1,919 research outputs found
The thermal emission of the exoplanets WASP-1b and WASP-2b
We present a comparative study of the thermal emission of the transiting
exoplanets WASP-1b and WASP-2b using the Spitzer Space Telescope. The two
planets have very similar masses but suffer different levels of irradiation and
are predicted to fall either side of a sharp transition between planets with
and without hot stratospheres. WASP-1b is one of the most highly irradiated
planets studied to date. We measure planet/star contrast ratios in all four of
the IRAC bands for both planets (3.6-8.0um), and our results indicate the
presence of a strong temperature inversion in the atmosphere of WASP-1b,
particularly apparent at 8um, and no inversion in WASP-2b. In both cases the
measured eclipse depths favor models in which incident energy is not
redistributed efficiently from the day side to the night side of the planet. We
fit the Spitzer light curves simultaneously with the best available radial
velocity curves and transit photometry in order to provide updated measurements
of system parameters. We do not find significant eccentricity in the orbit of
either planet, suggesting that the inflated radius of WASP-1b is unlikely to be
the result of tidal heating. Finally, by plotting ratios of secondary eclipse
depths at 8um and 4.5um against irradiation for all available planets, we find
evidence for a sharp transition in the emission spectra of hot Jupiters at an
irradiation level of 2 x 10^9 erg/s/cm^2. We suggest this transition may be due
to the presence of TiO in the upper atmospheres of the most strongly irradiated
hot Jupiters.Comment: 10 pages, submitted to Ap
Thermal emission from WASP-24b at 3.6 and 4.5 {\mu}m
Aims. We observe occultations of WASP-24b to measure brightness temperatures
and to determine whether or not its atmosphere exhibits a thermal inversion
(stratosphere). Methods. We observed occultations of WASP-24b at 3.6 and 4.5
{\mu}m using the Spitzer Space Telescope. It has been suggested that there is a
correlation between stellar activity and the presence of inversions, so we
analysed existing HARPS spectra in order to calculate log R'HK for WASP-24 and
thus determine whether or not the star is chromospherically active. We also
observed a transit of WASP-24b in the Str\"{o}mgren u and y bands, with the
CAHA 2.2-m telescope. Results. We measure occultation depths of 0.159 \pm 0.013
per cent at 3.6 {\mu}m and 0.202 \pm 0.018 per cent at 4.5 {\mu}m. The
corresponding planetary brightness temperatures are 1974 \pm 71 K and 1944 \pm
85 K respectively. Atmosphere models with and without a thermal inversion fit
the data equally well; we are unable to constrain the presence of an inversion
without additional occultation measurements in the near-IR. We find log R'HK =
-4.98 \pm 0.12, indicating that WASP-24 is not a chromospherically active star.
Our global analysis of new and previously-published data has refined the system
parameters, and we find no evidence that the orbit of WASP-24b is non-circular.
