondary minima of SZ Psc are analysed in the light of the “star spot model” for RS CVn type binaries. Presence of scatter during the totality of primary minimum and its absence during the totality of secondary minimum of SZ Psc provide evidence towards one of the assumptions of the model,i.e. the spot activity confines to one of the hemispheres of the cooler star.

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