188 research outputs found
The sdB pulsating star V391 Peg and its putative giant planet revisited after 13 years of time-series photometric data
V391 Peg (alias HS 2201+2610) is a subdwarf B (sdB) pulsating star that shows both p- and g-modes. By studying the arrival times
of the p-mode maxima and minima through the O–C method, in a previous article the presence of a planet was inferred with an
orbital period of 3.2 years and a minimum mass of 3.2 MJup. Here we present an updated O–C analysis using a larger data set of
1066 h of photometric time series (∼2.5× larger in terms of the number of data points), which covers the period between 1999 and 2012
(compared with 1999–2006 of the previous analysis). Up to the end of 2008, the new O–C diagram of the main pulsation frequency (f1)
is compatible with (and improves) the previous two-component solution representing the long-term variation of the pulsation period
(parabolic component) and the giant planet (sine wave component). Since 2009, the O–C trend of f1 changes, and the time derivative
of the pulsation period (p˙) passes from positive to negative; the reason of this change of regime is not clear and could be related to
nonlinear interactions between different pulsation modes. With the new data, the O–C diagram of the secondary pulsation frequency
(f2) continues to show two components (parabola and sine wave), like in the previous analysis. Various solutions are proposed to fit
the O–C diagrams of f1 and f2, but in all of them, the sinusoidal components of f1 and f2 differ or at least agree less well than before.
The nice agreement found previously was a coincidence due to various small effects that are carefully analyzed. Now, with a larger
dataset, the presence of a planet is more uncertain and would require confirmation with an independent method. The new data allow
us to improve the measurement of p˙ for f1 and f2: using only the data up to the end of 2008, we obtain p˙ 1 = (1.34 ± 0.04) × 10−12 and
p˙ 2 = (1.62 ± 0.22) × 10−12. The long-term variation of the two main pulsation periods (and the change of sign of p˙ 1) is visible also in
direct measurements made over several years. The absence of peaks near f1 in the Fourier transform and the secondary peak close to
f2 confirm a previous identification as l = 0 and l = 1, respectively, and suggest a stellar rotation period of about 40 days. The new data
allow constraining the main g-mode pulsation periods of the star
A 3D view of the Hyades stellar and sub-stellar population
Our scientific goal is to provide a 3D map of the nearest open cluster to the
Sun, the Hyades, combining the recent release of Gaia astrometric data,
ground-based parallaxes of sub-stellar member candidates and photometric data
from surveys which cover large areas of the cluster.
We combined the second Gaia release with ground-based H-band parallaxes
obtained with the infrared camera on the 2-m robotic Liverpool telescope to
astrometrically identify stellar and sub-stellar members of the Hyades, the
nearest open cluster to the Sun.
We find 1764 objects within 70 degree radius from the cluster center from the
Gaia second data release, whose kinematic properties are consistent with the
Hyades. We limit our study to 30 pc from the cluster center (47.03+/-0.20 pc)
where we identify 710 candidate members, including 85 and 385 in the core and
tidal radius, respectively. We determine proper motions and parallaxes of eight
candidate brown dwarf members and confirm their membership. Using the 3D
positions and a model-based mass-luminosity relation we derive a luminosity and
mass function in the 0.04 to 2.5 Msun range. We confirm evidence for mass
segregation in the Hyades and find a dearth of brown dwarfs in the core of the
cluster. From the white dwarf members we estimate an age of 640
Myr.
