550 research outputs found
Friedel–Crafts addition of indoles to nitrones promoted by trimethylsilyl trifluoromethanesulfonate
N-alkylindoles undergo Friedel–Crafts addition to aryl and secondary alkyl nitrones in the presence of trimethylsilyl trifluoromethanesulfonate and a trialkylamine to produce 3-(1- (silyloxyamino)alkyl)indoles. Spontaneous conversion to the bisindolyl(aryl)methanes, which is thermodynamically favored for nitrones derived from aromatic aldehydes, is suppressed under the reaction conditions. The silyloxyamino group can be deprotected with tetrabutylammonium fluoride to yield the hydroxylamine
Developing a Drift Rate Distribution for Technosignature Searches of Exoplanets
A stable-frequency transmitter with relative radial acceleration to a
receiver will show a change in received frequency over time, known as a "drift
rate''. For a transmission from an exoplanet, we must account for multiple
components of drift rate: the exoplanet's orbit and rotation, the Earth's orbit
and rotation, and other contributions. Understanding the drift rate
distribution produced by exoplanets relative to Earth, can a) help us constrain
the range of drift rates to check in a Search for Extraterrestrial Intelligence
(SETI) project to detect radio technosignatures and b) help us decide validity
of signals-of-interest, as we can compare drifting signals with expected drift
rates from the target star. In this paper, we modeled the drift rate
distribution for 5300 confirmed exoplanets, using parameters from the
NASA Exoplanet Archive (NEA). We find that confirmed exoplanets have drift
rates such that 99\% of them fall within the 53 nHz range. This implies a
distribution-informed maximum drift rate 4 times lower than previous
work. To mitigate the observational biases inherent in the NEA, we also
simulated an exoplanet population built to reduce these biases. The results
suggest that, for a Kepler-like target star without known exoplanets, 0.44
nHz would be sufficient to account for 99\% of signals. This reduction in
recommended maximum drift rate is partially due to inclination effects and bias
towards short orbital periods in the NEA. These narrowed drift rate maxima will
increase the efficiency of searches and save significant computational effort
in future radio technosignature searches.Comment: 15 pages, 8 figure
The Breakthrough Listen Search for Intelligent Life: A 3.95-8.00 GHz Search for Radio Technosignatures in the Restricted Earth Transit Zone
We report on a search for artificial narrowband signals of 20 stars within
the restricted Earth Transit Zone as a part of the ten-year Breakthrough Listen
(BL) search for extraterrestrial intelligence. The restricted Earth Transit
Zone is the region of the sky from which an observer would see the Earth
transit the Sun with an impact parameter of less than 0.5. This region of the
sky is geometrically unique, providing a potential way for an extraterrestrial
intelligence to discover the Solar System. The targets were nearby (7-143 pc)
and the search covered an electromagnetic frequency range of 3.95-8.00 GHz. We
used the Robert C. Byrd Green Bank Telescope to perform these observations with
the standard BL data recorder. We searched these data for artificial narrowband
(Hz) signals with Doppler drift rates of Hz s. We found
one set of potential candidate signals on the target HIP 109656 which was then
found to be consistent with known properties of anthropogenic radio frequency
interference. We find no evidence for radio technosignatures from
extraterrestrial intelligence in our observations. The observing campaign
achieved a minimum detectable flux which would have allowed detections of
emissions that were to times as powerful as the signaling
capability of the Arecibo radar transmitter, for the nearest and furthest stars
respectively. We conclude that at least of the systems in the restricted
Earth Transit Zone within 150 pc do not possess the type of transmitters
searched in this survey. To our knowledge, this is the first targeted search
for extraterrestrial intelligence of the restricted Earth Transit Zone. All
data used in this paper are publicly available via the Breakthrough Listen
Public Data Archive (http://seti.berkeley.edu/bldr2).Comment: 17 pages, 8 figures, submitted to Ap
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Games people play with brands: An application of Transactional Analysis to marketplace relationships.
