402 research outputs found
The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars
Phosphorus (P) is a critical element for life on Earth yet the cosmic
production sites of P are relatively uncertain. To understand how P has evolved
in the solar neighborhood, we measured abundances for 163 FGK stars over a
range of -1.09 [Fe/H] 0.47 using observations from the Habitable-zone
Planet Finder (HPF) instrument on the Hobby-Eberly Telescope (HET). Atmospheric
parameters were calculated by fitting a combination of astrometry, photometry,
and Fe I line equivalent widths. Phosphorus abundances were measured by
matching synthetic spectra to a P I feature at 10529.52 angstroms. Our [P/Fe]
ratios show that chemical evolution models generally under-predict P over the
observed metallicity range. Additionally, we find that the [P/Fe] differs by
0.1 dex between thin disk and thick disk stars that were identified with
kinematics. The P abundances were compared with -elements, iron-peak,
odd-Z, and s-process elements and we found that P in the disk most strongly
resembles the evolution of the -elements. We also find molar P/C and
N/C ratios for our sample match the scatter seen from other abundance studies.
Finally, we measure a [P/Fe] = 0.09 0.1 ratio in one low- halo
star and probable Gaia-Sausage-Enceladus (GSE) member, an abundance ratio
0.3 - 0.5 dex lower than the other Milky Way disk and halo stars at
similar metallicities. Overall, we find that P is likely most significantly
produced by massive stars in core collapse supernovae (CCSNe) based on the
largest P abundance survey to-date.Comment: 19 pages, 10 figures, accepted for publication in The Astronomical
Journa
Host Star Properties And Transit Exclusion For The HD 38529 Planetary System
The transit signature of exoplanets provides an avenue through which characterization of exoplanetary properties may be undertaken, such as studies of mean density, structure, and atmospheric composition. The Transit Ephemeris Refinement and Monitoring Survey is a program to expand the catalog of transiting planets around bright host stars by refining the orbits of known planets discovered with the radial velocity technique. Here we present results for the HD 38529 system. We determine fundamental properties of the host star through direct interferometric measurements of the radius and through spectroscopic analysis. We provide new radial velocity measurements that are used to improve the Keplerian solution for the two known planets, and we find no evidence for a previously postulated third planet. We also present 12 years of precision robotic photometry of HD 38529 that demonstrate the inner planet does not transit and the host star exhibits cyclic variations in seasonal mean brightness with a timescale of approximately six years
The band structure of BeTe - a combined experimental and theoretical study
Using angle-resolved synchrotron-radiation photoemission spectroscopy we have
determined the dispersion of the valence bands of BeTe(100) along ,
i.e. the [100] direction. The measurements are analyzed with the aid of a
first-principles calculation of the BeTe bulk band structure as well as of the
photoemission peaks as given by the momentum conserving bulk transitions.
Taking the calculated unoccupied bands as final states of the photoemission
process, we obtain an excellent agreement between experimental and calculated
spectra and a clear interpretation of almost all measured bands. In contrast,
the free electron approximation for the final states fails to describe the BeTe
bulk band structure along properly.Comment: 21 pages plus 4 figure
An L Band Spectrum of the Coldest Brown Dwarf
The coldest brown dwarf, WISE 0855, is the closest known planetary-mass,
free-floating object and has a temperature nearly as cold as the solar system
gas giants. Like Jupiter, it is predicted to have an atmosphere rich in
methane, water, and ammonia, with clouds of volatile ices. WISE 0855 is faint
at near-infrared wavelengths and emits almost all its energy in the
mid-infrared. Skemer et al. 2016 presented a spectrum of WISE 0855 from 4.5-5.1
micron (M band), revealing water vapor features. Here, we present a spectrum of
WISE 0855 in L band, from 3.4-4.14 micron. We present a set of atmosphere
models that include a range of compositions (metallicities and C/O ratios) and
water ice clouds. Methane absorption is clearly present in the spectrum. The
mid-infrared color can be better matched with a methane abundance that is
depleted relative to solar abundance. We find that there is evidence for water
ice clouds in the M band spectrum, and we find a lack of phosphine spectral
features in both the L and M band spectra. We suggest that a deep continuum
opacity source may be obscuring the near-infrared flux, possibly a deep
phosphorous-bearing cloud, ammonium dihyrogen phosphate. Observations of WISE
0855 provide critical constraints for cold planetary atmospheres, bridging the
temperature range between the long-studied solar system planets and accessible
exoplanets. JWST will soon revolutionize our understanding of cold brown dwarfs
with high-precision spectroscopy across the infrared, allowing us to study
their compositions and cloud properties, and to infer their atmospheric
dynamics and formation processes.Comment: 19 pages, 21 figures. Accepted for publication in Ap
The soil electric potential signature of summer drought
During the period from late April to early August, a timeseries of soil electric potential measurements in the upper 15 cm of mineral soil were collected daily at the University of Michigan Botanical Gardens using an automatic data collection system. These data, after conversion to a surrogate measure of electrolyte concentration, provide a unique record of the 1988 summer drought in a continental location. The effects of rainfall-dewfall electrolyte dilution, evaporation-induced electrolyte concentration and upward-downward soil water advection are well-illustrated in the data. These observations demonstrate that soil electric potential is an easily measured variable of high information content, especially when collected with other system-linked environmental data.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/41671/1/704_2004_Article_BF00866203.pd
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A High-End Estimate of Sea Level Rise for Practitioners
