skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: Lower molar shape and size in prosimian and platyrrhine primates: S t . C lair and B oyer

Authors:
 [1];  [2]
  1. Center for Functional Anatomy and Evolution, Johns Hopkins University, Baltimore Maryland 21205
  2. Department of Evolutionary Anthropology, Duke University, Durham North Carolina 27708
Publication Date:
Sponsoring Org.:
USDOE Office of Environmental Management (EM)
OSTI Identifier:
1401697
Grant/Contract Number:
NSF DDIG BCS-0622544 to DM Boyer; NSF BCS 1304045 to DM Boyer and EM St. Clair
Resource Type:
Journal Article: Publisher's Accepted Manuscript
Journal Name:
American Journal of Physical Anthropology
Additional Journal Information:
Journal Volume: 161; Journal Issue: 2; Related Information: CHORUS Timestamp: 2017-10-20 17:42:25; Journal ID: ISSN 0002-9483
Publisher:
Wiley Blackwell (John Wiley & Sons)
Country of Publication:
United States
Language:
English

Citation Formats

St. Clair, Elizabeth M., and Boyer, Doug M.. Lower molar shape and size in prosimian and platyrrhine primates: S t . C lair and B oyer. United States: N. p., 2016. Web. doi:10.1002/ajpa.23021.
St. Clair, Elizabeth M., & Boyer, Doug M.. Lower molar shape and size in prosimian and platyrrhine primates: S t . C lair and B oyer. United States. doi:10.1002/ajpa.23021.
St. Clair, Elizabeth M., and Boyer, Doug M.. 2016. "Lower molar shape and size in prosimian and platyrrhine primates: S t . C lair and B oyer". United States. doi:10.1002/ajpa.23021.
@article{osti_1401697,
title = {Lower molar shape and size in prosimian and platyrrhine primates: S t . C lair and B oyer},
author = {St. Clair, Elizabeth M. and Boyer, Doug M.},
abstractNote = {},
doi = {10.1002/ajpa.23021},
journal = {American Journal of Physical Anthropology},
number = 2,
volume = 161,
place = {United States},
year = 2016,
month = 6
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record at 10.1002/ajpa.23021

Save / Share:
  • Cerium oxide nanoparticles were synthesized by solution combustion method with varying the oxidizer (cerium nitrate hexa hydrate) to fuel (Glycine) molar ratio. The prepared samples were characterized by UV-visible spectrometer, X-ray diffractometer (XRD), Scanning electron microscope (SEM) and Energy dispersive X-Ray analysis (EDAX). XRD pattern reveals the formation of cubic fluorite structure of CeO{sub 2}. It was observed that finest crystallites were found at extreme fuel-deficient condition and it is good enough to produce favorable powder characteristics. The average crystallite size was found to be 14.46 nm to 21.57 nm. The temperature dependent dc conductivity was carried out using Keithleymore » source meter between the temperature range from 300 K to 573 K. From this study it was found that the conductivity increases with increase of temperature due to semiconducting behavior of CeO{sub 2} and it decreases with particle size due to increase in the energy band gap.« less
  • LaIr/sub 2/Si/sub 2/ has a high-temperature form crystallizing in the primitive tetragonal CaBe/sub 2/Ge/sub 2/-type structure (space group P4/nmm; a = 4.191 A, c = 9.944 A), and a low-temperature form of the body-centered tetragonal ThCr/sub 2/Si/sub 2/ type (space group I4/mmm; a = 4.109 A, c = 10.299 A). Both structures are BaAl/sub 4/-type derivatives. The high-temperature modification may be quenched from above the transformation temperature of 1720 /sup 0/C and becomes superconducting at 1.6 K, while the low-temperature modification is normal down to 1 K. The structures of both modifications have been refined in single-crystal studies. The exceptionalmore » polymorphism of LaIr/sub 2/Si/sub 2/ is discussed, emphasizing structural relationships and the occurrence of superconductivity in the high-temperature modification.« less
  • Most, if not all, disk galaxies have a thin (classical) disk and a thick disk. In most models thick disks are thought to be a necessary consequence of the disk formation and/or evolution of the galaxy. We present the results of a study of the thick disk properties in a sample of carefully selected edge-on galaxies with types ranging from T = 3 to T = 8. We fitted one-dimensional luminosity profiles with physically motivated functions-the solutions of two stellar and one gaseous isothermal coupled disks in equilibrium-which are likely to yield more accurate results than other functions used inmore » previous studies. The images used for the fits come from the Spitzer Survey of Stellar Structure in Galaxies (S{sup 4}G). We found that thick disks are on average more massive than previously reported, mostly due to the selected fitting function. Typically, the thin and thick disks have similar masses. We also found that thick disks do not flare significantly within the observed range in galactocentric radii and that the ratio of thick-to-thin disk scale heights is higher for galaxies of earlier types. Our results tend to favor an in situ origin for most of the stars in the thick disk. In addition, the thick disk may contain a significant amount of stars coming from satellites accreted after the initial buildup of the galaxy and an extra fraction of stars coming from the secular heating of the thin disk by its own overdensities. Assigning thick disk light to the thin disk component may lead to an underestimate of the overall stellar mass in galaxies because of different mass-to-light ratios in the two disk components. On the basis of our new results, we estimate that disk stellar masses are between 10% and 50% higher than previously thought and we suggest that thick disks are a reservoir of 'local missing baryons'.« less
  • The nature and properties of dark matter (DM) are both outstanding issues in physics. Besides clustering in halos, the universal character of gravity implies that self-gravitating compact DM configurations-predicted by various models-might be spread throughout the universe. Their astrophysical signature can be used to probe fundamental particle physics, or to test alternative descriptions of compact objects in active galactic nuclei. Here, we discuss the most promising dissection tool of such configurations: the inspiral of a compact stellar-size object and consequent gravitational-wave (GW) emission. The inward motion of this ''test probe'' encodes unique information about the nature of the supermassive configuration.more » When the probe travels through some compact region we show, within a Newtonian approximation, that the quasi-adiabatic inspiral is mainly driven by DM accretion and by dynamical friction, rather than by radiation reaction. When accretion dominates, the frequency and amplitude of the GW signal produced during the latest stages of the inspiral are nearly constant. In the exterior region we study a model in which the inspiral is driven by GW and scalar-wave emission, described at a fully relativistic level. Resonances in the energy flux appear whenever the orbital frequency matches the effective mass of the DM particle, corresponding to the excitation of the central object's quasinormal frequencies. Unexpectedly, these resonances can lead to large dephasing with respect to standard inspiral templates, to such an extent as to prevent detection with matched filtering techniques. We discuss some observational consequences of these effects for GW detection.« less