Conclusions. These results emphasise the importance of complementing Spitzer
measurements with observations at shorter wavelengths to gain a full
understanding of hot Jupiter atmospheres.Comment: 7 pages, 4 figures, 3 tables. Accepted for publication in A&
Spitzer observations of the thermal emission from WASP-43b
WASP-43b is one of the closest-orbiting hot Jupiters, with a semimajor axis
of a = 0.01526 +/- 0.00018 AU and a period of only 0.81 days. However, it
orbits one of the coolest stars with a hot Jupiter (Tstar = 4520 +/- 120 K),
giving the planet a modest equilibrium temperature of Teq = 1440 +/- 40 K,
assuming zero Bond albedo and uniform planetary energy redistribution. The
eclipse depths and brightness temperatures from our jointly fit model are
0.347% +/- 0.013% and 1670 +/- 23 K at 3.6 {\mu}m and 0.382% +/- 0.015% and
1514 +/- 25 K at 4.5 {\mu}m. The eclipse timings improved the estimate of the
orbital period, P, by a factor of three (P = 0.81347436 +/- 1.4*10-7 days) and
put an upper limit on the eccentricity (e = 0.010+0.010 -0.007). We use our
Spitzer eclipse depths along with four previously reported ground-based
photometric observations in the near-infrared to constrain the atmospheric
properties of WASP-43b. The data rule out a strong thermal inversion in the
dayside atmosphere of WASP-43b. Model atmospheres with no thermal inversions
and fiducial oxygen-rich compositions are able to explain all the available
data. However, a wide range of metallicities and C/O ratios can explain the
data. The data suggest low day-night energy redistribution in the planet,
consistent with previous studies, with a nominal upper limit of about 35% for
the fraction of energy incident on the dayside that is redistributed to the
nightside.Comment: 11 pages, 9 figure
Thermal emission at 3.6-8 mu m from WASP-19b: a hot Jupiter without a stratosphere orbiting an active star
We report detection of thermal emission from the exoplanet WASP-19b at 3.6, 4.5, 5.8 and 8.0 mu m. We used the InfraRed Array Camera on the Spitzer Space Telescope to observe two occultations of WASP-19b by its host star. We combine our new detections with previous measurements of WASP-19b\u27s emission at 1.6 and 2.09 mu m to construct a spectral energy distribution of the planet\u27s dayside atmosphere. By comparing this with model-atmosphere spectra, we find that the dayside atmosphere of WASP-19b lacks a strong temperature inversion. As WASP-19 is an active star (log R\u27(HK) = -4.50 +/- 0.03), this finding supports the hypothesis of Knutson, Howard and Isaacson that inversions are suppressed in hot Jupiters orbiting active stars. The available data are unable to differentiate between a carbon-rich and an oxygen-rich atmosphere
Thermal emission at 4.5 and 8 μm of WASP-17b, an extremely large planet in a slightly eccentric orbit
We report the detection of thermal emission at 4.5 and 8 μm from the planet WASP-17b. We used Spitzer to measure the system brightness at each wavelength during two occultations of the planet by its host star. By combining the resulting light curves with existing transit light curves and radial-velocity measurements in a simultaneous analysis, we find the radius of WASP-17b to be 2.0RJup, which is 0.2RJup larger than any other known planet and 0.7RJup larger than predicted by the standard cooling theory of irradiated gas giant planets. We find the retrograde orbit of WASP-17b to be slightly eccentric, with 0.0012 < e < 0.070 (3σ). Such a low eccentricity suggests that, under current models, tidal heating alone could not have bloated the planet to its current size, so the radius of WASP-17b is currently unexplained. From the measured planet-star flux-density ratios we infer 4.5 and 8 μm brightness temperatures of 1881 ± 50 and 1580 ± 150 K, respectively, consistent with a low-albedo planet that efficiently redistributes heat from its day side to its night sid
The Influence of Organizational Context on Quitting Intention
This study uses multilevel methods to investigate the effects of organizational context on job satisfaction and quitting intention among staff working in long-term mental health care settings. Two types of organizational features are examined: group job satisfaction and structural features of the work unit (unit size, workload, and level of client functioning on the unit). A review of the organizational literature reveals that most empirical research has investigated job satisfaction at the individual level of analysis rather than the group level. The authors argue that the affective context of a group has real and measurable consequences for individual attitudes and behavior, independent of individual attitudes toward the job. Using multilevel modeling, study findings support the premise that group job satisfaction exercises effects on intention to quit independent of individuals’ dispositions toward their jobs. These effects are both direct and interactive. The findings underscore the importance of affective context in shaping individual attitudes and behavioral intentions.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/68775/2/10.1177_0164027599212003.pd
