53 research outputs found
The first light-curve analysis of eclipsing binaries observed by the INTEGRAL/OMC
Three Algol-type binaries in Cygnus constellation were selected for an
analysis from a huge database of observations made by the INTEGRAL/OMC camera.
These data were processed and analyzed, resulting in a first light-curve study
of these neglected eclipsing binaries. The temperatures of the primary
components range from 9500 K to 10500 K and the inclinations are circa 73deg
(for PV Cyg and V1011 Cyg), while almost 90deg for V822 Cyg. All of them seem
to be main-sequence stars, well within their critical Roche lobes.
Nevertheless, further detailed analyses are still needed.Comment: 6 pages, 4 figures, 2 tables, published in New As
Period changes in six semi-detached Algol-type binaries
Six semi-detached Algol-type binaries lacking a period analysis were chosen
to test for a presence of a third body. The O-C diagrams of these binaries were
analyzed with the least-squares method by using all available times of minima.
Also fourteen new minima, obtained from our observations, were included in the
present research. The light-time effect was adopted as a main factor for the
detailed description of the long-term period changes. Third bodies were found
with orbital periods from 46 up to 84 years, and eccentricities from 0.0 to
0.78 for the selected binaries. The mass functions and the minimal masses of
such bodies were also calculated.Comment: 14 pages, 8 figure
A Tight Upper Limit on Oscillations in the Ap star Epsilon Ursae Majoris from WIRE Photometry
Observations of Epsilon UMa obtained with the star tracker on the Wide Field
Infrared Explorer (WIRE) satellite during a month in mid-2000 are analyzed.
This is one of the most precise photometry of an Ap star. The amplitude
spectrum is used to set an upper limit of 75 parts per million for the
amplitude of stellar pulsations in this star unless it accidentally oscillates
with a single mode at the satellite orbit, its harmonics or their one day
aliases. This is the tightest limit put on the amplitude of oscillations in an
Ap star. As the rotation period of Epsilon UMa is relatively short (5.1 d), it
cannot be argued that the observations were made at a wrong rotational phase.
Our results thus support the idea that some Ap stars do not pulsate at all.Comment: 4 pages, 4 figures, 2 style files, accepted for publication in ApJ
Radial Velocity Studies of Close Binary Stars. XI
Radial-velocity measurements and sine-curve fits to the orbital radial
velocity variations are presented for ten close binary systems: DU Boo, ET Boo,
TX Cnc, V1073 Cyg, HL Dra, AK Her, VW LMi, V566 Oph, TV UMi and AG Vir. By this
contribution, the DDO program has reached the point of 100 published radial
velocity orbits. The radial velocities have been determined using an improved
fitting technique which uses rotational profiles to approximate individual
peaks in broadening functions.
Three systems, ET Boo, VW LMi and TV UMi, were found to be quadruple while AG
Vir appears to be a spectroscopic triple. ET Boo, a member of a close visual
binary with years, was previously known to be a multiple
system, but we show that the second component is actually a close,
non-eclipsing binary. The new observations enabled us to determine the
spectroscopic orbits of the companion, non-eclipsing pairs in ET Boo and VW
LMi. The particularly interesting case is VW LMi, where the period of the
mutual revolution of the two spectroscopic binaries is only 355 days.