Relationships have been normalised in marketing theory as mutuality beneficial, long-term dyads. This obscures their emotional content, ignores critical conceptualisations of corporate exploitation, and fails to capture the range of possible marketplace relationship forms. In this paper we offer Berne’s (1964) Transactional Analysis (TA) as a way to uncover the biographical psychology that informs marketplace relationship structures and their accompanying emotions, and to provide a critique of such arrangements. We first explain TA, its origins, its relationship with psychoanalysis, its limitations, and contemporary extensions beyond therapy. We then present the structural basis of marketplace relationships from a TA perspective, before illustrating how TA Game Analysis can be applied through an analysis of the iPhone and related mobile phone contracts, and the Games If I didn’t Love Apple and Smallprint. Finally we discuss the implications of such an approach for transforming market practices based on recognition of Marketplace Games and their modification
Exotic trees
We discuss the scaling properties of free branched polymers. The scaling
behaviour of the model is classified by the Hausdorff dimensions for the
internal geometry: d_L and d_H, and for the external one: D_L and D_H. The
dimensions d_H and D_H characterize the behaviour for long distances while d_L
and D_L for short distances. We show that the internal Hausdorff dimension is
d_L=2 for generic and scale-free trees, contrary to d_H which is known be equal
two for generic trees and to vary between two and infinity for scale-free
trees. We show that the external Hausdorff dimension D_H is directly related to
the internal one as D_H = \alpha d_H, where \alpha is the stability index of
the embedding weights for the nearest-vertex interactions. The index is
\alpha=2 for weights from the gaussian domain of attraction and 0<\alpha <2 for
those from the L\'evy domain of attraction. If the dimension D of the target
space is larger than D_H one finds D_L=D_H, or otherwise D_L=D. The latter
result means that the fractal structure cannot develop in a target space which
has too low dimension.Comment: 33 pages, 6 eps figure
HATS-8b: A Low-Density Transiting Super-Neptune
HATS-8b is a low density transiting super-Neptune discovered as part of the
HATSouth project. The planet orbits its solar-like G dwarf host (V=14.03
0.10 and T =5679 50 K) with a period of 3.5839 d. HATS-8b is the
third lowest mass transiting exoplanet to be discovered from a wide-field
ground based search, and with a mass of 0.138 0.019 M it is
approximately half-way between the masses of Neptune and Saturn. However
HATS-8b has a radius of 0.873 (+0.123,-0.075) R, resulting in a bulk
density of just 0.259 0.091 g.cm. The metallicity of the host star
is super-Solar ([Fe/H]=0.210 0.080), arguing against the idea that low
density exoplanets form from metal-poor environments. The low density and large
radius of HATS-8b results in an atmospheric scale height of almost 1000 km, and
in addition to this there is an excellent reference star of near equal
magnitude at just 19 arcsecond separation on the sky. These factors make
HATS-8b an exciting target for future atmospheric characterization studies,
particularly for long-slit transmission spectroscopy.Comment: 11 pages, 7 figures, accepted for publication in A
A pilot safety-feasibility dietary trial targeting insulin inhibition in ten patients with advanced cancer
HATS-7b: A Hot Super Neptune Transiting a Quiet K Dwarf Star
IW ../submit_V2/abstract.txt ( Row 1 Col 1 6:48 Ctrl-K H for help We report
the discovery by the HATSouth network of HATS-7b, a transiting Super-Neptune
with a mass of 0.120+/-0.012MJ, a radius of 0.563+/-(0.046,0.034)RJ, and an
orbital period of 3.1853days. The host star is a moderately bright
(V=13.340+/-0.010mag, K_S=10.976+/-0.026mag) K dwarf star with a mass of
0.849+/-0.027Msun , a radius of 0.815+/-(0.049,-0.035)Rsun, and a metallicity
of [Fe/H]=+0.250+/-0.080. The star is photometrically quiet to within the
precision of the HATSouth measurements and has low RV jitter. HATS-7b is the
second smallest radius planet discovered by a wide-field ground-based transit
survey, and one of only a handful of Neptune-size planets with mass and radius
determined to 10% precision. Theoretical modeling of HATS-7b yields a
hydrogen-helium fraction of 18+/-4% (rock-iron core and H2-He envelope), or
9+/-4% (ice core and H2-He envelope), i.e.it has a composition broadly similar
to that of Uranus and Neptune, and very different from that of Saturn, which
has 75% of its mass in H2-He. Based on a sample of transiting exoplanets with
accurately (<20%) determined parameters, we establish approximate power-law
relations for the envelopes of the mass-density distribution of exoplanets.
