Detection of Sectoral Modes in the Eclipsing Binary KIC 4851217

2017 ◽  
Vol 14 (S339) ◽  
pp. 295-298
Author(s):  
M. Fedurco ◽  
Š. Parimucha ◽  
P. Gajdoš
Keyword(s):  
Light Curve ◽  
Frequency Analysis ◽  
Secondary Component ◽  
Frequency Range ◽  
Eclipsing Binary ◽  
Quadrupole Mode ◽  
Linear Coupling ◽  
Orbital Frequency ◽  
Short Period ◽  
Low Amplitude

AbstractKIC 4851217 is a short period eclipsing binary (P = 2.47 days) in the field of the Kepler K1 mission. As well as variability caused by the eclipses, low-amplitude pulsations are also present in the data. A frequency analysis of the residual light-curve revealed δ Sct pulsations in the frequency range from 15–21 d−1 with amplitudes up to 3.5 mmag. Strong linear coupling (fi = fp + kforb) to orbital frequency was found, indicating tidally locked modes. From an analysis of 5 selected groups of frequencies we identified a radial mode on the secondary component, 3 dipole modes (l = |m| = 1), one of them present on the secondary component, and a quadrupole mode (l = |m| = 2), also located on the secondary component.

scholarly journals Discovery of β Cep pulsations in the eclipsing binary V453 Cygni

2020 ◽  
Vol 497 (1) ◽  
pp. L19-L23 ◽  
Author(s):  
John Southworth ◽  
D M Bowman ◽  
A Tkachenko ◽  
K Pavlovski
Keyword(s):  
Physical Properties ◽  
Satellite Data ◽  
Binary Stars ◽  
Mass Measurement ◽  
Physical Processes ◽  
Primary Star ◽  
Eclipsing Binary ◽  
Period Orbit ◽  
Orbital Frequency ◽  
Short Period

ABSTRACT V453 Cyg is an eclipsing binary containing 14 and 11 $\, {\rm M}_\odot$ stars in an eccentric short-period orbit. We have discovered β Cep-type pulsations in this system using Transiting Exoplanet Survey Satellite data. We identify seven significant pulsation frequencies, between 2.37 and 10.51 d−1, in the primary star. These include six frequencies that are separated by yet significantly offset from harmonics of the orbital frequency, indicating they are tidally perturbed modes. We have determined the physical properties of the system to high precision: V453 Cyg A is the first β Cep pulsator with a precise mass measurement. The system is a vital tracer of the physical processes that govern the evolution of massive single and binary stars.

scholarly journals Epsilon Aurigae: A Supergiant and a Super Disk

1989 ◽  
Vol 107 ◽  
pp. 336-336
Author(s):  
Sean Carroll ◽  
Edward Guinan ◽  
George McCook ◽  
Robert Donahue
Keyword(s):  
Light Curve ◽  
Orbital Period ◽  
Instability Strip ◽  
Eclipsing Binary ◽  
Characteristic Period ◽  
Photoelectric Observations ◽  
Low Amplitude ◽  
Epsilon Aurigae ◽  
Villanova University

The eclipsing binary Epsilon Aurigae consists of an F0 supergiant and a cool, mysterious eclipsing companion with an orbital period of 27.1 years. The light curve of this system reveals two sources of variability: the eclipses themselves and the intrinsic variation of the supergiant. Multifilter photoelectric observations were made with the 38 cm reflector at the Villanova University Observatory. These data were analyzed along with other sources to reveal the nature of the components of the Epsilon Aurigae system. The system undergoes low-amplitude semi-regular light variations with a characteristic period of 110 days and perhaps a longer period of 500-600 days. The proximity of Epsilon Aur to the Cepheid instability strip on the H-R diagram suggests that the pulsation mechanism for this star may be similar to that of Cepheids.

scholarly journals KIC 10486425: A Kepler eclipsing binary system with a pulsating component

2013 ◽  
Vol 9 (S301) ◽  
pp. 433-434 ◽  
Author(s):  
Filiz Kahraman Aliçavuş ◽  
Esin Soydugan
Keyword(s):  
Binary System ◽  
Fourier Analysis ◽  
Light Curve ◽  
Frequency Analysis ◽  
Dominant Frequency ◽  
Eclipsing Binary

