Cinématique stellaire | EPFL Graph Search

La cinématique stellaire est l'étude du mouvement des étoiles. Puisqu'elle ne cherche pas à comprendre les origines et causes du mouvement, la cinématique stellaire diffère de la dynamique stellaire, qui tient compte notamment des effets gravitationnels. La cinématique stellaire peut fournir des informations sur l'origine et l'âge des étoiles ainsi que sur la structure et l'évolution de la galaxie environnante. La cinématique stellaire distingue plusieurs types de mouvements individuels et collectifs d'étoiles. Courant stellaire Groupes cinématiques Un groupe d’étoiles qui ont un mouvement spatial et un âge similaire est connu sous le nom de groupe cinématique. Les astronomes peuvent déterminer si des étoiles font partie d’un groupe cinématique grâce à des caractéristiques physiques similaires telles l'âge, la métallicité et la cinématique (vitesse radiale et mouvement propre). Les étoiles parmi ces groupes ont souvent la même origine. Ils sont formés par la

Numerical model of Total Knee Replacement replicating chair rising

Tshahé Auria Anongba Varela

Although the procedure of total knee replacement (TKR) has been improved for the last decades, patients may still face postoperative complications. Specially, causes of complications related to patellar resurfacing, such as osteonecrosis, patellar bone fracture, anterior knee pain and implant failure, are still unclear. Predicting strain state of the patellar bone after TKR by means of numerical modeling may help in understanding and possibly preventing such complications. First TKR model has been already developed within LBO (built in Abaqus/Standard). The model replicates loaded squat movement (Oxford rig). As the model is planned to be applied to the real TKA patients and compared with their real kinematics, squat movement could be problematic to accomplish for these patients. Thus we want also ask them to perform chair rising movement. In the project we propose to extend existing model of squat to “chair rising” movement. First, the student should study existing in vivo studies of chair rising to estimate kinematics during the movement. And then to implement this movement in Abaqus. The aim is to estimate patellar bone strain during this movement.

2014

Thermo-hydro-mechanical behavior of energy tunnels

Matthias Timothee Stanislas Wojnarowicz

Subsurface geothermal in combination with Ground Heat Exchanger (GHE) and heat pumps systems had proved over the past decade to be an effective way in space heating and cooling. GHE’s embedded in geostructures such as tunnels has become more and more attractive in the current state where we try to mitigate greenhouse gas effects. The scope of this paper is to provide a fully coupled numerical model to assess the different physical aspects of an energy tunnel such as the kinetic and thermal boundaries layers development, thermally induce stress, and the heat generation. To do so, a finite element model is used to assess the heat exchange between, the GHE, the concrete lining, the air within the tunnel, the surrounding ground, and groundwater flow. The numerical model is then confronted with data from real-scale experimentation that was performed in Torino in 2018. The predictions from the numerical model show a quite good match with the data from the experimental prototype. Later on, similar models are generated to assess the effect of the heat exchange on air velocity and temperature within the tunnel as well as the induced thermal stress. The numerical results highlight the formation of both the kinematic and thermal boundary layer and shows that those boundaries are affected by the GHE’s activation. For the kinematic aspect, the lower temperatures observed in the vicinity of the heat exchangers tend to lower the velocity magnitude especially close to the wall surface. This change in velocity may be linked to a buoyancy effect cause by the lower temperature of the air in this regions. Indeed natural convection occurs along the tunnel, cooler fluid is pushed down while the warmer fluid rise; locally a lower temperature tends to decrease the viscosity of the fluid and increase its volumic mass. It was observed that the activation of GHE’s enhances this phenomenon in their vicinity due to the temperature gradient that they produce. Moreover, GHE’s activation tends to increase the overall turbulence of the flow and thus the eddies’ formation. The locations of those disturbance are difficult to predict due to the fact that small disturbance may generate large vorticity within the flow. However, it is shown that after passing the GHE zone, the velocity profile tends to stabilize to the undisturbed case. The kinematic entry length seems to happen further down the stream in the case where GHE’s are activated. This is due to the temperature disturbance generated by GHE’s activation. This phenomenon is increased with respect to the number of GHE loops activated. Furthermore, some probing was performed in the vicinity of the heat exchanger to assess the thermal induce stress due to the heating operation. The recorded stress shows peaks at early stages due to the higher temperature gradient that is generated between the GHE’s and concrete at beginning. Finally, after some time, the temperature reaches a steady state hence the stabilized thermal response recorded.

2020

UV-extended E-MILES stellar population models: young components in massive early-type galaxies

Elena Ricciardelli

We present UV-extended E-MILES stellar population synthesis models covering the spectral range.. 1680-50 000 angstrom at moderately high resolution. We employ the NGSL space-based stellar library to compute spectra of single-age, single-metallicity stellar populations in the wavelength range from 1680 to 3540 angstrom. These models represent a significant improvement in resolution and age/metallicity coverage over previous studies based on earlier space-based libraries. These model spectra were joined with those we computed in the visible using MILES, and other empirical libraries for redder wavelengths. The models span the metallicity range -1.79

Oxford Univ Press2016

Thermo-hydro-mechanical behavior of energy tunnels

Matthias Timothee Stanislas Wojnarowicz

2020