Fractal Property in the Light Curve of BL Lac Object S5 0716 + 714

2014 ◽  
Vol 35 (3) ◽  
pp. 293-296
Author(s):  
J. W. Ou ◽  
Y. G. Zheng
Keyword(s):  
Light Curve ◽  
Fractal Property ◽  
Bl Lac

scholarly journals Observations of PKS 2155–304 with the Extreme Ultraviolet Explorer

1994 ◽  
Vol 159 ◽  
pp. 322-322
Author(s):  
A. Fruscione ◽  
C.S. Bowyer ◽  
T.E. Carone ◽  
S.M. Kahn ◽  
A. Königl ◽  
...  
Keyword(s):  
Light Curve ◽  
Spectroscopic Data ◽  
Extreme Ultraviolet ◽  
High Accuracy ◽  
Bl Lac ◽  
Deep Survey

We have studied the first extreme ultraviolet spectroscopic data and a high accuracy light curve for the BL Lac object PKS 2155–304 observed with the Extreme Ultraviolet Explorer (EUVE) on July 21–22, 1992. This target was observed with the Deep Survey Spectrometer telescope for approximateley 30,000 sec during the in-orbit-calibration phase of the mission, allowing to obtain simultaneous image and spectrum.

scholarly journals QUASI-PERIODIC OSCILLATIONS OF ∼15 MINUTES IN THE OPTICAL LIGHT CURVE OF THE BL LAC S5 0716+714

2010 ◽  
Vol 719 (2) ◽  
pp. L153-L157 ◽  
Author(s):  
Bindu Rani ◽  
Alok C. Gupta ◽  
U. C. Joshi ◽  
S. Ganesh ◽  
Paul J. Wiita
Keyword(s):  
Light Curve ◽  
Periodic Oscillations ◽  
Bl Lac ◽  
Optical Light Curve

scholarly journals DETECTION OF POSSIBLE QUASI-PERIODIC OSCILLATIONS IN THE LONG-TERM OPTICAL LIGHT CURVE OF THE BL LAC OBJECT OJ 287

2016 ◽  
Vol 832 (1) ◽  
pp. 47 ◽  
Author(s):  
G. Bhatta ◽  
S. Zola ◽  
Ł. Stawarz ◽  
M. Ostrowski ◽  
M. Winiarski ◽  
...  
Keyword(s):  
Light Curve ◽  
Periodic Oscillations ◽  
Bl Lac ◽  
Optical Light Curve

scholarly journals A study of the middle time-scale periodic behavior of light curve of BL Lac object OJ287

2015 ◽  
Vol 64 (13) ◽  
pp. 139801
Author(s):  
Ding Nan ◽  
Zhang Hao-Jing ◽  
Zhang Xiong ◽  
Ou Jian-Wen ◽  
Luo Dan
Keyword(s):  
Light Curve ◽  
Time Scale ◽  
Periodic Behavior ◽  
Bl Lac

scholarly journals A study of the light curve periodic behavior of BL Lac object S5 0716+714

2007 ◽  
Vol 56 (7) ◽  
pp. 4305
Author(s):  
Zhang Hao-Jing ◽  
Zhang Xiong
Keyword(s):  
Light Curve ◽  
Periodic Behavior ◽  
Bl Lac

scholarly journals A Variability Study of Long-term Optical Data of OJ 287

2012 ◽  
Vol 8 (S290) ◽  
pp. 269-270 ◽  
Author(s):  
Y. Liu ◽  
J. H. Fan ◽  
H. G. Wang ◽  
G. G. Deng
Keyword(s):  
Light Curve ◽  
Power Law ◽  
Decay Time ◽  
Time Scale ◽  
Power Spectra ◽  
Optical Data ◽  
Bl Lac ◽  
Optical Light Curve ◽  
Variability Study

AbstractIn this paper, we investigated the possible exponential decays in the long term optical light curve of the BL Lac {OJ 287}. We developed a method that can be used to decomposing a light curve into a linear combination of exponential decays. The decomposing shows that the decay time scales range from ~ 103.6 to ~ 10−4 days. The power spectra has frequency-dependent power-law with slop ~ 0.5, and the peak of power is at the time scale of decay on ~ 160 days.

A NEW ANALYSIS OF THE MEDIUM-TIMESCALE PERIODICITY IN S5 0716+714

2004 ◽  
Vol 13 (04) ◽  
pp. 659-668 ◽  
Author(s):  
L. MA ◽  
G. Z. XIE ◽  
S. B. ZHOU ◽  
L. E. CHEN ◽  
S. X. DING ◽  
...  
Keyword(s):  
Power Spectrum ◽  
Light Curve ◽  
Observation Data ◽  
Spectrum Method ◽  
Bl Lac ◽  
Power Spectrum Method ◽  
Good Agreement

In this paper, we have collected the available observation data of BL Lac S5 0716+714 in I-band from published literature during 1994 to 2000. The light curve shows S5 0716+714 is very active and very complicated non-sinusoidal variations. We studied its medium-timescale periodicity using the Jurkevich and power spectrum method to search for the possible medium-timescale periods and found that one possible medium-timescale periodic with a period of around 14±0.1 day is obtained for S5 0716+714. It is interesting to note that these results are in good agreement with the previous results by Impey et al. (2000) and Qian et al. (2002), and this work provides a new analysis and evidence of the medium-timescale periodicity in BL Lac S5 0716+714. The helical jet model seems to be more reasonable for explaining our results than other models.

The Eclipsing Binary WX Eridani

1979 ◽  
Vol 46 ◽  
pp. 385
Author(s):  
M.B.K. Sarma ◽  
K.D. Abhankar
Keyword(s):  
Light Curve ◽  
Spectral Type ◽  
Orbital Period ◽  
Primary Component ◽  
Light Curves ◽  
Absorption Feature ◽  
Primary Star ◽  
Eclipsing Binary ◽  
The Times ◽  
Phase Angles

AbstractThe Algol-type eclipsing binary WX Eridani was observed on 21 nights on the 48-inch telescope of the Japal-Rangapur Observatory during 1973-75 in B and V colours. An improved period of P = 0.82327038 days was obtained from the analysis of the times of five primary minima. An absorption feature between phase angles 50-80, 100-130, 230-260 and 280-310 was present in the light curves. The analysis of the light curves indicated the eclipses to be grazing with primary to be transit and secondary, an occultation. Elements derived from the solution of the light curve using Russel-Merrill method are given. From comparison of the fractional radii with Roche lobes, it is concluded that none of the components have filled their respective lobes but the primary star seems to be evolving. The spectral type of the primary component was estimated to be F3 and is found to be pulsating with two periods equal to one-fifth and one-sixth of the orbital period.

RSCVn Stars in the Southern Hemisphere

1979 ◽  
Vol 46 ◽  
pp. 371-384 ◽  
Author(s):  
J.B. Hearnshaw
Keyword(s):  
Light Curve ◽  
Southern Hemisphere ◽  
Orbital Period ◽  
Binary Stars ◽  
Small Amplitude ◽  
Light Variation ◽  
Orbital Phase

RSCVn stars are fully detached binary stars which show intrinsic small amplitude (up to 0.3 amplitude peak-to-peak) light variations, as well as, in most of the known cases, eclipses. The spectra are F to G, IV to V for the hotter component and usually KOIV for the cooler. They are also characterised by abnormally strong H and K emission from the cooler star, or, occasionally, from both components. The orbital and light curve periods are in the range 1 day to 2 weeks. An interesting feature is the migration of the light variations to earlier orbital phase, as the light variation period is shorter than the orbital period by a few parts in 10+4to a few parts in 10+3.

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