6,347 research outputs found
The Penn State - Toru\'n Centre for Astronomy Planet Search stars IV. Dwarfs and the complete sample
Our knowledge of the intrinsic parameters of exoplanets is as precise as our
determinations of their stellar hosts parameters. In the case of radial
velocity searches for planets, stellar masses appear to be crucial. But before
estimating stellar masses properly, detailed spectroscopic analysis is
essential. With this paper we conclude a general spectroscopic description of
the Pennsylvania-Torun Planet Search (PTPS) sample of stars. We aim at a
detailed description of basic parameters of stars representing the complete
PTPS sample. We present atmospheric and physical parameters for dwarf stars
observed within the PTPS along with updated physical parameters for the
remaining stars from this sample after the first Gaia data release. We used
high resolution (R=60 000) and high signal-to-noise-ratio (S/N=150-250) spectra
from the Hobby-Eberly Telescope and its High Resolution Spectrograph. Stellar
atmospheric parameters were determined through a strictly spectroscopic local
thermodynamic equilibrium analysis (LTE) of the equivalent widths of FeI and
FeII lines. Stellar masses, ages, and luminosities were estimated through a
Bayesian analysis of theoretical isochrones. We present , log ,
[Fe/H], micrturbulence velocities, absolute radial velocities, and rotational
velocities for 156 stars from the dwarf sample of PTPS. For most of these stars
these are the first determinations. We refine the definition of PTPS subsamples
of stars (giants, subgiants, and dwarfs) and update the luminosity classes for
all PTPS stars. Using available Gaia and Hipparcos parallaxes, we redetermine
the stellar parameters (masses, radii, luminosities, and ages) for 451 PTPS
stars. The complete PTPS sample of 885 stars is composed of 132 dwarfs, 238
subgiants, and 515 giants, of which the vast majority are of roughly solar
mass.Comment: 11 pages, 10 figures, Accepted for publication in Astronomy &
Astrophysic
Three red giants with substellar-mass companions
We present three giant stars from the ongoing Penn State-Toru\'n Planet
Search with the Hobby-Eberly Telescope, which exhibit radial velocity
variations that point to a presence of planetary --mass companions around them.
BD+49 828 is a K0 giant with a = minimum mass companion in
AU (d),
orbit. HD 95127, a log/=,
, K0 giant has a = minimum mass companion in
AU (d), orbit.
Finally, HD 216536, is a K0 giant with a minimum mass companion in
AU (d),
orbit. Both, HD 95127 b and HD 216536 b in their
compact orbits, are very close to the engulfment zone and hence prone to
ingestion in the near future. BD+49 828 b is among the longest period planets
detected with the radial velocity technique until now and it will remain
unaffected by stellar evolution up to a very late stage of its host. We discuss
general properties of planetary systems around evolved stars and planet
survivability using existing data on exoplanets in more detail.Comment: 47 pages, 11 figures. Accepted by Ap
Comparison of Grain Refinement in Selected Materials Subjected to Hydrostatic Extrusion
The subject of this study was to examine and compare the impact of intense hydrostatic extrusion on grain refinement in three different alloys: duplex stainless steel, commercially used aluminum alloy (6060) and Ag-Cu12 alloy. As a result of the process grain sizes from 370 nm to 90 nm were obtained in aluminum and duplex steel. To analyze the of hydrostatic on mechanical properties tensile tests were also carried out. The highest grain refinement (70 nm) and yield strength increase (over 300%) was observed in duplex steel af-ter hydrostatic extrusion.
When you are citing the document, use the following link http://essuir.sumdu.edu.ua/handle/123456789/3560
TAPAS IV. TYC 3667-1280-1 b - the most massive red giant star hosting a warm Jupiter
We present the latest result of the TAPAS project that is devoted to intense
monitoring of planetary candidates that are identified within the
PennState-Toru\'n planet search.
We aim to detect planetary systems around evolved stars to be able to build
sound statistics on the frequency and intrinsic nature of these systems, and to
deliver in-depth studies of selected planetary systems with evidence of
star-planet interaction processes.
The paper is based on precise radial velocity measurements: 13 epochs
collected over 1920 days with the Hobby-Eberly Telescope and its
High-Resolution Spectrograph, and 22 epochs of ultra-precise HARPS-N data
collected over 961 days.
We present a warm-Jupiter (, 0.4)
companion with an orbital period of 26.468 days in a circular () orbit
around a giant evolved (, ) star
with . This is the most massive and oldest star
found to be hosting a close-in giant planet. Its proximity to its host
() means that the planet has a probability of
transits; this calls for photometric follow-up study.
This massive warm Jupiter with a near circular orbit around an evolved
massive star can help set constraints on general migration mechanisms for warm
Jupiters and, given its high equilibrium temperature, can help test energy
deposition models in hot Jupiters.Comment: 5 pages, 3 figures, accepted by A&
TAPAS - Tracking Advanced Planetary Systems with HARPS-N. II. Super Li-rich giant HD 107028
Lithium rich giant stars are rare objects. For some of them, Li enrichment
exceeds abundance of this element found in solar system meteorites, suggesting
that these stars have gone through a Li enhancement process. We identified a Li
rich giant HD 107028 with A(Li) > 3.3 in a sample of evolved stars observed
within the PennState Torun Planet Search. In this work we study different
enhancement scenarios and we try to identify the one responsible for Li
enrichment for HD 107028. We collected high resolution spectra with three
different instruments, covering different spectral ranges. We determine stellar
parameters and abundances of selected elements with both equivalent width
measurements and analysis, and spectral synthesis. We also collected multi
epoch high precision radial velocities in an attempt to detect a companion.