Sea level rise (SLR) is a long-lasting consequence of climate change because global anthropogenic warming takes centuries to millennia to equilibrate for the deep ocean and ice sheets. SLR projections based on climate models support policy analysis, risk assessment and adaptation planning today, despite their large uncertainties. The central range of the SLR distribution is estimated by process-based models. However, risk-averse practitioners often require information about plausible future conditions that lie in the tails of the SLR distribution, which are poorly defined by existing models. Here, a community effort combining scientists and practitioners builds on a framework of discussing physical evidence to quantify high-end global SLR for practitioners. The approach is complementary to the IPCC AR6 report and provides further physically plausible high-end scenarios. High-end estimates for the different SLR components are developed for two climate scenarios at two timescales. For global warming of +2°C in 2100 (RCP2.6/SSP1-2.6) relative to pre-industrial values our high-end global SLR estimates are up to 0.9 m in 2100 and 2.5 m in 2300. Similarly, for a (RCP8.5/SSP5-8.5), we estimate up to 1.6 m in 2100 and up to 10.4 m in 2300. The large and growing differences between the scenarios beyond 2100 emphasize the long-term benefits of mitigation. However, even a modest 2°C warming may cause multi-meter SLR on centennial time scales with profound consequences for coastal areas. Earlier high-end assessments focused on instability mechanisms in Antarctica, while here we emphasize the importance of the timing of ice shelf collapse around Antarctica. This is highly uncertain due to low understanding of the driving processes. Hence both process understanding and emission scenario control high-end SLR
Transits of Known Planets Orbiting a Naked-Eye Star
© 2020 The American Astronomical Society. All rights reserved.Some of the most scientifically valuable transiting planets are those that were already known from radial velocity (RV) surveys. This is primarily because their orbits are well characterized and they preferentially orbit bright stars that are the targets of RV surveys. The Transiting Exoplanet Survey Satellite (TESS) provides an opportunity to survey most of the known exoplanet systems in a systematic fashion to detect possible transits of their planets. HD 136352 (Nu2 Lupi) is a naked-eye (V = 5.78) G-type main-sequence star that was discovered to host three planets with orbital periods of 11.6, 27.6, and 108.1 days via RV monitoring with the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph. We present the detection and characterization of transits for the two inner planets of the HD 136352 system, revealing radii of 1.482-0.056+0.058 R â and 2.608-0.077+0.078 R â for planets b and c, respectively. We combine new HARPS observations with RV data from the Keck/High Resolution Echelle Spectrometer and the Anglo-Australian Telescope, along with TESS photometry from Sector 12, to perform a complete analysis of the system parameters. The combined data analysis results in extracted bulk density values of Ïb = 7.8-1.1+1.2 g cm-3 and Ïc = 3.50-0.36+0.41 g cm-3 for planets b and c, respectively, thus placing them on either side of the radius valley. The combination of the multitransiting planet system, the bright host star, and the diversity of planetary interiors and atmospheres means this will likely become a cornerstone system for atmospheric and orbital characterization of small worlds.Peer reviewe
Uniform Atmospheric Retrieval Analysis of Ultracool Dwarfs II : Properties of 11 T-dwarfs
Accepted ApJ. Supplemental material including full posteriors will be included through the link in the published ApJ article © 2017 The American Astronomical Society. All rights reserved.Brown dwarf spectra are rich in information revealing of the chemical and physical processes operating in their atmospheres. We apply a recently developed atmospheric retrieval tool to an ensemble of late T-dwarf (600-800K) near infrared spectra. With these spectra we are able to place direct constraints the molecular abundances of HO, CH, CO, CO, NH, HS, and Na+K, gravity, thermal structure (and effective temperature), photometric radius, and cloud optical depths. We find that ammonia, water, methane, and the alkali metals are present and well constrained in all 11 objects. From the abundance constraints we find no significant trend in the water, methane, or ammonia abundances with temperature, but find a very strong (25) increasing trend in the alkali metal abundances with effective temperature, indicative of alkali rainout. We also find little evidence for optically thick clouds. With the methane and water abundances, we derive the intrinsic atmospheric metallicity and carbon-to-oxygen ratios. We find in our sample, that metallicities are typically sub solar and carbon-to-oxygen ratios are somewhat super solar, different than expectations from the local stellar population. We also find that the retrieved vertical thermal profiles are consistent with radiative equilibrium over the photospheric regions. Finally, we find that our retrieved effective temperatures are lower than previous inferences for some objects and that our radii are larger than expectations from evolutionary models, possibly indicative of un-resolved binaries. This investigation and methodology represents a paradigm in linking spectra to the determination of the fundamental chemical and physical processes governing cool brown dwarf atmospheres.Peer reviewe
First bromine doped cryogenic implosion at the National Ignition Facility
We report on the first experiment dedicated to the study of nuclear reactions
on dopants in a cryogenic capsule at the National Ignition Facility (NIF). This
was accomplished using bromine doping in the inner layers of the CH ablator of
a capsule identical to that used in the NIF shot N140520. The capsule was doped
with 310 bromine atoms. The doped capsule shot, N170730,
resulted in a DT yield that was 2.6 times lower than the undoped equivalent.
The Radiochemical Analysis of Gaseous Samples (RAGS) system was used to collect
and detect Kr atoms resulting from energetic deuteron and proton ion
reactions on Br. RAGS was also used to detect N produced
dominantly by knock-on deuteron reactions on the C in the ablator.
High-energy reaction-in-flight neutrons were detected via the
Bi(n,4n)Bi reaction, using bismuth activation foils located 50
cm outside of the target capsule. The robustness of the RAGS signals suggest
that the use of nuclear reactions on dopants as diagnostics is quite feasible
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