Incorporation of a gravity wave momentum deposition parameterization into the Venus Thermosphere General Circulation Model (VTGCM)

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/96657/1/jgre20038.pd

Discovery of carbon monoxide in the upper atmosphere of Pluto

Pluto's icy surface has changed colour and its atmosphere has swelled since its last closest approach to the Sun in 1989. The thin atmosphere is produced by evaporating ices, and so can also change rapidly, and in particular carbon monoxide should be present as an active thermostat. Here we report the discovery of gaseous CO via the 1.3mm wavelength J=2-1 rotational transition, and find that the line-centre signal is more than twice as bright as a tentative result obtained by Bockelee-Morvan et al. in 2000. Greater surface-ice evaporation over the last decade could explain this, or increased pressure could have caused the atmosphere to expand. The gas must be cold, with a narrow line-width consistent with temperatures around 50 K, as predicted for the very high atmosphere, and the line brightness implies that CO molecules extend up to approximately 3 Pluto radii above the surface. The upper atmosphere must have changed markedly over only a decade since the prior search, and more alterations could occur by the arrival of the New Horizons mission in 2015.Comment: 5 pages; accepted for publication in MNRAS Letter

Seasonal melting and the formation of sedimentary rocks on Mars, with predictions for the Gale Crater mound

A model for the formation and distribution of sedimentary rocks on Mars is proposed. The rate-limiting step is supply of liquid water from seasonal melting of snow or ice. The model is run for a O(10^2) mbar pure CO2 atmosphere, dusty snow, and solar luminosity reduced by 23%. For these conditions snow only melts near the equator, and only when obliquity >40 degrees, eccentricity >0.12, and perihelion occurs near equinox. These requirements for melting are satisfied by 0.01-20% of the probability distribution of Mars' past spin-orbit parameters. Total melt production is sufficient to account for aqueous alteration of the sedimentary rocks. The pattern of seasonal snowmelt is integrated over all spin-orbit parameters and compared to the observed distribution of sedimentary rocks. The global distribution of snowmelt has maxima in Valles Marineris, Meridiani Planum and Gale Crater. These correspond to maxima in the sedimentary-rock distribution. Higher pressures and especially higher temperatures lead to melting over a broader range of spin-orbit parameters. The pattern of sedimentary rocks on Mars is most consistent with a Mars paleoclimate that only rarely produced enough meltwater to precipitate aqueous cements and indurate sediment. The results suggest intermittency of snowmelt and long globally-dry intervals, unfavorable for past life on Mars. This model makes testable predictions for the Mars Science Laboratory rover at Gale Crater. Gale Crater is predicted to be a hemispheric maximum for snowmelt on Mars.Comment: Submitted to Icarus. Minor changes from submitted versio

INFRARED AND VISIBLE PHOTON UPCONVERSION IN PRASEODYMIUM(III) DOPED LANTHANUM-FLUORIDE AND LANTHANUM-CHLORIDE(NEODYMIUM(III)).

Abstract not availabl

Aboriginal Adaptations on the Colorado Plateau: A View from the Island-in-the-Sky, Canyonlands National Park, Utah

This final report documents the results of archaeological inventory, excavation, and analysis of prehistoric cultural resources within a 45-kilometer (28-mile) long corridor in the Island-in-the-Sky District of Canyonlands National Park, Utah. During three field seasons of survey, mapping, and excavation in 1983-1985, the research team recorded 32 artifact scatters, plotted 90,000 prehistoric artifacts and 250 historic items, completed 600 one-square-meter test pits, and conducted 10 block excavations. Block excavations at two locations in Gray\u27s Pasture revealed a plant processing/hunting field camp (42SA16858) and a disturbed pithouse (42SA8506). Associated features and materials included a puddled clay-lined hearth, a slab-lined pit, a cached Mesa Verde Black-on-white olla, six additional restored ceramic vessels, chipped and ground stone tools, human remains, animal bone, and macrobotanical material. Radiometric determinations for these locations ranged from 1335 B.P. (corrected A.D. 690-795) to 940 B.P. (corrected A.D. 620-895). Radiometric dates for sites examined within the project area ranged from 2990 B.P. (corrected 1400-925 B.C.) to 120 B.P. (corrected A.D. 1655-1950). Research problems for this project included aboriginal patterns of land use, paleonutrition/diet/health, food storage, and caching strategies. Special emphasis was given to the investigation of artifact assemblage-diversity at varying spatial scales within surface artifact scatters

2007: The 2003 November 14 occultation by Titan of TYC 1343-1865-1. II. Analysis of light curves

