252 research outputs found
A unified solution for the orbit and light-time effect in the V505 Sgr system
The multiple system V505 Sagittarii is composed of at least three stars: a
compact eclipsing pair and a distant component, which orbit is measured
directly using speckle interferometry. In order to explain the observed orbit
of the third body in V505 Sagittarii and also other observable quantities,
namely the minima timings of the eclipsing binary and two different radial
velocities in the spectrum, we thoroughly test a fourth-body hypothesis - a
perturbation by a dim, yet-unobserved object. We use an N-body numerical
integrator to simulate future and past orbital evolution of 3 or 4 components
in this system. We construct a suitable chi^2 metric from all available
speckle-interferometry, minima-timings and radial-velocity data and we scan a
part of a parameter space to get at least some of allowed solutions. In
principle, we are able to explain all observable quantities by a presence of a
fourth body, but the resulting likelihood of this hypothesis is very low. We
also discuss other theoretical explanations of the minima timings variations.
Further observations of the minima timings during the next decade or
high-resolution spectroscopic data can significantly constrain the model
Eclipsing Binaries Showing Light Time Effect
Four eclipsing binaries, which show apparent changes of period, have been
studied with respect to a possible presence of the light time effect. With a
least squares method we calculated new light elements of these systems, the
mass function of the predicted third body, and its minimum mass. We discuss the
probability of the presence of such bodies in terms of mass function, changes
in radial velocity and third light in solution of light curves.Comment: 4 pages, 4 figures, 1 table, conference proceeding
ASDEX Upgrades New Plasma Control Scheme
ASDEX Upgrade is a medium sized tokamak experiment investigating highly shaped plasma and advanced scenarios to be extrapolated for ITER. Eleven independent magnetic coils allow for proper shaping and plasma current control. For plasma heating and current drive eight NBI beam lines, two ICRH antenna pairs and four ECRH gyrotrons are available. Five channels for controlling gas valves and a pellet injector serve for fuelling. All actuators are driven by a digital discharge control system. One basic enhancement of the latest generation is a unified framework for all feedforward and feedback control tasks in a discharge. The framework consists of two layers. The core layer implements wind-up safe feedback controllers with a collection of overlayed output limitations. Each controller is dynamically switchable in references, controlled variables, control law and control parameters via a control mode. The coordination layer implements intelligent discharge protection or optimisation algorithms which synchronously can change control modes and dynamically can generate reference waveforms adapted to the discharge's state and goal. The core layer comprises the backbone of plasma control. Current, shape, heating and fuel control all use a library of highly configurable single- and multivalriable control laws. P, PI and PID controllers are standard components but state space and sliding mode policies can easily be supplemented, too. Likewise, a broad selection of output limiters is available in the library. It ranges from constant values to rate limiters, and multi-signal dependent polynomial characteristics. The controller is aware of any output limitation and can take anti-wind-up measures. Furthermore, a feedforward policy allows to tune the behaviour upon mode transitions, like smooth adaptation or freezing the last output. With the coordination layer, tasks like marfe protection, power exhaust protection and soft pulse termination are accomplished. These specialised algorithms are plugged into the framework using a common interface. The framework approach easily allows for further extensions and opens a door for future experimental investigations
New inclination changing eclipsing binaries in the Magellanic Clouds
Context: Multiple stellar systems are unique laboratories for astrophysics.
Analysis of their orbital dynamics may reveal invaluable information about the
physical properties of the participating stars. Unfortunately, there are only a
few known and well described multiple systems, this is even more so for systems
located outside the Milky Way galaxy. A particularly interesting situation
occurs when the inner binary in a compact triple system is eclipsing. This is
because the stellar interaction, typically resulting in precession of orbital
planes, may be observable as a variation of depth of the eclipses on a long
timescale. Aims: We aim to present a novel method to determine compact triples
using publicly available photometric data from large surveys. Here we apply it
to eclipsing binaries (EBs) in Magellanic Clouds from OGLE III database.
Methods: We analyzed light curves (LCs) of 26121 LMC and 6138 SMC EBs with the
goal to identify those for which the orbital inclination varies in time.
Archival LCs of the selected systems, when complemented by our own observations
with Danish 1.54m telescope, were thoroughly analyzed using the PHOEBE program.
