13,571 research outputs found
Jupiter as a Giant Cosmic Ray Detector
We explore the feasibility of using the atmosphere of Jupiter to detect
Ultra-High-Energy Cosmic Rays (UHECR's). The large surface area of Jupiter
allows us to probe cosmic rays of higher energies than previously accessible.
Cosmic ray extensive air showers in Jupiter's atmosphere could in principle be
detected by the Large Area Telescope (LAT) on the Fermi observatory. In order
to be observed, these air showers would need to be oriented toward the Earth,
and would need to occur sufficiently high in the atmosphere that the gamma rays
can penetrate. We demonstrate that, under these assumptions, Jupiter provides
an effective cosmic ray "detector" area of km. We predict
that Fermi-LAT should be able to detect events of energy eV with
fluence erg cm at a rate of about one per month. The observed
number of air showers may provide an indirect measure of the flux of cosmic
rays eV. Extensive air showers also produce a synchrotron
signature that may be measurable by ALMA. Simultaneous observations of Jupiter
with ALMA and Fermi-LAT could be used to provide broad constraints on the
energies of the initiating cosmic rays.Comment: 8 pages, 5 figures. Accepted for publication in the Astrophysical
Journal Letter
Visual and control aspects of saccadic eye movements
Physiological, behavioral, and control investigation of rapid saccadic jump eye movement in human
Anomalous isotopic predissociation in the F³Πu(v=1) state of Oâ
Using a tunable, narrow-bandwidth vacuum-ultraviolet source based on third-harmonic generation from excimer-pumped dye-laser radiation, the F³ΠuâX³Σg-(1,0)photoabsorption cross sections of Âčâ¶Oâ and ÂčâžOâ have been recorded in high resolution. Rotational analyses have been performed and the resultant F(v=1) term values fitted to the ³ΠHamiltonian of Brown and Merer [J. Mol. Spectrosc. 74, 488 (1979)]. A large rotationless isotope effect is observed in the F(v=1)predissociation, wherein the Lorentzian linewidth component for ÂčâžOâ is a factor of âŒ50 smaller than the corresponding Âčâ¶Oâlinewidth. This effect, a consequence of the nonadiabatic rotationless predissociation mechanism, is described using a coupled-channel treatment of the strongly Rydberg-valence-mixed 3Î u states. Significant J, e/f-parity, and sublevel dependencies observed in the isotopic F(v=1) rotational widths are found to derive from an indirect predissociation mechanism involving an accidental degeneracy with the E³Σâu(v=3) level, itself strongly predissociated by ³Σâu Rydberg-valence interactions, together with L-uncoupling (rotational) interactions between the Rydberg components of the F and E states. Transitions into the E(v=3) level are observed directly for the first time, specifically in the ÂčâžOâ spectrumPartial support
was provided by an NSF International Opportunities for Scientists
and Engineers Program Grant No. INT-9513350, and
Visiting Fellowships for G.S. and J.B.W. at the Australian
National University
Ionisation and discharge in cloud-forming atmospheres of brown dwarfs and extrasolar planets
Brown dwarfs and giant gas extrasolar planets have cold atmospheres with rich chemical compositions from which mineral cloud particles form. Their properties, like particle sizes and material composition, vary with height, and the mineral cloud particles are charged due to triboelectric processes in such dynamic atmospheres. The dynamics of the atmospheric gas is driven by the irradiating host star and/or by the rotation of the objects that changes during its lifetime. Thermal gas ionisation in these ultra-cool but dense atmospheres allows electrostatic interactions and magnetic coupling of a substantial atmosphere volume. Combined with a strong magnetic field , a chromosphere and aurorae might form as suggested by radio and x-ray observations of brown dwarfs. Non-equilibrium processes like cosmic ray ionisation and discharge processes in clouds will increase the local pool of free electrons in the gas. Cosmic rays and lighting discharges also alter the composition of the local atmospheric gas such that tracer molecules might be identified. Cosmic rays affect the atmosphere through air showers in a certain volume which was modelled with a 3D Monte Carlo radiative transfer code to be able to visualise their spacial extent. Given a certain degree of thermal ionisation of the atmospheric gas, we suggest that electron attachment to charge mineral cloud particles is too inefficient to cause an electrostatic disruption of the cloud particles. Cloud particles will therefore not be destroyed by Coulomb explosion for the local temperature in the collisional dominated brown dwarf and giant gas planet atmospheres. However, the cloud particles are destroyed electrostatically in regions with strong gas ionisation. The potential size of such cloud holes would, however, be too small and might occur too far inside the cloud to mimic the effect of, e.g. magnetic field induced star spots
