The Periodicity Analysis of the Light Curve of 3C 279 and Implications for the Precession Jet

2009 ◽  
Vol 121 (885) ◽  
pp. 1172-1179 ◽  
Author(s):  
H. Z. Li ◽  
G. Z. Xie ◽  
L. E. Chen ◽  
H. Dai ◽  
B. Y. Lei ◽  
...  
Keyword(s):  
Light Curve ◽  
Periodicity Analysis

Periodicity analysis of the radio light curve of the Seyfert galaxy III Zw 2

New Astronomy ◽  
2010 ◽  
Vol 15 (2) ◽  
pp. 254-259 ◽  
Author(s):  
H.Z. Li ◽  
G.Z. Xie ◽  
H. Dai ◽  
L.E. Chen ◽  
T.F. Yi ◽  
...  
Keyword(s):  
Light Curve ◽  
Seyfert Galaxy ◽  
Periodicity Analysis

THE PERIODICITY ANALYSIS OF THE LIGHT CURVE OF PKS 0735+178 AND IMPLICATIONS FOR ITS CENTRAL STRUCTURE

2004 ◽  
Vol 13 (04) ◽  
pp. 771-782 ◽  
Author(s):  
S. X. DING ◽  
G. Z. XIE ◽  
E. W. LIANG ◽  
S. B. ZHOU ◽  
L. MA
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Light Curve ◽  
Observation Data ◽  
Binary Black Hole ◽  
Periodicity Analysis ◽  
Power Spectrum Method ◽  
Hole Model ◽  
The Masses ◽  
Good Agreement

The observation data in the B band for BL Lacerate object PKS 0735+178 during 1970–1998 from twenty two publications have been compiled into a light curve. The light curve shows that PKS 0735+178 is very active and exhibits very complicated non-sinusoidal variations. Using both Jurkevich's method and Power spectrum method to analyze these data we have found two periods of 5.26±0.98 years and 1.24±0.05 years for the outbursts in PKS 0735+178. It is of interest to note that the results of the two methods are the same (almost). In addition, these values are in good agreement with the results found by Smith et al.47 and Webb et al.61 We also apply the binary black hole model to explain the central structure of this object and obtain the masses of the primary and secondary black holes are 1.7×109M⊙ and 2.88×107M⊙ respectively. It should be monitored in future to obtain more data for further analysis to test the hypothesis.

A Periodicity Analysis of the Light Curve of 3C 454.3

2006 ◽  
Vol 6 (4) ◽  
pp. 421-429 ◽  
Author(s):  
Huai-Zhen Li ◽  
Guang-Zhong Xie ◽  
Shu-Bai Zhou ◽  
Hong-Tao Liu ◽  
Guang-Wei Cha ◽  
...  
Keyword(s):  
Light Curve ◽  
Periodicity Analysis

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.

A Radial Velocity and Light Curve Study of Pulsations and Binarity in Proto-Planetary Nebulae

2015 ◽  
Vol 71-72 ◽  
pp. 127-128
Author(s):  
B.J. Hrivnak ◽  
W. Lu ◽  
G. Van de Steene ◽  
H. Van Winckel ◽  
J. Sperauskas ◽  
...  
Keyword(s):  
Light Curve ◽  
Radial Velocity ◽  
Planetary Nebulae

SN2017ein: bolometric light curve and physical parameters

2017 ◽  
Vol 4 (1) ◽  
pp. 15-19
Author(s):  
P.S. Tadjimuratov ◽  
◽  
D. Mirzakulov ◽  
Keyword(s):  
Light Curve ◽  
Physical Parameters

Optical Light Curve of the Type I[CLC]a[/CLC] Supernova 1998[CLC]bu[/CLC] in M96 and the Supernova Calibration of the Hubble Constant

1999 ◽  
Vol 117 (3) ◽  
pp. 1175-1184 ◽  
Author(s):  
Nicholas B. Suntzeff ◽  
M. M. Phillips ◽  
R. Covarrubias ◽  
M. Navarrete ◽  
J. J. Pérez ◽  
...  
Keyword(s):  
Light Curve ◽  
Hubble Constant ◽  
Type I ◽  
Optical Light Curve
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