509 research outputs found
Asteroseismology with the WIRE satellite
I give a summary of results from the WIRE satellite, which has been used to
observe bright stars from 1999-2000 and 2003-2006. The WIRE targets are
monitored for up to five weeks with a duty cycle of 30-40%. The aim has been to
characterize the flux variation of stars across the Hertzsprung-Russell
diagram. I present an overview of the results for solar-like stars, delta Scuti
stars, giant stars, and eclipsing binaries.Comment: Accepted for publication in CoAst. Proceedings of the Vienna Workshop
on the Future of Asteroseismology (September 2006). 8 pages, 2 figure
Evidence of resonant mode coupling and the relationship between low and high frequencies in a rapidly rotating A star
In the theory of resonant mode coupling, the parent and child modes are
directly related in frequency and phase. The oscillations present in the fast
rotating Delta Scuti star KIC 8054146 allow us to test the most general and
generic aspects of such a theory. The only direct way to separate the parent
and coupled (child) modes is to examine the correlations in amplitude
variability between the different frequencies. For the dominant family of
related frequencies, only a single mode and a triplet are the origins of nine
dominant frequency peaks ranging from 2.93 to 66.30 cycles per day (as well as
dozens of small-amplitude combination modes and a predicted and detected third
high-frequency triplet). The mode-coupling model correctly predicts the large
amplitude variations of the coupled modes as a product of the amplitudes of the
parent modes, while the phase changes are also correctly modeled. This differs
from the behavior of 'normal' combination frequencies in that the amplitudes
are three orders of magnitude larger and may exceed even the amplitudes of the
parent modes. We show that two dominant low frequencies at 5.86 and 2.93 cycles
per day in the gravity-mode region are not harmonics of each other, and their
properties follow those of the almost equidistant high-frequency triplet. We
note that the previously puzzling situation of finding two strong peaks in the
low-frequency region related by nearly a factor of two in frequency has been
seen in other Delta Scuti stars as well.Comment: To be published in the Astrophysical Journa
Pulsation of EE Cam
EE Cam is a previously little studied Delta Scuti pulsator with amplitudes
between those of the HADS (High-Amplitude Delta Scuti stars) group and the
average low-amplitude pulsators. Since the size of stellar rotation determines
both which pulsation modes are selected by the star as well as their
amplitudes, the star offers a great opportunity to examine the astrophysical
connections. Extensive photometric measurements covering several months were
carried out. 15 significant pulsation frequencies were extracted. The dominant
mode at 4.934 cd was identified as a radial mode by examining the phase
shifts at different wavelengths. Medium-dispersion spectra yielded a
value of km s. This shows that EE Cam belongs to the
important transition region between the HADS and normal Delta Scuti stars.Comment: 13 pages, 3 figures, 3 table
A new method for the spectroscopic identification of stellar non-radial pulsation modes. II. Mode identification of the Delta Scuti star FG Virginis
We present a mode identification based on new high-resolution time-series
spectra of the non-radially pulsating Delta Scuti star FG~Vir (HD 106384, V =
6.57, A5V). From 2002 February to June a global Delta Scuti Network (DSN)
campaign, utilizing high-resolution spectroscopy and simultaneous photometry
has been conducted for FG~Vir in order to provide a theoretical pulsation
model. In this campaign we have acquired 969 Echelle spectra covering 147 hours
at six observatories. The mode identification was carried out by analyzing line
profile variations by means of the Fourier parameter fit method, where the
observational Fourier parameters across the line are fitted with theoretical
values. This method is especially well suited for determining the azimuthal
order m of non-radial pulsation modes and thus complementary with the method of
Daszynska-Daszkiewicz (2002) which does best at identifying the degree l. 15
frequencies between 9.2 and 33.5 c/d were detected spectroscopically. We
determined the azimuthal order m of 12 modes and constrained their harmonic
degree l. Only modes of low degree (l <= 4) were detected, most of them having
axisymmetric character mainly due to the relatively low projected rotational
velocity of FG Vir. The detected non-axisymmetric modes have azimuthal orders
between -2 and 1. We derived an inclination of 19 degrees, which implies an
equatorial rotational rate of 66 km/s.Comment: 14 pages, 26 figure
A Quantitative Analysis of the Available Multicolor Photometry for Rapidly Pulsating Hot B Subdwarfs
We present a quantitative and homogeneous analysis of the broadband
multicolor photometric data sets gathered so far on rapidly pulsating hot B
subdwarf stars. This concerns seven distinct data sets related to six different
stars. Our analysis is carried out within the theoretical framework developed
by Randall et al., which includes full nonadiabatic effects. The goal of this
analysis is partial mode identification, i.e., the determination of the degree
index l of each of the observed pulsation modes. We assume possible values of l
from 0 to 5 in our calculations. For each target star, we compute a specific
model atmosphere and a specific pulsation model using estimates of the
atmospheric parameters coming from time-averaged optical spectroscopy. For
every assumed value of l, we use a formal chi-squared approach to model the
observed amplitude-wavelength distribution of each mode, and we compute a
quality-of-fit Q probability to quantify the derived fit and to discriminate
objectively between the various solutions. We find that no completely
convincing and unambiguous l identification is possible on the basis of the
available data, although partial mode discrimination has been reached for 25
out of the 41 modes studied. A brief statistical study of these results
suggests that a majority of the modes must have l values of 0, 1, and 2, but
also that modes with l = 4 could very well be present while modes with l = 3
appear to be rarer. This is in line with recent results showing that l = 4
modes in rapidly pulsating B subdwarfs have a higher visibility in the optical
domain than modes with l = 3. Although somewhat disappointing in terms of mode
discrimination, our results still suggest that the full potential of multicolor
photometry for l identification in pulsating subdwarfs is within reach.Comment: 59 pages, 18 figures, accepted for publication in the Astrophysical
Journal Supplement Serie
A photometric study of the newly discovered eclipsing cataclysmic variable SDSS J040714.78-064425.1
We present the results obtained from unfiltered photometric CCD observations
of the newly discovered cataclysmic variable SDSS J040714.78-064425.1 made
during 7 nights in November 2003. We establish the dwarf nova nature of the
object as it was in outburst during our observations. We also confirm the
presence of deep eclipses with a period of 0.17017d+/-0.00003 in the optical
light curve of the star. In addition, we found periods of 0.166d+/-0.001 and
possibly also 5.3d+/-0.7 in the data. The 0.17017d periodicity is consistent
within the errors with the proposed orbital period of 0.165d (Szkody et. al.