We identify a list of members in the Hyades cluster from the most massive
stars down to the brown dwarfs. We produce for the first time a 3D map of the
Hyades cluster in the stellar and sub-stellar regimes and make available the
list of candidate members.Comment: 27 pages, 2 appendices, 12 figures and 7 tables in main text,
accepted for publication in A&A. Corrections for language edition not
included in that version. Table of members will be public in CD
PG 1613+426: a new sdB pulsator
We report the detection of short period oscillations in the hot subdwarf B
(sdB) star PG 1613+426 from time-series photometry carried out with the 91-cm
Cassegrain telescope of the Catania Astrophysical Observatory. This star, which
is brighter than the average of the presently known sdB pulsators, with B =
14.14 mag, has and , its position
is near the hot end of the sdB instability strip, and it is a pulsator with a
well observed peak in the power spectrum at . This star
seems to be well suited for high precision measurements, which could detect a
possible multi-mode pulsation behaviourComment: 3 pages, 4 figures. to appear on A&
Kepler detection of a new extreme planetary system orbiting the subdwarf-B pulsator KIC10001893
KIC10001893 is one out of 19 subdwarf-B (sdB) pulsators observed by the
Kepler spacecraft in its primary mission. In addition to tens of pulsation
frequencies in the g-mode domain, its Fourier spectrum shows three weak peaks
at very low frequencies, which is too low to be explained in terms of g modes.
The most convincing explanation is that we are seeing the orbital modulation of
three Earth-size planets (or planetary remnants) in very tight orbits, which
are illuminated by the strong stellar radiation. The orbital periods are
P1=5.273, P2=7.807, and P3=19.48 hours, and the period ratios P2/P1=1.481 and
P3/P2=2.495 are very close to the 3:2 and 5:2 resonances, respectively. One of
the main pulsation modes of the star at 210.68 {\mu}Hz corresponds to the third
harmonic of the orbital frequency of the inner planet, suggesting that we see,
for the first time in an sdB star, g-mode pulsations tidally excited by a
planetary companion. The extreme planetary system that emerges from the Kepler
data is very similar to the recent discovery of two Earth-size planets orbiting
the sdB pulsator KIC05807616 (Charpinet et al. 2011a).Comment: 6 pages, 5 figures, accepted for publication in Astronomy and
Astrophysic
Pyomyositis associated with abscess formation caused by streptococcus pneumoniae in children: a case report and review of literature
Background: Pyomyositis is an unusual bacterial infection but potential severe in children. Staphylococcus Aureus is the main caused of this disease (70–90%), following by Streptococcus Pyogenes (4–16%). Streptococcus Pneumoniae rarely caused invasive muscular infections. We describe a case of pyomyositis caused by Streptococcus Pneumonia in an adolescent 12-year-old female. Case presentation: I.L. referred to our hospital for high fever associated with right hip and abdominal pain. The blood exams showed increase of leukocytes with prevalence of neutrophils with high level of inflammatory markers (CRP 46,17 mg/dl; Procalcitonin 25,8 ng/ml). The abdomen ultrasonography was unremarkable. The CT and MRI of the abdomen and right hip revealed pyomyositis of the iliopsoas, piriformis and internal shutter associated with collection of pus between the muscular planes (Fig. 1). The patient was admitted to our paediatric care unit, and she was initially treatment with intravenous Ceftriaxone (100 mg/kg/day) and Vancomycin (60 mg/kg/day). On day 2, a pansensitive Streptococcus Pneumoniae was isolated from the blood culture, and the antibiotic treatment was changed to only IV Ceftriaxone. She was successively treated with IV Ceftriaxone for 3 weeks, then continued with oral Amoxicillin for a total of 6 weeks of therapy. The follow up showed a complete resolution of the pyomyositis and psoas abscess after 2 months. Conclusion: Pyomyositis associate with abscess is a rare and very dangerous disease in children. The clinical presentation can mimic symptoms of other pathologies like osteomyelitis or septic arthritis, so many times is hard to identify. The main risk factors include story of recent trauma and immunodeficiency, not present in our case report. The therapy involves the antibiotics and, if possible, abscess drainage. In literature there is much discussion about duration of antibiotic therapy
The sdB pulsating star V391 Peg and its putative giant planet revisited after 13 years of time-series photometric data