Collected data show that HD 107028 is a star at the base of Red Giant Branch.
Except for high Li abundance, we have not identified any other anomalies in its
chemical composition, and there is no indication of a low mass or stellar
companion. We exclude Li production at the Luminosity Function Bump on RGB, as
the effective temperature and luminosity suggest that the evolutionary state is
much earlier than RGB Bump. We also cannot confirm the Li enhancement by
contamination, as we do not observe any anomalies that are associated with this
scenario. After evaluating various scenarios of Li enhancement we conclude that
the Li-overabundance of HD 107028 originates from Main Sequence evolution, and
may be caused by diffusion process.Comment: Accepted for publication in A&
Tracking Advanced Planetary Systems (TAPAS) with HARPS-N. III. HD 5583 and BD+15 2375 - two cool giants with warm companions
Evolved stars are crucial pieces to understand the dependency of the planet
formation mechanism on the stellar mass and to explore deeper the mechanism
involved in star-planet interactions. Over the past ten years, we have
monitored about 1000 evolved stars for radial velocity variations in search for
low-mass companions under the Penn State - Torun Centre for Astronomy Planet
Search program with the Hobby-Eberly Telescope. Selected prospective candidates
that required higher RV precision measurements have been followed with HARPS-N
at the 3.6 m Telescopio Nazionale Galileo under the TAPAS project.
We aim to detect planetary systems around evolved stars to be able to build
sound statistics on the frequency and intrinsic nature of these systems, and to
deliver in-depth studies of selected planetary systems with evidence of
star-planet interaction processes. For HD 5583 we obtained 14 epochs of precise
RV measurements collected over 2313 days with the Hobby-Eberly Telescope (HET),
and 22 epochs of ultra-precise HARPS-N data collected over 976 days. For BD+15
2375 we collected 24 epochs of HET data over 3286 days and 25 epochs of HARPS-S
data over 902 days.
We report the discovery of two planetary mass objects orbiting two evolved
Red Giant stars: HD~5583 has a m sin i = 5.78 M companion at 0.529~AU in
a nearly circular orbit (e=0.076), the closest companion to a giant star
detected with the RV technique, and BD+15~2735 that with a m sin i= 1.06
M holds the record of the lightest planet found so far orbiting an
evolved star (in a circular e=0.001, 0.576~AU orbit). These are the third and
fourth planets found within the TAPAS project, a HARPS-N monitoring of evolved
planetary systems identified with the Hobby-Eberly Telescope.Comment: 9 pages, 6 figures. Accepted by Astronomy and Astrophysic
A novel approach to crystallisation of nanodispersible microparticles by spray drying for improved tabletability
YesHigh-dose API powders which are to be tableted by direct compression should have high compactibility and compressibility. This note reports on a novel approach to the manufacture of crystalline powders intended for direct compaction with improved compactibility and compressibility properties. The poorly compactable API, chlorothiazide, was spray dried from a water/acetone solvent mix producing additive-free nanocrystalline microparticles (NCMPs) of median particle size 3.5 μm. Tablets compacted from NCMPs had tensile strengths ranging from 0.5 to 4.6 MPa (compared to 0.6–0.9 MPa for tablets of micronised CTZ) at compression forces ranging from 6 kN to 13 kN. NCMP tablets also had high porosities (34–20%) and large specific surface areas (4.4–4.8 m2/g). The time taken for tablets made of NCMPs to erode was not statistically longer (p > 0.05) than for tablets made of micronised CTZ. Fragmentation of NCMPs on compression was observed. The volume fraction of particles below 1 μm present in the suspension recovered after erosion of NCMP tablets was 34.8 ± 3.43%, while no nanosized particles were detected in the slurry after erosion of compacted micronised CTZ.Solid State Pharmaceutical Cluster (SSPC), supported by Science Foundation Ireland under grant number 07/SRC/B1158
Digital topoclimatic maps of Warsaw
Cyfrowe mapy topoklimatyczne Warszawy są efektem pierwszego etapu badań mającego na celu stworzenie bazy danych o środowisku fizyczno-geograficznym tej aglomeracji. Przy tworzeniu bazy danych zastosowano metody GIS. Wykonano mapy elementów meteorologicznych (temperatury powietrza, prędkości wiatru i całkowitego promieniowania słonecznego) oraz mapy zanieczyszczenia powietrza. Przy zastosowaniu modelu MENEX obliczono ilość ciepła zmagazynowanego przez organizm człowieka i promieniowania słonecznego pochłoniętego przez człowieka. W końcowym etapie wykonano syntetyczne mapy, np. obciążenia cieplnego człowieka, topoklimatyczną i biotopoklimatyczną.Digital topoclimatic maps of Warsaware the effect of the first step of the studies dealing with creation of the data base of physico-geographical environment of this agglomeration. GIS methods are used in this purpose. At present there were made basic maps of meteorological elements (air temperature, wind speed and global solar radiation) as well as air pollution maps. With the use of the MENEX model there were calculated maps of net heat storage of the human organism and solar radiation absorbed by man. Finally some synthetic maps were made e.g. heat load of man, topoclimatic and biotopoclimatic (which takes into account heat load of man and air pollution)
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