2003) and 0.1700d (Monard 2004). Using the known relation between the orbital
and superhump periods, we interpret the 0.166d and 5.3d periods as the negative
superhump and the nodal precession period respectively. SDSS
J040714.78-064425.1 is then classified as a negative superhump system with one
of the largest orbital periods.Comment: 6 pages, 8 figures. accepted by PAS
The Unique Frequency Spectrum of the Blazhko RRc Star LS Her
The Blazhko effect in RR Lyrae stars is still poorly understood
theoretically. Stars with multiple Blazhko periods or in which the Blazhko
effect itself varies are particularly challenging. This study investigates the
Blazhko effect in the RRc star LS Her. Detailed VRI CCD photometry has been
performed on 63 nights during six months. LS Her is confirmed to have a Blazhko
period of 12.75+/-0.02 days. However, where normally the side frequencies of
the Blazhko triplet are expected, an equidistant group of three frequencies is
found on both sides of the main pulsation frequency. As a consequence the
period and amplitude of the Blazhko effect itself vary in a cycle of 109+/-4
days. LS Her is a unique object turning out to be very important in the
verification of the theories for the Blazhko effect.Comment: Accepted for publication in MNRA
Spectra disentangling applied to the Hyades binary Theta^2 Tau AB: new orbit, orbital parallax and component properties
Theta^2 Tauri is a detached and single-lined interferometric-spectroscopic
binary as well as the most massive binary system of the Hyades cluster. The
system revolves in an eccentric orbit with a periodicity of 140.7 days. The
secondary has a similar temperature but is less evolved and fainter than the
primary. It is also rotating more rapidly. Since the composite spectra are
heavily blended, the direct extraction of radial velocities over the orbit of
component B was hitherto unsuccessful. Using high-resolution spectroscopic data
recently obtained with the Elodie (OHP, France) and Hermes (ORM, La Palma,
Spain) spectrographs, and applying a spectra disentangling algorithm to three
independent data sets including spectra from the Oak Ridge Observatory (USA),
we derived an improved spectroscopic orbit and refined the solution by
performing a combined astrometric-spectroscopic analysis based on the new
spectroscopy and the long-baseline data from the Mark III optical
interferometer. As a result, the velocity amplitude of the fainter component is
obtained in a direct and objective way. Major progress based on this new
determination includes an improved computation of the orbital parallax. Our
mass ratio is in good agreement with the older estimates of Peterson et al.
(1991, 1993), but the mass of the primary is 15-25% higher than the more recent
estimates by Torres et al. (1997) and Armstrong et al. (2006). Due to the
strategic position of the components in the turnoff region of the cluster,
these new determinations imply stricter constraints for the age and the
metallicity of the Hyades cluster. The location of component B can be explained
by current evolutionary models, but the location of the more evolved component
A is not trivially explained and requires a detailed abundance analysis of its
disentangled spectrum.Comment: in press, 13 pages, 10 Postscript figures, 5 tables. Table~4 is
available as online material. Keywords: astrometry - techniques: high angular
resolution - stars: binaries: visual - stars: binaries: spectroscopic -
stars: fundamental parameter
SPB stars in the open SMC cluster NGC 371
Pulsation in beta Cep and SPB stars are driven by the kappa mechanism which
depends critically on the metallicity. It has therefore been suggested that
beta Cep and SPB stars should be rare in the Magellanic Clouds which have lower
metallicities than the solar neighborhood. To test this prediction we have
observed the open SMC cluster NGC 371 for 12 nights in order to search for beta
Cep and SPB stars. Surprisingly, we find 29 short-period B-type variables in
the upper part of the main sequence, many of which are probably SPB stars. This
result indicates that pulsation is still driven by the kappa mechanism even in
low metallicity environments. All the identified variables have periods longer
than the fundamental radial period which means that they cannot be beta Cep
stars. Within an amplitude detection limit of 5 mmag no stars in the top of the
HR-diagram show variability with periods shorter than the fundamental radial
period. So if beta Cep stars are present in the cluster they oscillate with
amplitudes below 5 mmag, which is significantly lower than the mean amplitude
of beta Cep stars in the Galaxy. We see evidence that multimode pulsation is
more common in the upper part of the main sequence than in the lower. We have
also identified 5 eclipsing binaries and 3 periodic pulsating Be stars in the
cluster field.Comment: 8 pages, 11 figures. Accepted for publication in MNRA
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