Cdmx
3 Papers
Cdmx is an academic researcher. The author has contributed to research in topics: Supernova & Stars. The author has an hindex of 1, co-authored 3 publications.
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Papers
The sculpting of rectangular and jet-like morphologies in supernova remnants by anisotropic equatorially-confined progenitor stellar winds
Pablo F. Velázquez,D. M.-A. Meyer,A. Chiotellis,Arminda Cruz-Álvarez,E. M. Schneiter,J. C. Toledo-Roy,Estela Marta Reynoso,A. E. I. D. C. Nucleares,Universidad Nacional Autnoma de M'exico,Ap. 70-543,Cdmx,04510,M'exico Universitat Potsdam,Institut fur Physik und Astronomie,Karl-Liebknecht-Strasse 2425,14476 Potsdam,G. Astronomy,Astrophysics,Space Applications,R Sensing,National Observatory of Athens,15236,Penteli,Greece 4rth Lykeion Acharnon,Acharneon Ippeon,Paliggenesias,136 74 Acharnes,Greece Departamento de Materiales y Tecnolog'ia,FCEFyN-UNC,Av. V'elez Sarsfield 1611,C'ordoba,A. I. D. A. Y. F. D. Espacio,Av. Int. Guiraldes 2620,P. Iafe,Ciudad Universitaria,1428,Buenos Aires,Argentina +37 more
TL;DR: In this paper , the authors used three-dimensional magnetohydrodynamic simulations to show that rectangular and jet-like morphologies can be explained by supernovae (SNe), either type Ia or type II, expanding within anisotropic, bipolar stellar wind bubbles driven by the progenitor star.
Boltzmann-Poisson-like approach to simulating the galactic halo response to satellite accretion Dependence on the halo density profile
G. Aguilar-Arguello,Octavio Valenzuela,Arturo Trelles Universidad Nacional Aut'onoma de M'exico,I. D. Astronom'ia,Cdmx,M'exico. +5 more
TL;DR: In this article , a collisionless Boltzmann equation (CBE) + Poisson solver was used to simulate the density and velocity response modes in simulations of galactic-type DM halos accreting LMC-sized satellites.
2
Rectangular core-collapse supernova remnants: Application to Puppis A
D. M.-A. Meyer,Pablo F. Velázquez,Oleh Petruk,A. Chiotellis,M. Pohl,F. Camps-Farina,M. Petrov,Estela Marta Reynoso,J. C. Toledo-Roy,E. M. Schneiter,A. Castellanos-Ramírez,A. Potsdam,Institut fur Physik und Astronomie,Karl-Liebknecht-Strasse 2425,14476 Potsdam,G. I. D. C. Nucleares,Universidad Nacional Autonoma de Mexico,C. 04510,Mexico City,Mexico Institute for Applied Problems in Mechanics,Mathematics,Nas Ukraine,Naukova 3-b,79060 Lviv,Ukraine Astronomical Observatory of Taras Shevchenko Natio Kyiv,3. O. S. Kyiv,04053,UK Institute for Astronomy,Astrophysics,Space Applications,R Sensing,National Observatory of Athens,15236,Penteli,6. GreeceDESYPlatanenallee,15738 Zeuthen,G. F. S. D. D. A. Y. Astrof'isica,U. Madrid,28014 Madrid,Spain Max Planck Computing,D. Facility,2. Giessenbachstrasse,D. Garching,G. I. D. A. Y. F. D. Espacio,Av. Int. Guiraldes 2620,P. Iafe,Ciudad Universitaria,1428,Buenos Aires,Argentina Departamento de Materiales y Tecnolog'ia,FCEFyN-UNC,Av. V'elez Sarsfield 1611,C'ordoba,Argentina Universidad Nacional Aut'onoma de M'exico,I. D. Astronom'ia,A. 70-264,Cdmx,04510,M'exico. +58 more
TL;DR: In this article , it was shown through 2.5D magneto-hydrodynamical simulations, in the context of a Wolf-Rayet-evolving star, that it affects the development of its supernova remnant, which adopts a tubular shape that results from the interaction between the isotropic supernova ejecta and the stellar progenitor bubble into which the supernova blast wave expands.