Time dependence of the EB's inclination was described using the theory of
orbital-plane precession. By observing the parameter-dependence of the
precession rate, we were able to constrain the third companion mass and its
orbital period around EB. Results: We identified 58 candidates of new compact
triples in Magellanic Clouds. This is the largest published sample of such
systems so far. Eight of them were analyzed thoroughly and physical parameters
of inner binary were determined together with an estimation of basic
characteristics of the third star. These data may provide important clues about
stellar formation mechanisms for objects with different metalicity than found
in our galactic neighborhood.Comment: Accepted for publication in Astronomy and Astrophysic
Time-dependent spectral-feature variations of stars displaying the B[e] phenomenon III. HD 50138
We analyse spectroscopic observations of the B[e] star HD 50138 (MWC 158,
V743 Mon, or IRAS 06491-0654), a member of the FS CMa group, obtained over the
last twenty years. Four different epochs are identified in the observational
data, where the variability of the spectral features is substantially
different. Additionally, two long periods of (3 000 +/- 500) and (5 000 +/-
1000) days are found in the variations of the equivalent widths of the H alpha
and [OI] 6300 A lines and radial velocities of the H alpha line violet peak.
Modest signatures of a regular period of ~34 days in the radial velocities of
the H alpha red peak and H beta central depression are found in the season
2013/2014. The H alpha V/R changes indicate a periodicity of ~50 days. The
correlations between individual spectral features significantly restricts the
model of the object and suggest that it is most likely a binary system with a
highly distorted disc with spiral arms around the primary component. At the
same time, no obvious signs of the secondary component has been found in the
object's spectrum
Improved model of the triple system V746 Cas that has a bipolar magnetic field associated with the tertiary
V746 Cas is known to be a triple system composed of a close binary with an
alternatively reported period of either 25.4d or 27.8d and a third component in
a 62000d orbit. The object was also reported to exhibit multiperiodic light
variations with periods from 0.83d to 2.50d, on the basis of which it was
classified as a slowly pulsating B star. Interest in further investigation of
this system was raised by the detection of a variable magnetic field. Analysing
spectra from four instruments, earlier published radial velocities, and several
sets of photometric observations, we arrived at the following conclusions: (1)
The optical spectrum is dominated by the lines of the B-type primary
(Teff1~16500(100) K), contributing 70% of the light in the optical region, and
a slightly cooler B tertiary (Teff3~13620(150) K). The lines of the low-mass
secondary are below our detection threshold; we estimate that it could be a
normal A or F star. (2) We resolved the ambiguity in the value of the inner
binary period and arrived at a linear ephemeris of T_super.conj.=HJD
2443838.78(81)+25.41569(42)xE. (3) The intensity of the magnetic field
undergoes a~sinusoidal variation in phase with one of the known photometric
periods, namely 2.503867(19)d, which we identify with the rotational period of
the tertiary. (4) The second photometric 1.0649524(40)d period is identified
with the rotational period of the B-type primary, but this interpretation is
much less certain and needs further verification. (5) If our interpretation of
photometric periods is confirmed, the classification of the object as a slowly
pulsating B star should be revised. (6) Applying an N-body model to different
types of available observational data, we constrain the orbital inclination of
the inner orbit to ~60 deg to 85 deg even in the absence of eclipses, and
estimate the probable properties of the triple system and its components.Comment: Accepted for publication in Astronomy and Astrophysic
Properties and nature of Be stars 30. Reliable physical properties of a semi-detached B9.5e+G8III binary BR CMi = HD 61273 compared to those of other well studied semi-detached emission-line binaries
Reliable determination of the basic physical properties of hot emission-line
binaries with Roche-lobe filling secondaries is important for developing the
theory of mass exchange in binaries. It is a very hard task, however, which is
complicated by the presence of circumstellar matter in these systems. So far,
only a small number of systems with accurate values of component masses, radii,
and other properties are known. Here, we report the first detailed study of a
new representative of this class of binaries, BR CMi, based on the analysis of
radial velocities and multichannel photometry from several observatories, and
compare its physical properties with those for other well-studied systems. BR
CMi is an ellipsoidal variable seen under an intermediate orbital inclination
of ~51 degrees, and it has an orbital period of 12.919059(15) d and a circular
orbit. We used the disentangled component spectra to estimate the effective
temperatures 9500(200) K and 4655(50) K by comparing them with model spectra.
They correspond to spectral types B9.5e and G8III. We also used the
disentangled spectra of both binary components as templates for the 2-D
cross-correlation to obtain accurate RVs and a reliable orbital solution. Some
evidence of a secular period increase at a rate of 1.1+/-0.5 s per year was
found. This, together with a very low mass ratio of 0.06 and a normal mass and
radius of the mass gaining component, indicates that BR CMi is in a slow phase
of the mass exchange after the mass-ratio reversal. It thus belongs to a still
poorly populated subgroup of Be stars for which the origin of Balmer emission
lines is safely explained as a consequence of mass transfer between the binary
components.Comment: 17 pages, 5 figures, accepted for publication in Astronomy and
Astrophysics. appears in Astronomy and Astrophysics 201
- …