AbstractWe present frequency analysis of the Kepler light curve of KIC 10486425, an eclipsing binary system with a pulsating component. The parameters of the binary were obtained by modelling the light curve with the Wilson-Devinney program. The residuals from this modelling were subject to Fourier analysis which allowed us to detect 120 periodic terms characteristic for γ Dor-type pulsations. The dominant frequency of these changes amounts to 1.3189 d−1.

scholarly journals Spot evolution in the eclipsing binary CoRoT 105895502

2019 ◽  
Vol 623 ◽  
pp. A107 ◽  
Author(s):  
S. Czesla ◽  
S. Terzenbach ◽  
R. Wichmann ◽  
J. H. M. M. Schmitt
Keyword(s):  
Light Curve ◽  
Binary Systems ◽  
Temporal Behavior ◽  
Mass Ratio ◽  
Late Type ◽  
Stellar Rotation ◽  
Orbital Inclination ◽  
Eclipsing Binary ◽  
Short Period ◽  
Curve Modeling

Stellar activity is ubiquitous in late-type stars. The special geometry of eclipsing binary systems is particularly advantageous to study the stellar surfaces and activity. We present a detailed study of the 145 d CoRoT light curve of the short-period (2.17 d) eclipsing binary CoRoT 105895502. By means of light-curve modeling with Nightfall, we determine the orbital period, effective temperature, Roche-lobe filling factors, mass ratio, and orbital inclination of CoRoT 105895502 and analyze the temporal behavior of starspots in the system. Our analysis shows one comparably short-lived (≈40 d) starspot, remaining quasi-stationary in the binary frame, and one starspot showing prograde motion at a rate of 2.3° day−1, whose lifetime exceeds the duration of the observation. In the CoRoT band, starspots account for as much as 0.6% of the quadrature flux of CoRoT 105895502, however we cannot attribute the spots to individual binary components with certainty. Our findings can be explained by differential rotation, asynchronous stellar rotation, or systematic spot evolution.

Light curve analysis of the short period eclipsing binary RT and

1979 ◽  
Vol 66 (2) ◽  
pp. 475-486 ◽  
Author(s):  
S. Mancuso ◽  
L. Milano ◽  
G. Russo ◽  
C. Sollazzo
Keyword(s):  
Light Curve ◽  
Curve Analysis ◽  
Light Curve Analysis ◽  
Eclipsing Binary ◽  
Short Period

scholarly journals PROPERTIES OF THE RECENTLY DISCOVERED ECLIPSING BINARY GSC 03421-01402

2021 ◽  
pp. 1-11
Author(s):  
Christopher Lloyd, ◽  
James Screech,
Keyword(s):  
Light Curve ◽  
Eclipsing Binary ◽  
Close Pair ◽  
Low Amplitude

GSC 03421-01402 is a low-amplitude eclipsing binary with a period of 7.6800475(44) d. The eclipsing binary is one component of a close pair identified in the Gaia EDR3 data with ∆G = 0.m45. The light-curve suggests that the primary eclipse is total with an observed depth of 0.m13, but due to dilution the true depth could be ∼ 0.23 or 0.37 mag. A weak, 0.02 mag, secondary eclipse is seen displaced slightly to phase 0.491. The system is probably a detached Algol-type eclipsing binary dominated by a mid G-type primary, but until the uncertainties in the relative magnitudes and distance are resolved much remains in doubt.

scholarly journals A new B-subdwarf eclipsing binary with an extremely short period

1986 ◽  
Vol 118 ◽  
pp. 305-306 ◽  
Author(s):  
J W Menzies ◽  
F Marang
Keyword(s):  
Light Curve ◽  
Preliminary Analysis ◽  
Eclipsing Binary ◽  
Common Envelope ◽  
Short Period

The B-type Subdwarf BD-07°3477 has been found to be an eclipsing binary with a period of about 2h48m. A preliminary analysis of the light curve reveals the system to be fully detached. It appears to be similar in many respects to the O-Subdwarf binary AA Dor which is thought to be the remnant of a system which has undergone a common envelope phase of evolution.

scholarly journals An extreme-mass ratio, short-period eclipsing binary consisting of a B dwarf primary and a pre-main-sequence M star companion discovered by KELT

