Isotopic evidence of saber-tooth development, growth rate, and diet from the adult canine of Smilodon fatalis from Rancho La Brea

2004 ◽  
Vol 206 (3-4) ◽  
pp. 303-310 ◽  
Author(s):  
Robert S. Feranec
PLoS ONE ◽  
2016 ◽  
Vol 11 (9) ◽  
pp. e0162270 ◽  
Author(s):  
Wendy J. Binder ◽  
Kassaundra S. Cervantes ◽  
Julie A. Meachen

2012 ◽  
Vol 273 (9) ◽  
pp. 981-991 ◽  
Author(s):  
Adam Hartstone-Rose ◽  
Ryan C. Long ◽  
Aisling B. Farrell ◽  
Christopher A. Shaw

2021 ◽  
Vol 20 (2) ◽  
pp. 133
Author(s):  
Manuel J. Salesa ◽  
Mauricio Antón ◽  
Alan Turner ◽  
Jorge Morales

Los llamados “félidos dientes de sable” aparecen en el registro fósil a partir del Mioceno superior, desapareciendo hace tan solo unos 10.000 años. Los últimos representantes de este grupo fueron los cazadores dominantes en las comunidades de mamíferos de las que formaron parte. Su anatomía, altamente especializada, es bastante bien conocida gracias a yacimientos como Rancho La Brea (EEUU), del cual se conocen restos de miles de individuos de Smilodon fatalis. Sin embargo, muy poco se sabía sobre la anatomía de los primeros macairodontinos y sobre el origen de este modelo de depredador. El descubrimiento del complejo de yacimientos del Cerro de los Batallones (Torrejón de Velasco, Madrid) ha proporcionado gran cantidad de restos de uno de los macairodontinos más primitivos, Paramachairodus ogygia, lo que ha permitido estudiar en profundidad su anatomía funcional, en concreto en este trabajo el complejo cráneo-cervical, y proponer una hipótesis que explique el origen para este grupo tan especializado de carnívoros.  


BMC Biology ◽  
2021 ◽  
Vol 19 (1) ◽  
Author(s):  
Alistair R. Evans ◽  
Tahlia I. Pollock ◽  
Silke G. C. Cleuren ◽  
William M. G. Parker ◽  
Hazel L. Richards ◽  
...  

Abstract Background A major goal of evolutionary developmental biology is to discover general models and mechanisms that create the phenotypes of organisms. However, universal models of such fundamental growth and form are rare, presumably due to the limited number of physical laws and biological processes that influence growth. One such model is the logarithmic spiral, which has been purported to explain the growth of biological structures such as teeth, claws, horns, and beaks. However, the logarithmic spiral only describes the path of the structure through space, and cannot generate these shapes. Results Here we show a new universal model based on a power law between the radius of the structure and its length, which generates a shape called a ‘power cone’. We describe the underlying ‘power cascade’ model that explains the extreme diversity of tooth shapes in vertebrates, including humans, mammoths, sabre-toothed cats, tyrannosaurs and giant megalodon sharks. This model can be used to predict the age of mammals with ever-growing teeth, including elephants and rodents. We view this as the third general model of tooth development, along with the patterning cascade model for cusp number and spacing, and the inhibitory cascade model that predicts relative tooth size. Beyond the dentition, this new model also describes the growth of claws, horns, antlers and beaks of vertebrates, as well as the fangs and shells of invertebrates, and thorns and prickles of plants. Conclusions The power cone is generated when the radial power growth rate is unequal to the length power growth rate. The power cascade model operates independently of the logarithmic spiral and is present throughout diverse biological systems. The power cascade provides a mechanistic basis for the generation of these pointed structures across the tree of life.


Author(s):  
Wilfried Sigle ◽  
Matthias Hohenstein ◽  
Alfred Seeger

Prolonged electron irradiation of metals at elevated temperatures usually leads to the formation of large interstitial-type dislocation loops. The growth rate of the loops is proportional to the total cross-section for atom displacement,which is implicitly connected with the threshold energy for atom displacement, Ed . Thus, by measuring the growth rate as a function of the electron energy and the orientation of the specimen with respect to the electron beam, the anisotropy of Ed can be determined rather precisely. We have performed such experiments in situ in high-voltage electron microscopes on Ag and Au at 473K as a function of the orientation and on Au as a function of temperature at several fixed orientations.Whereas in Ag minima of Ed are found close to <100>,<110>, and <210> (13-18eV), (Fig.1) atom displacement in Au requires least energy along <100>(15-19eV) (Fig.2). Au is thus the first fcc metal in which the absolute minimum of the threshold energy has been established not to lie in or close to the <110> direction.


2020 ◽  
Vol 640 ◽  
pp. A53
Author(s):  
L. Löhnert ◽  
S. Krätschmer ◽  
A. G. Peeters

Here, we address the turbulent dynamics of the gravitational instability in accretion disks, retaining both radiative cooling and irradiation. Due to radiative cooling, the disk is unstable for all values of the Toomre parameter, and an accurate estimate of the maximum growth rate is derived analytically. A detailed study of the turbulent spectra shows a rapid decay with an azimuthal wave number stronger than ky−3, whereas the spectrum is more broad in the radial direction and shows a scaling in the range kx−3 to kx−2. The radial component of the radial velocity profile consists of a superposition of shocks of different heights, and is similar to that found in Burgers’ turbulence. Assuming saturation occurs through nonlinear wave steepening leading to shock formation, we developed a mixing-length model in which the typical length scale is related to the average radial distance between shocks. Furthermore, since the numerical simulations show that linear drive is necessary in order to sustain turbulence, we used the growth rate of the most unstable mode to estimate the typical timescale. The mixing-length model that was obtained agrees well with numerical simulations. The model gives an analytic expression for the turbulent viscosity as a function of the Toomre parameter and cooling time. It predicts that relevant values of α = 10−3 can be obtained in disks that have a Toomre parameter as high as Q ≈ 10.


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