Oscillator strengths and line widths of dipole-allowed transitions in ÂčâŽNâ between 89.7 and 93.5ânm
Line oscillator strengths in the 20 electric dipole-allowed bands of ÂčâŽNâ in the 89.7â93.5nm (111480â106950cmâ»Âč) region are reported from photoabsorptionmeasurements at an instrumental resolution of âŒ6mĂ
(0.7cmâ»Âč) full width at half maximum. The absorptionspectrum comprises transitions to vibrational levels of the 3pÏᔀcâČâÂčΣᔀâș, 3pÏᔀc³Πᔀ, and 3sÏgoâÂčΠᔀRydberg states and of the bâČÂčΣᔀâș and bÂčΠᔀ valence states. The J dependences of band f values derived from the experimental line f values are reported as polynomials in JâČ(JâČ+1) and are extrapolated to JâČ=0 in order to facilitate comparisons with results of coupled Schrödinger-equation calculations. Most bands in this study are characterized by a strong J dependence of the band f values and display anomalous P-, Q-, and R-branch intensity patterns. Predissociation line widths, which are reported for 11 bands, also exhibit strong J dependences. The f value and line width patterns can inform current efforts to develop comprehensive spectroscopic models that incorporate rotational effects and predissociation mechanisms, and they are critical for the construction of realistic atmospheric radiative-transfer models.This work was supported in part by NASA Grant No.
NNG05GA03G to Wellesley College and Australian Research
Council Discovery Program Grant No. DP0558962
Microscopic Black Hole Production in TeV-Scale Gravity
Models with extra spatial dimensions and TeV-scale gravity offer the first
opportunity to test the conjecture of black hole formation in trans-Planckian
energy scattering with small impact parameters. After a brief review of
gravitational scattering at ultrahigh energies and scenarios of TeV-scale
gravity, search strategies at the LHC, at the Pierre Auger (cosmic ray)
Observatory and at the neutrino telescopes AMANDA/IceCube are illustrated with
the simplest but nevertheless representative example: production of
Schwarzschild black holes and their observation via Hawking radiation in the
large extra dimension scenario. Some more general features of the production of
higher-dimensional black holes and/or uncertainties in the estimates are also
outlined.Comment: 18 pages, 5 figures; Talk presented at XXX ITEP Winter School of
Physics, Moscow, Russia, February 2002, references adde
The influence of expertise on brain activation of the action observation network during anticipation of tennis and volleyball serves
In many daily activities, and especially in sport, it is necessary to predict the effects of others' actions in order to initiate appropriate responses. Recently, researchers have suggested that the action-observation network (AON) including the cerebellum plays an essential role during such anticipation, particularly in sport expert performers. In the present study, we examined the influence of task-specific expertise on the AON by investigating differences between two expert groups trained in different sports while anticipating action effects. Altogether, 15 tennis and 16 volleyball experts anticipated the direction of observed tennis and volleyball serves while undergoing functional magnetic resonance imaging (fMRI). The expert group in each sport acted as novice controls in the other sport with which they had only little experience. When contrasting anticipation in both expertise conditions with the corresponding untrained sport, a stronger activation of AON areas (SPL, SMA), and particularly of cerebellar structures, was observed. Furthermore, the neural activation within the cerebellum and the SPL was linearly correlated with participant's anticipation performance, irrespective of the specific expertise. For the SPL, this relationship also holds when an expert performs a domain-specific anticipation task. Notably, the stronger activation of the cerebellum as well as of the SMA and the SPL in the expertise conditions suggests that experts rely on their more fine-tuned perceptual-motor representations that have improved during years of training when anticipating the effects of others' actions in their preferred sport. The association of activation within the SPL and the cerebellum with the task achievement suggests that these areas are the predominant brain sites involved in fast motor predictions. The SPL reflects the processing of domain-specific contextual information and the cerebellum the usage of a predictive internal model to solve the anticipation task. © 2014 Balser, Lorey, Pilgramm, Naumann, Kindermann, Stark, Zentgraf, Williams and Munzert