V391 Peg (alias HS 2201+2610) is a subdwarf B (sdB) pulsating star that shows both p- and g-modes. By studying the arrival times of the p-mode maxima and minima through the O-C method, in a previous article the presence of a planet was inferred with an orbital period of 3.2 years and a minimum mass of 3.2 MJup. Here we present an updated O-C analysis using a larger data set of 1066 h of photometric time series ( 2.5× larger in terms of the number of data points), which covers the period between 1999 and 2012 (compared with 1999-2006 of the previous analysis). Up to the end of 2008, the new O-C diagram of the main pulsation frequency (f1) is compatible with (and improves) the previous two-component solution representing the long-term variation of the pulsation period (parabolic component) and the giant planet (sine wave component). Since 2009, the O-C trend of f1 changes, and the time derivative of the pulsation period (p.) passes from positive to negative; the reason of this change of regime is not clear and could be related to nonlinear interactions between different pulsation modes. With the new data, the O-C diagram of the secondary pulsation frequency (f2) continues to show two components (parabola and sine wave), like in the previous analysis. Various solutions are proposed to fit the O-C diagrams of f1 and f2, but in all of them, the sinusoidal components of f1 and f2 differ or at least agree less well than before. The nice agreement found previously was a coincidence due to various small effects that are carefully analyzed. Now, with a larger dataset, the presence of a planet is more uncertain and would require confirmation with an independent method. The new data allow us to improve the measurement of p. for f1 and f2: using only the data up to the end of 2008, we obtain p.1 = (1.34 ± 0.04) × 10-12 and p.2 = (1.62 ± 0.22) × 10-12. The long-term variation of the two main pulsation periods (and the change of sign of p.1) is visible also in direct measurements made over several years. The absence of peaks near f1 in the Fourier transform and the secondary peak close to f2 confirm a previous identification as l = 0 and l = 1, respectively, and suggest a stellar rotation period of about 40 days. The new data allow constraining the main g-mode pulsation periods of the star
New nonadiabatic pulsation computations on full PG1159 evolutionary models: the theoretical GW Vir instability strip revisited
We reexamine the theoretical instability domain of pulsating PG1159 stars (GW
Vir variables). We performed an extensive g-mode stability analysis on PG1159
evolutionary models with stellar masses ranging from 0.530 to 0.741 Mo for
which the complete evolutionary stages of their progenitors from the ZAMS,
through the thermally pulsing AGB and born-again phases to the domain of the
PG1159 stars have been considered. We found that pulsations in PG1159 stars are
excited by the kappa-mechanism due to partial ionization of carbon and oxygen,
and that no composition gradients are needed between the surface layers and the
driving region, much in agreement with previous studies. We show, for the first
time, the existence of a red edge of the instability strip at high
luminosities. We found that all of the GW Vir stars lay within our theoretical
instability strip. Our results suggest a qualitative good agreement between the
observed and the predicted ranges of unstable periods of individual stars.
Finally, we found that generally the seismic masses (derived from the period
spacing) of GW Vir stars are somewhat different from the masses suggested by
evolutionary tracks coupled with spectroscopy. Improvements in the evolution
during the thermally pulsing AGB phase and/or during the core helium burning
stage and early AGB could help to alleviate the persisting discrepancies.Comment: 10 pages, 8 figures. To be published in Astronomy and Astrophysic
Follow-up observations of pulsating subdwarf B stars: Multisite campaigns on PG 1618+563B and PG 0048+091
We present follow-up observations of pulsating subdwarf B (sdB) stars as part
of our efforts to resolve the pulsation spectra for use in asteroseismological
analyses. This paper reports on multisite campaigns of the pulsating sdB stars
PG 1618+563B and PG 0048+091. Data were obtained from observatories placed
around the globe for coverage from all longitudes. For PG 1618+563B, our
five-site campaign uncovered a dichotomy of pulsation states: Early during the
campaign the amplitudes and phases (and perhaps frequencies) were quite
variable while data obtained late in the campaign were able to fully resolve
five stable pulsation frequencies. For PG 0048+091, our five-site campaign
uncovered a plethora of frequencies with short pulsation lifetimes. We find
them to have observed properties consistent with stochastically excited
oscillations, an unexpected result for subdwarf B stars. We discuss our
findings and their impact on subdwarf B asteroseismology.Comment: 50 pages including 17 figures and 10 tables. Accepted for publication
in the Astrophysical Journa
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