HATS-7b, which, together with the recently discovered HATS-8b, is one of the
first two transiting super-Neptunes discovered in the Southern sky, is a prime
target for additional follow-up observations with Southern hemisphere
facilities to characterize the atmospheres of Super-Neptunes (which we define
as objects with mass greater than that of Neptune, and smaller than halfway
between that of Neptune and Saturn, i.e. 0.054 MJ<Mp<0.18 MJ).Comment: 11 pages, accepted for publication by Ap
HAT-P-57b: A Short-Period Giant Planet Transiting A Bright Rapidly Rotating A8V Star Confirmed Via Doppler Tomography
We present the discovery of HAT-P-57b, a P = 2.4653 day transiting planet
around a V = 10.465 +- 0.029 mag, Teff = 7500 +- 250 K main sequence A8V star
with a projected rotation velocity of v sin i = 102.1 +- 1.3 km s^-1. We
measure the radius of the planet to be R = 1.413 +- 0.054 R_J and, based on RV
observations, place a 95% confidence upper limit on its mass of M < 1.85 M_J .
Based on theoretical stellar evolution models, the host star has a mass and
radius of 1.47 +- 0.12 M_sun, and 1.500 +- 0.050 R_sun, respectively.
Spectroscopic observations made with Keck-I/HIRES during a partial transit
event show the Doppler shadow of HAT-P-57b moving across the average spectral
line profile of HAT-P- 57, confirming the object as a planetary system. We use
these observations, together with analytic formulae that we derive for the line
profile distortions, to determine the projected angle between the spin axis of
HAT-P-57 and the orbital axis of HAT-P-57b. The data permit two possible
solutions, with -16.7 deg < lambda < 3.3 deg or 27.6 deg < lambda < 57.4 deg at
95% confidence, and with relative probabilities for the two modes of 26% and
74%, respectively. Adaptive optics imaging with MMT/Clio2 reveals an object
located 2.7" from HAT-P-57 consisting of two point sources separated in turn
from each other by 0.22". The H and L -band magnitudes of the companion stars
are consistent with their being physically associated with HAT-P-57, in which
case they are stars of mass 0.61 +- 0.10 M_sun and 0.53 +- 0.08 M_sun. HAT-P-57
is the most rapidly rotating star, and only the fourth main sequence A star,
known to host a transiting planet.Comment: 18 pages, 14 figures, 5 tables, accepted for publication in A
HATS-15 b and HATS-16 b: Two massive planets transiting old G dwarf stars
We report the discovery of HATS-15 b and HATS-16 b, two massive transiting
extrasolar planets orbiting evolved ( Gyr) main-sequence stars. The
planet HATS-15 b, which is hosted by a G9V star ( mag), is a hot
Jupiter with mass of and radius of
, and completes its orbit in nearly 1.7 days.
HATS-16 b is a very massive hot Jupiter with mass of and radius of ; it orbits around
its G3 V parent star ( mag) in days. HATS-16 is slightly
active and shows a periodic photometric modulation, implying a rotational
period of 12 days which is unexpectedly short given its isochronal age. This
fast rotation might be the result of the tidal interaction between the star and
its planet.Comment: 16 pages, 8 figures, submitted to PAS
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