High C/O Chemistry and Weak Thermal Inversion in the Extremely Irradiated Atmosphere of Exoplanet WASP-12b
The carbon-to-oxygen ratio (C/O) in a planet provides critical information about its primordial origins and subsequent evolution. A primordial C/O greater than 0.8 causes a carbide-dominated interior as opposed to the silicate-dominated composition as found on Earth; the solar C/O is 0.54. Theory, shows that high C/O leads to a diversity of carbon-rich planets that can have very different interiors and atmospheres from those in the solar system. Here we report the detection of C/O greater than or equal to 1 in a planetary atmosphere. The transiting hot Jupiter WASP-12b has a dayside atmosphere depleted in water vapour and enhanced in methane by over two orders of magnitude compared to a solar-abundance chemical equilibrium model at the expected temperatures. The observed concentrations of the prominent molecules CO, CH4, and H2O are consistent with theoretical expectations for an atmosphere with the observed C/O = 1. The C/O ratios are not known for giant planets in the solar system, although they are expected to equal the solar value. If high C/O ratios are common, then extrasolar planets are likely very different in interior composition, and formed very differently, from expectations based on solar composition, potentially explaining the large diversity in observed radii. We also find that the extremely irradiated atmosphere (greater than 2500 K) of WASP-12b lacks a prominent thermal inversion, or a stratosphere, and has very efficient day-night energy circulation. The absence of a strong thermal inversion is in stark contrast to theoretical predictions for the most highly irradiated hot-Jupiter atmospheres
Infrared radiation from an extrasolar planet
A class of extrasolar giant planets - the so-called `hot Jupiters' - orbit
within 0.05 AU of their primary stars. These planets should be hot and so emit
detectable infrared radiation. The planet HD 209458b is an ideal candidate for
the detection and characterization of this infrared light because it is
eclipsed by the star. This planet has an anomalously large radius (1.35 times
that of Jupiter), which may be the result of ongoing tidal dissipation, but
this explanation requires a non-zero orbital eccentricity (~0.03), maintained
by interaction with a hypothetical second planet. Here we report detection of
infrared (24 micron) radiation from HD 209458b, by observing the decrement in
flux during secondary eclipse, when the planet passes behind the star. The
planet's 24 micron flux is 55 +/- 10 micro-Jy (1 sigma), with a brightness
temperature of 1130 +/- 150 Kelvins, confirming the predicted heating by
stellar irradiation. The secondary eclipse occurs at the midpoint between
transits of the planet in front of the star (to within +/- 7 min, 1 sigma),
which means that a dynamically significant orbital eccentricity is unlikely.Comment: to appear in Nature April 7, posted to Nature online March 23 (11
pages, 3 figures
The political ontology of collaborative water governance
This article examines the various definitions of, and analytical approaches to, collaborative water governance (CWG). While the concept’s usage has increased over the past decade, there lacks any deep engagement with the concept of the political at the heart of CWG. This article argues that contemporary approaches to CWG risk emptying the concept of its utility and coherence. Correcting this deficiency requires a focus on the social and ideational constructions of water. This will strengthen future collaborative water arrangements and enable deeper appreciation of the ways the political makes and remakes what is possible in water governance
Thermal emission at 3.6-8 micron from WASP-19b: a hot Jupiter without a stratosphere orbiting an active star
We report detection of thermal emission from the exoplanet WASP-19b at 3.6,
4.5, 5.8 and 8.0 micron. We used the InfraRed Array Camera on the Spitzer Space
Telescope to observe two occultations of WASP-19b by its host star. We combine
our new detections with previous measurements of WASP-19b's emission at 1.6 and
2.09 micron to construct a spectral energy distribution of the planet's dayside
atmosphere. By comparing this with model-atmosphere spectra, we find that the
dayside atmosphere of WASP-19b lacks a strong temperature inversion. As WASP-19
is an active star (log RHK = -4.50 +/- 0.03), this finding supports the
hypothesis of Knutson, Howard & Isaacson (2010) that inversions are suppressed
in hot Jupiters orbiting active stars. The available data are unable to
differentiate between a carbon-rich and an oxygen-rich atmosphere.Comment: As accepted for publication in MNRAS. 12 pages, 5 figures, 3 table
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