Orbital Period of a Binary System in the Field-Boost Approach.

2004 ◽  
Vol 17 (4) ◽  
pp. 435-441
Author(s):  
J. Lucinda ◽  
D. W. Foryta ◽  
M. G. Rodbard
Keyword(s):  
Binary System ◽  
Orbital Period

scholarly journals Onthe changes in the physical properties of the ionized region around the Weigelt structures in η Carinae over the 5.54-yr spectroscopic cycle

2020 ◽  
Vol 495 (3) ◽  
pp. 2754-2770 ◽  
Author(s):  
M Teodoro ◽  
T R Gull ◽  
M A Bautista ◽  
D J Hillier ◽  
G Weigelt ◽  
...  
Keyword(s):  
Binary System ◽  
Electron Temperature ◽  
Ionization Potential ◽  
Orbital Period ◽  
Equatorial Plane ◽  
Proper Motion ◽  
Emission Lines ◽  
Central Source ◽  
High Ionization ◽  
Orbital Cycle

ABSTRACT We present HST/STIS observations and analysis of two prominent nebular structures around the central source of η Carinae, the knots C and D. The former is brighter than the latter for emission lines from intermediate- or high-ionization potential ions. The brightness of lines from intermediate- and high-ionization potential ions significantly decreases at phases around periastron. We do not see conspicuous changes in the brightness of lines from low-ionization potential (<13.6 eV) ions over the orbital period. Line ratios suggest that the total extinction towards the Weigelt structures is AV = 2.0. Weigelt C and D are characterized by an electron density of 106.9 cm−3 that does not significantly change throughout the orbital cycle. The electron temperature varies from 5500 (around periastron) to 7200 K (around apastron). The relative changes in the brightness of the He i lines are well reproduced by the variations in the electron temperature alone. We found that, at phases around periastron, the electron temperature seems to be higher for Weigelt C than that of D. The Weigelt structures are located close to the Homunculus equatorial plane, at a distance of about 1240 au from the central source. From the analysis of proper motion and age, the Weigelt complex can be associated with the equatorial structure called ‘Butterfly Nebula’ surrounding the central binary system.

scholarly journals The multiple system Sk-67°18 in the LMC

1995 ◽  
Vol 163 ◽  
pp. 251-253 ◽  
Author(s):  
V. S. Niemela ◽  
W. Seggewiss ◽  
A. F. J. Moffat
Keyword(s):  
Binary System ◽  
Radial Velocity ◽  
Spectral Type ◽  
Orbital Period ◽  
Large Magellanic Cloud ◽  
Primary Component ◽  
Magellanic Cloud ◽  
Bright Star ◽  
High Mass ◽  
Eclipsing Binary

The bright star Sk—67°18 (Brey 5) in the Large Magellanic Cloud (LMC) contains an eclipsing binary system. Our radial velocity study reveals that the orbital period is almost exactly two days. The spectra also show that the star's primary component is not of spectral type WN, but that the star is rather an Of+O type binary where the primary is probably of type O3f*. Furthermore, Sk—67°18 appears to be a high-mass multiple system.

scholarly journals Multiwavelength Variability in the Symbiotic Nova V1016 CYG

2004 ◽  
Vol 194 ◽  
pp. 224-224
Author(s):  
Š. Parimucha ◽  
M. Vańko
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Orbital Period ◽  
Uv Spectroscopy ◽  
Infrared Photometry ◽  
Symbiotic System ◽  
Photoelectric Photometry ◽  
Mira Variable ◽  
Multiwavelength Variability

Analysis of the optical and infrared photometry together with UV spectroscopy led to discovery of the 15-years periodicity in the symbiotic system V1016 Cyg. This period could be interpreted as a orbital period in the binary system consisting of the Mira variable and the hot white dwarf.We have analyzed long-term optical photographic and UBV photoelectric photometry of V1016 Cyg. Collected observations cover pre- and post-outburst stages of the system. The light, curve suggests four stages of activity: the pre-out burst flare in 1949, the main nova-like outburst in 1904, and two post-outbursts, decreasing-amplitude flares in 1980 and 1994, respectively. Activity episodes affecting the system repeat with an interval of ~ 15 years. The ephemeris for the activity maxima is (see Parimucha et al., 2000).