Abstract We observed a stellar occultation by Titan on 2003 November 14 from La Palma Observatory using ULTRACAM with three Sloan filters: u , g , and i (358, 487, and 758 nm, respectively). The occultation probed latitudes 2 • S and 1 • N during immersion and emersion, respectively. A prominent central flash was present in only the i filter, indicating wavelength-dependent atmospheric extinction. We inverted the light curves to obtain six lower-limit temperature profiles between 335 and 485 km (0.04 and 0.003 mb) altitude. The i profiles agreed with the temperature measured by the Huygens Atmospheric Structure Instrument [Fulchignoni, M., and 43 colleagues, 2005. Nature 438, 785-791] above 415 km (0.01 mb). The profiles obtained from different wavelength filters systematically diverge as altitude decreases, which implies significant extinction in the light curves. Applying an extinction model [Elliot, J.L., Young, L.A., 1992. Astron. J. 103, 991-1015] gave the altitudes of line of sight optical depth equal to unity: 396 ± 7 and 401 ± 20 km (u immersion and emersion); 354 ± 7 and 387 ± 7 km (g immersion and emersion); and 336 ± 5 and 318 ± 4 km (i immersion and emersion). Further analysis showed that the optical depth follows a power law in wavelength with index 1.3 ± 0.2. We present a new method for determining temperature from scintillation spikes in the occulting body's atmosphere. Temperatures derived with this method are equal to or warmer than those measured by the Huygens Atmospheric Structure Instrument. Using the highly structured, three-peaked central flash, we confirmed the shape of Titan's middle atmosphere using a model originally derived for a previous Tita

GAS6/AXL Axis Regulates Prostate Cancer Invasion, Proliferation, and Survival in the Bone Marrow Niche12

Our recent studies have shown that annexin II, expressed on the cell surface of osteoblasts, plays an important role in the adhesion of hematopoietic stem cells (HSCs) to the endosteal niche. Similarly, prostate cancer (PCa) cells express the annexin II receptor and seem to use the stem cell niche for homing to the bone marrow. The role of the niche is thought to be the induction and sustenance of HSC dormancy. If metastatic PCa cells occupy a similar or the same ecological niche as HSCs, then it is likely that the initial role of the HSC niche will be to induce dormancy in metastatic cells. In this study, we demonstrate that the binding of PCa to annexin II induces the expression of the growth arrest-specific 6 (GAS6) receptors AXL, Sky, and Mer, which, in the hematopoietic system, induce dormancy. In addition, GAS6 produced by osteoblasts prevents PCa proliferation and protects PCa from chemotherapy-induced apoptosis. Our results suggest that the activation of GAS6 receptors on PCa in the bone marrow environment may play a critical role as a molecular switch, establishing metastatic tumor cell dormancy

Atmospheric Dynamics of Terrestrial Planets

The solar system presents us with a number of planetary bodies with shallow atmospheres that are sufficiently Earth-like in their form and structure to be termed “terrestrial.” These atmospheres have much in common, in having circulations that are driven primarily by heating from the Sun and radiative cooling to space, which vary markedly with latitude. The principal response to this forcing is typically in the form of a (roughly zonally symmetric) meridional overturning that transports heat vertically upward and in latitude. But even within the solar system, these planets exhibit many differences in the types of large-scale waves and instabilities that also contribute substantially to determining their respective climates. Here we argue that the study of simplified models (either numerical simulations or laboratory experiments) provides considerable insights into the likely roles of planetary size, rotation, thermal stratification, and other factors in determining the styles of global circulation and dominant waves and instability processes. We discuss the importance of a number of key dimensionless parameters, for example, the thermal Rossby and the Burger numbers as well as nondimensional measures of the frictional or radiative timescales, in defining the type of circulation regime to be expected in a prototypical planetary atmosphere subject to axisymmetric driving. These considerations help to place each of the solar system terrestrial planets into an appropriate dynamical context and also lay the foundations for predicting and understanding the climate and circulation regimes of (as yet undiscovered) Earth-like extrasolar planets. However, as recent discoveries of “super-Earth” planets around some nearby stars are beginning to reveal, this parameter space is likely to be incomplete, and other factors, such as the possibility of tidally locked rotation and tidal forcing, may also need to be taken into account for some classes of extrasolar planet

The 2003 November 14 occultation by Titan of TYC 1343-1865-1. II. Analysis of light curves

We observed a stellar occultation by Titan on 2003 November 14 from La Palma Observatory using ULTRACAM with three Sloan filters: u', g', and i' (358, 487, and 758 nm, respectively). The occultation probed latitudes 2 degrees S and 1 degrees N during immersion and emersion, respectively. A prominent central flash was present in only the i' filter, indicating wavelength-dependent atmospheric extinction. We inverted the light curves to obtain six lower-limit temperature profiles between 335 and 485 km (0.04 and 0.003 mb) altitude. The i' profiles agreed with the temperature measured by the Huygens Atmospheric Structure Instrument [Fulchignoni, M., and 43 colleagues, 2005. Nature 438, 785-791] above 415 km (0.01 mb). The profiles obtained from different wavelength filters systematically diverge as altitude decreases, which implies significant extinction in the light curves. Applying an extinction model [Elliot, J.L., Young, L.A., 1992. Astron. J. 103, 991-1015] gave the attitudes of line of sight optical depth equal to unity: 396 +/- 7 and 401 +/- 20 km (u' immersion and emersion); 354 7 and 387 +/- 7 km (g' immersion and emersion); and 336 +/- 5 and 318 +/- 4 km (i' immersion and emersion). Further analysis showed that the optical depth follows a power law in wavelength with index 1.3 +/- 0.2. We present a new method for determining temperature from scintillation spikes in the occulting body's atmosphere. Temperatures derived with this method are equal to or warmer than those measured by the Huygens Atmospheric Structure Instrument. Using the highly structured, three-peaked central flash, we confirmed the shape of Titan's middle atmosphere using a model originally derived for a previous Titan occultation