While most of the studied eclipsing pairs are contact binaries, ET Boo is
composed of two double-lined detached binaries and HL Dra is single-lined
detached or semi-detached system. Five systems of this group were observed
spectroscopically before: TX Cnc, V1073 Cyg, AK Her (as a single-lined binary),
V566 Oph, AG Vir, but our new data are of much higher quality than the previous
studies.Comment: Accepted by AJ, August 2006, 10 figures, 3 table
Asteroseismology of the Beta Cephei star 12 (DD) Lacertae: photometric observations, pulsational frequency analysis and mode identification
We report a multisite photometric campaign for the Beta Cephei star 12
Lacertae. 750 hours of high-quality differential photoelectric Stromgren,
Johnson and Geneva time-series photometry were obtained with 9 telescopes
during 190 nights. Our frequency analysis results in the detection of 23
sinusoidal signals in the light curves. Eleven of those correspond to
independent pulsation modes, and the remainder are combination frequencies. We
find some slow aperiodic variability such as that seemingly present in several
Beta Cephei stars. We perform mode identification from our colour photometry,
derive the spherical degree l for the five strongest modes unambiguously and
provide constraints on l for the weaker modes. We find a mixture of modes of 0
<= l <= 4. In particular, we prove that the previously suspected rotationally
split triplet within the modes of 12 Lac consists of modes of different l;
their equal frequency splitting must thus be accidental.
One of the periodic signals we detected in the light curves is argued to be a
linearly stable mode excited to visible amplitude by nonlinear mode coupling
via a 2:1 resonance. We also find a low-frequency signal in the light
variations whose physical nature is unclear; it could be a parent or daughter
mode resonantly coupled. The remaining combination frequencies are consistent
with simple light-curve distortions.
The range of excited pulsation frequencies of 12 Lac may be sufficiently
large that it cannot be reproduced by standard models. We suspect that the star
has a larger metal abundance in the pulsational driving zone, a hypothesis also
capable of explaining the presence of Beta Cephei stars in the LMC.Comment: 12 pages, 7 figures, MNRAS, in pres
V456 Ophiuchi and V490 Cygni: Systems with the shortest apsidal-motion periods
Our main aim is the first detailed analysis of the two eclipsing binaries
V456 Oph and V490 Cyg. The system V456 Oph has been studied both
photometrically via an analysis of its light curve observed by the INTEGRAL/OMC
and by the period analysis of all available times of minima. V490 Cyg has been
studied by means of a period analysis only. Many new times of minima for both
systems have recently been observed and derived. This allows us for the first
time to study in detail the processes that affect both binaries. The main
result is the discovery that both systems have eccentric orbits. For V456 Oph
we deal with the eccentric eclipsing binary system with the shortest orbital
period known (about 1.016 day), while the apsidal motion period is about 23
years. V490 Cyg represents the eclipsing system with the shortest apsidal
motion period (about 18.8 years only). The two components of V456 Oph are
probably of spectral type F. We compare and discuss the V456 Oph results from
the light curve and the period analysis, but a more detailed spectroscopy is
needed to confirm the physical parameters of the components more precisely.Comment: 4 pages, 3 figures, published in A&A: 2011A&A...527A..43
Catalog of Galactic Beta Cephei Stars
We present an extensive and up-to-date catalog of Galactic Beta Cephei stars.
This catalog is intended to give a comprehensive overview of observational
characteristics of all known Beta Cephei stars. 93 stars could be confirmed to
be Beta Cephei stars. For some stars we re-analyzed published data or conducted
our own analyses. 61 stars were rejected from the final Beta Cephei list, and
77 stars are suspected to be Beta Cephei stars. A list of critically selected
pulsation frequencies for confirmed Beta Cephei stars is also presented. We
analyze the Beta Cephei stars as a group, such as the distributions of their
spectral types, projected rotational velocities, radial velocities, pulsation
periods, and Galactic coordinates. We confirm that the majority of these stars
are multiperiodic pulsators. We show that, besides two exceptions, the Beta
Cephei stars with high pulsation amplitudes are slow rotators. We construct a
theoretical HR diagram that suggests that almost all 93 Beta Cephei stars are
MS objects. We discuss the observational boundaries of Beta Cephei pulsation
and their physical parameters. We corroborate that the excited pulsation modes
are near to the radial fundamental mode in frequency and we show that the mass
distribution of the stars peaks at 12 solar masses. We point out that the
theoretical instability strip of the Beta Cephei stars is filled neither at the
cool nor at the hot end and attempt to explain this observation
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