614 research outputs found
Efficiency of planetesimal ablation in giant planetary envelopes
Observations of exoplanetary spectra are leading to unprecedented constraints
on their atmospheric elemental abundances, particularly O/H, C/H, and C/O
ratios. Recent studies suggest that elemental ratios could provide important
constraints on formation and migration mechanisms of giant exoplanets. A
fundamental assumption in such studies is that the chemical composition of the
planetary envelope represents the sum-total of compositions of the accreted gas
and solids during the formation history of the planet. We investigate the
efficiency with which accreted planetesimals ablate in a giant planetary
envelope thereby contributing to its composition rather than sinking to the
core. From considerations of aerodynamic drag causing `frictional ablation' and
the envelope temperature structure causing `thermal ablation', we compute mass
ablations for impacting planetesimals of radii 30 m to 1 km for different
compositions (ice to iron) and a wide range of velocities and impact angles,
assuming spherical symmetry. Icy impactors are fully ablated in the outer
envelope for a wide range of parameters. Even for Fe impactors substantial
ablation occurs in the envelope for a wide range of sizes and velocities. For
example, iron impactors of sizes below ~0.5 km and velocities above ~30 km/s
are found to ablate by ~60-80% within the outer envelope at pressures below
10^3 bar due to frictional ablation alone. For deeper pressures (~10^7 bar),
substantial ablation happens over a wider range of parameters. Therefore, our
exploratory study suggests that atmospheric abundances of volatile elements in
giant planets reflect their accretion history during formation
Thermal Emission of WASP-14b Revealed with Three Spitzer Eclipses
Exoplanet WASP-14b is a highly irradiated, transiting hot Jupiter. Joshi et
al. calculate an equilibrium temperature Teq of 1866 K for zero albedo and
reemission from the entire planet, a mass of 7.3 +/- 0.5 Jupiter masses and a
radius of 1.28 +/- 0.08 Jupiter radii. Its mean density of 4.6 g/cm3 is one of
the highest known for planets with periods less than 3 days. We obtained three
secondary eclipse light curves with the Spitzer Space Telescope. The eclipse
depths from the best jointly fit model are +/- at 4.5
{\mu}m and +/- at 8.0 {\mu}m. The corresponding brightness
temperatures are 2212 +/- 94 K and 1590 +/- 116 K. A slight ambiguity between
systematic models suggests a conservative 3.6 {\mu}m eclipse depth of
+/- and brightness temperature of 2242 +/- 55 K. Although extremely
irradiated, WASP-14b does not show any distinct evidence of a thermal
inversion. In addition, the present data nominally favor models with day night
energy redistribution less than . The current data are generally
consistent with oxygen-rich as well as carbon-rich compositions, although an
oxygen-rich composition provides a marginally better fit. We confirm a
significant eccentricity of e = 0.087 +/- 0.002 and refine other orbital
parameters.Comment: 16 pages, 16 figure
A Study on the Seismic Response of Ground and Reinforced Concrete Buildings in Belgaum Region, India
In the recent years, each unpredictable earthquake (for example Kobe, 1995; Taiwan, 1999; Kocaeli, 1999 and Bhuj, 2001) has revealed its own saga of destruction and failure of engineered structures. Therefore, regional variation in potential earthquake damage should be carefully assessed for better planning towards disaster mitigation. This requires assessment of the seismic ground motion parameters. The present study focus on the seismic response of ground and reinforced concrete buildings in Belgaum region (located in zone III, as per IS 1893–Part1: 2002) in Karnataka state. At present no strong motion records are available in this region and therefore, wavelet-based spectrum compatibility approach is used to generate synthetic earthquake motions for the region. The effect of soil deposits in the region on propagation of seismic motion parameters to the ground surface is investigated based on equivalent linear approach. The Frequency response analysis of buildings of various configurations is carried out with three dimensional numerical modeling. The results indicate the maximum spectral accelerations at the ground surface in the range of 0.68g to 1.29g and peak ground acceleration (PGA) amplifications in the range of 2.16 to 3.13. The predicted fundamental period of soil deposits in the region varies from 0.2 s to 0.4 s. The configuration of buildings susceptible to resonance due to the close matching of resulting wave frequencies of the ground is identified
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&
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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