Biperiodic orbital period modulation of the W UMa binary system CK Bootis

New Astronomy ◽  
2012 ◽  
Vol 17 (7) ◽  
pp. 667-672 ◽  
Author(s):  
Alexandru Pop ◽  
Călin Vamoş
Keyword(s):  
Binary System ◽  
Orbital Period

scholarly journals Orbital Period Change of the Eclipsing Binary System SZ Piscium

2010 ◽  
Vol 62 (3) ◽  
pp. 671-674 ◽  
Author(s):  
Xiao-Liang Wang ◽  
Fu-Yuan Xiang ◽  
Yong-Po Tian ◽  
Xiao-Min Shi
Keyword(s):  
Binary System ◽  
Orbital Period ◽  
Period Change ◽  
Eclipsing Binary

scholarly journals Fermi-LAT Observation of PSR B1259-63 during Its 2021 Periastron Passage

Universe ◽  
2021 ◽  
Vol 7 (12) ◽  
pp. 472
Author(s):  
Zhi Chang ◽  
Shu Zhang ◽  
Yu-Peng Chen ◽  
Long Ji ◽  
Ling-Da Kong ◽  
...  
Keyword(s):  
Binary System ◽  
Orbital Period ◽  
Compact Object ◽  
Peak Time ◽  
Γ Ray

PSR B1259-63 is a γ-ray binary system, where the compact object is a pulsar. The system has an orbital period of 1236.7 days and shows peculiar γ-ray flares (in 100 MeV–300 GeV) after its periastron time. We analyzed the Fermi-LAT observation of PSR B1259-63 during its latest periastron passage, as well as its previous three periastrons. The bright GeV flares started about 60 days after the periastron epoch in 2021. This delay is larger than that around the 2017 periastron and much larger than earlier periastrons. The delay of the GeV flux peak time in each periastron passage is apparent in our results. We discussed the possible origin of this delay and made a prediction of the GeV flux peak time in next periastron passage, based on observation of the previous delays.

scholarly journals Light curve analysis of the eclipsing binary system V781 Tau

2021 ◽  
Vol 2145 (1) ◽  
pp. 012005
Author(s):  
N Lamlert ◽  
W Maithong
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Orbital Period ◽  
Binary Systems ◽  
Curve Analysis ◽  
Photometric System ◽  
Light Curve Analysis ◽  
Eclipsing Binary ◽  
The Public ◽  
Secondary Star

Abstract V781 Tau is one of W UMa eclipsing binary systems whose orbital period is 0.34 days. The 0.7-meter telescope with CCD photometric system in B and V filters was conducted at the Regional Observatory for the Public, Chachoengsao, Thailand during December 2018, UT. The Wilson-Devinney Technique was used for calculating the physical properties of V781 Tau. The results showed the inclination of their orbital is 66.140°±0.14. The effective temperature of the primary and secondary star is 6,060 and 5,881 K, respectively and the degree of contact is 4.38 %

scholarly journals Wavelet Analysis of Some Pulsating Stars

1993 ◽  
Vol 137 ◽  
pp. 761-763
Author(s):  
Károly Szatmáry ◽  
János Gál
Keyword(s):  
Binary System ◽  
Wavelet Analysis ◽  
Light Curve ◽  
Orbital Period ◽  
Fourier Spectrum ◽  
Time Effect ◽  
Mode Switching ◽  
Pulsating Stars ◽  
Variable Period

The detection of a variable period is very important as it gives information on the evolutionary state or on the binary nature of a pulsating star. If a pulsator is moving in a binary system, its light curve is frequency-modulated by the orbital period (light-time effect). Mode switching or chaos also may be the cause of the changes in the amplitude and period of the light variations.The determination of period variability is difficult. Usually the conventional Fourier-spectrum cannot give any information about a possible period variation. The 0-C diagram is useful to detect a variable period, but it does not give the amplitude and phase values.

Sign in / Sign up

Export Citation Format

Share Document