Pistachio (Pistacia vera) domestication and dispersal out of Central Asia
The pistachio (Pistacia vera L.) is commercially cultivated in semi-arid regions around the globe. Archaeobotanical, genetic, and linguistic data suggest that the pistachio was brought under cultivation somewhere within its wild range, spanning southern Central Asia, northern Iran, and northern Afghanistan. Historically, pistachio cultivation has primarily relied on grafting, suggesting that, as with many Eurasian tree crops, domestication resulted from genetically locking hybrids or favored individuals in place. Plant domestication and dispersal research has largely focused on weedy, highly adaptable, self-compatible annuals; in this discussion, we present a case study that involves a dioecious long-lived perennialmdash;a domestication process that would have required a completely different traditional ecological knowledge system than that utilized for grain cultivation. We argue that the pistachio was brought under cultivation in southern Central Asia, spreading westward by at least 2000 years ago (maybe a few centuries earlier to the mountains of modern Syria) and moved eastward only at the end of the first millennium AD. The seeds remain rare in archaeological sites outside its native range, even into the mid-second millennium AD, and may not have been widely cultivated until the past few hundred years.1. Introduction 1.1. Botany and Ecology 1.2. Progenitor Range and Ecology 2. Domestication 2.1. Grafting and Pollination 2.2. Archaeobotanical and Historical Sources 2.3. ArchaeobotanyâCentral Asian Data 3. Debated Early Evidence 4. Dispersal 5. Linguistics 6. Conclusion
Keck Spectroscopy of Faint 3<z<8 Lyman Break Galaxies:- Evidence for a Declining Fraction of Emission Line Sources In the Redshift Range 6<z<8
Using deep Keck spectroscopy of Lyman break galaxies selected from infrared
imaging data taken with WFC3/IR onboard the Hubble Space Telescope, we present
new evidence for a reversal in the redshift-dependent fraction of star forming
galaxies with detectable Lyman alpha emission in the redshift range 6.3 < z <
8.8. Our earlier surveys with the DEIMOS spectrograph demonstrated a
significant increase with redshift in the fraction of line emitting galaxies
over the interval 4 < z < 6, particularly for intrinsically faint systems which
dominate the luminosity density. Using the longer wavelength sensitivities of
LRIS and NIRSPEC, we have targeted 19 Lyman break galaxies selected using
recent WFC3/IR data whose photometric redshifts are in the range 6.3 < z < 8.8
and which span a wide range of intrinsic luminosities. Our spectroscopic
exposures typically reach a 5-sigma sensitivity of < 50 A for the rest-frame
equivalent width (EW) of Lyman alpha emission. Despite the high fraction of
emitters seen only a few hundred million years later, we find only 2 convincing
and 1 possible line emitter in our more distant sample. Combining with
published data on a further 7 sources obtained using FORS2 on the ESO VLT, and
assuming continuity in the trends found at lower redshift, we discuss the
significance of this apparent reversal in the redshift-dependent Lyman alpha
fraction in the context of our range in continuum luminosity. Assuming all the
targeted sources are at their photometric redshift and our assumptions about
the Lyman alpha EW distribution are correct, we would expect to find so few
emitters in less than 1% of the realizations drawn from our lower redshift
samples. Our new results provide further support for the suggestion that, at
the redshifts now being probed spectroscopically, we are entering the era where
the intergalactic medium is partially neutral.Comment: 8 pages, 5 figures, Accepted to ApJ 10/1/1
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