2020 ◽  
Vol 499 (3) ◽  
pp. 3775-3791
Author(s):  
Daniel J Stevens ◽  
George Zhou ◽  
Marshall C Johnson ◽  
Aaron C Rizzuto ◽  
Joseph E Rodriguez ◽  
...  
Keyword(s):  
Light Curve ◽  
Global Analysis ◽  
Binary Star ◽  
Spectral Energy Distribution ◽  
Broad Band ◽  
Phase Curve ◽  
Mass Ratio ◽  
Eclipsing Binary ◽  
Short Period ◽  
Low Mass

ABSTRACT We present the discovery of KELT J072709 + 072007 (HD 58730), a very low mass ratio (q ≡ M2/M1 ≈ 0.07) eclipsing binary (EB) identified by the Kilodegree Extremely Little Telescope (KELT) survey. We present the discovery light curve and perform a global analysis of four high-precision ground-based light curves, the Transiting Exoplanets Survey Satellite (TESS) light curve, radial velocity (RV) measurements, Doppler Tomography (DT) measurements, and the broad-band spectral energy distribution. Results from the global analysis are consistent with a fully convective ($M_2 = 0.22 \pm 0.02\ \, \mathrm{M}_{\odot })$ M star transiting a late-B primary ($M_1 = 3.34^{+0.07}_{-0.09}\ \, \mathrm{M}_{\odot }\,\mathrm{ and}\,\ T_{\rm eff,1} = 11960^{+430}_{-520}\ {\rm K}$). We infer that the primary star is $183_{-30}^{+33}$ Myr old and that the companion star’s radius is inflated by $26 \pm 8{{\ \rm per\ cent}}$ relative to the predicted value from a low-mass isochrone of similar age. We separately and analytically fit for the variability in the out-of-eclipse TESS phase curve, finding good agreement between the resulting stellar parameters and those from the global fit. Such systems are valuable for testing theories of binary star formation and understanding how the environment of a star in a close-but-detached binary affects its physical properties. In particular, we examine how a star’s properties in such a binary might differ from the properties it would have in isolation.

scholarly journals KIC 7385478: An Eclipsing Binary with a γ Doradus Component

2017 ◽  
Vol 34 ◽  
Author(s):  
Orkun Özdarcan ◽  
Hasan Ali Dal
Keyword(s):  
Light Curve ◽  
Orbital Period ◽  
Spectroscopic Data ◽  
Primary Component ◽  
Secondary Component ◽  
Photometric Analysis ◽  
Eclipsing Binary ◽  
Cool Star ◽  
Star Activity ◽  
Dominant Period

AbstractWe present spectroscopic and photometric analysis of the eclipsing binary KIC 7385478. We find that the system is formed by F1V + K4III–IV components. Combining results from analysis of spectroscopic data and Kepler photometry, we calculate masses and radii of the primary and the secondary components as M1 = 1.71 ± 0.08 M⊙, M2 = 0.37 ± 0.04 M⊙ and R1 = 1.59 ± 0.03 R⊙, R2 = 1.90 ± 0.03 R⊙, respectively. Position of the primary component in HR diagram is in the region of γ Doradus type pulsators and residuals from light curve modelling exhibit additional light variation with a dominant period of ~ 0.5 d. These are clear evidences of the γ Doradus type pulsations on the primary component. We also observe occasional increase in amplitude of the residuals, where the orbital period becomes the most dominant period. These may be attributed to the cool star activity originating from the secondary component.

scholarly journals Mass transfer and stellar wind effects in the eclipsing binary RT Andromedae

1981 ◽  
Vol 59 ◽  
pp. 491-494
Author(s):  
G.A. Bakos ◽  
J. Tremko
Keyword(s):  
Mass Transfer ◽  
Light Curve ◽  
Spectral Type ◽  
Orbital Period ◽  
Stellar Wind ◽  
Mass Ratio ◽  
Eclipsing Binary ◽  
Short Period ◽  
Photometric Elements ◽  
Number Of Authors

In recent years the short period eclipsing binary RT And has been studied extensively by a number of authors. From photo electric observations the light curve and the photometric elements were derived by Dean (1974) and Mancuso et al. (1979). The geometric dimensions of the binary confirm that the system is detached consisting of two stars of spectral type F8 V and KO V. The mass ratio is 0.66. In spite of this classification, effects appearing among semidetached systems have been observed, namely, variations of the amplitude and the shape of the light curve and changes of the length of the orbital period.

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