Search

Your search keyword '"Mastropietro C"' showing total 4 results
Start Over Author "Mastropietro C" Topic astrophysics
4 results on '"Mastropietro C"'

1. The Magellanic Clouds as a template for the study of stellar populations and galaxy interactions

Author

Cioni, M. -R. L., Bekki, K., Clementini, G., de Blok, W. J. G., Emerson, J. P., Evans, C. J., de Grijs, R., Gibson, B. K., Girardi, L., Groenewegen, M. A. T., Ivanov, V. D., Leisy, P., Marconi, M., Mastropietro, C., Moore, B., Naylor, T., Oliveira, J. M., Ripepi, V., van Loon, J. Th., Wilkinson, M. I., and Wood, P. R.

Subjects
Astrophysics
Abstract

The Magellanic System represents one of the best places to study the formation and evolution of galaxies. Photometric surveys of various depths, areas and wavelengths have had a significant impact on our understanding of the system; however, a complete picture is still lacking. VMC (the VISTA near-infrared YJKs survey of the Magellanic System) will provide new data to derive the spatially resolved star formation history and to construct a three-dimensional map of the system. These data combined with those from other ongoing and planned surveys will give us an absolutely unique view of the system opening up the doors to truly new science!, Comment: 8 pages, 12 figures, to appear in PASA as a key contribution to the Elizabeth and Frederic White conference on the Magellanic System (Sydney 16-17 July 2007). Replaced with refereed version

Published
2007
Full Text
View/download PDF

2. On the formation of the Magellanic Stream

Author

Mastropietro, C., Moore, B., Mayer, L., Stadel, J., and Wadsley, J.

Subjects
Astrophysics
Abstract

We use high resolution N-Body/SPH simulations to study the hydro-dynamical and gravitational interaction between the Large Magellanic Cloud and the Milky Way. We model the dark and hot extended halo components as well as the stellar/gaseous disks of the two galaxies. Tidal forces distort the LMC's disk, forcing a bar and creating a diffuse stellar halo and a strong warp, although very few stars are unbound from the LMC. Ram-pressure from a low density ionised halo is then sufficient to remove $1.4 \times 10^8M_\odot$ of gas from the LMC's disk forming a great circle trailing stream around the Galaxy., Comment: 4 pages, 2 figures, to be published in the proceedings of the "Satellite and Tidal Streams", La Palma 26-30 May 2003, Spain, eds. F. Prada, D. Martinez-Delgado, T. Mahoney

Published
2003

3. Ram-Pressure Induced Star Formation in the LMC

Author

Chiara Mastropietro, Ben Moore, Andreas Burkert, University of Zurich, and Mastropietro, C

Subjects
galaxies: Magellanic Clouds — methods: n, Physics, 530 Physics, Star formation, Milky Way, Astronomy, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, body simulations, Galaxy, Ram pressure, 1912 Space and Planetary Science, Space and Planetary Science, Planet, 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Halo, Large Magellanic Cloud, Astrophysics::Galaxy Astrophysics
Abstract

We use high-resolution n-body/SPH simulations to study the hydrodynamical interaction between the Large Magellanic Cloud and the hot halo of the Milky Way. We investigate whether the ram-pressure acting on the gaseous disk of the satellite can explain the peculiarities observed in the Hidistribution and the location of the recent star formation activity.

Published
2008
Full Text
View/download PDF

4. Effects of ram pressure on the gas distribution and star formation in the Large Magellanic Cloud

Author

Andreas Burkert, Ben Moore, Chiara Mastropietro, University of Zurich, Mastropietro, C, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Universitätssternwarte der Ludwig-Maximiliansuniversität, and Institute für Theoretische Physik, Universität Zürich

Subjects
Leading edge, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 530 Physics, Milky Way, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, methods: N, 1912 Space and Planetary Science, 0103 physical sciences, galaxies: interactions, Large Magellanic Cloud, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, body simulations, Ram pressure, Space and Planetary Science, 10231 Institute for Computational Science, Orbital motion, hydrodynamics, 3103 Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Halo, Supergiant, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: individual: LMC, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use high resolution N-body/SPH simulations to study the hydrodynamical interaction between the Large Magellanic Cloud (LMC) and the hot halo of the Milky Way. We investigate whether ram-pressure acting on the satellite's ISM can explain the peculiarities observed in the HI distribution and the location of the recent star formation activity. Due to the present nearly edge-on orientation of the disk with respect to the orbital motion, compression at the leading edge can explain the high density region observed in HI at the south-east border. In the case of a face-on disk (according to Mastropietro et al. 2008 the LMC was moving almost face-on before the last perigalactic passage), ram-pressure directed perpendicularly to the disk produces a clumpy structure characterized by voids and high density filaments that resemble those observed by the Parkes HI survey. As a consequence of the very recent edge-on motion, the H-alpha emission is mainly concentrated on the eastern side where 30 Doradus and most of the supergiant shells are located, although some H-alpha complexes form a patchy distribution on the entire disk. In this scenario only the youngest stellar complexes show a progression in age along the leading border of the disk., 18 pages, 18 figures, submitted to MNRAS

Published
2009
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results