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Evolutionary sequences of stellar models with new radiative opacities. VI.

We present a large grid of stellar evolutionary models with the initial chemical composition . These tracks are conceived to extend the grid of stellar models described in the previous papers of this series, and are computed with the new radiative opacities by Iglesias et al. (1992) and convective overshoot. The tracks span the range of initial masses from to , and extend from...

Theory of stellar population synthesis with an application to N-body simulations

Aparicio , A. , & Gallart , C. 1995 , AJ, 110 , 2105 Aparicio , A. , Gallart , C. , Chiosi , C. , & Bertelli , G. 1996 , ApJ, 469 , L97 Aparicio , A. , Gallart , C. , & Bertelli , G. 1997 , AJ, 114 , 680

Detailed AGB evolutionary models and near-infrared colours of intermediate-age stellar populations: tests on star clusters

We investigate the influence of asymptotic giant branch (AGB) stars on integrated colours of star clusters of ages between ~100 Myr and a few gigayears, and composition typical for the Magellanic Clouds. We use state-of-the-art stellar evolution models that cover the full thermal pulse phase, and take the influence of dusty envelopes on the emerging spectra into account. We...

Dissipative phenomena in extended-body interactions - I. Methods: Dwarf galaxies of the Local Group and their synthetic CMDs

Aims. Dissipative phenomena occurring during the orbital evolution of a dwarf satellite galaxy around a host galaxy may leave signatures in the star formation activity and signatures in the colour-magnitude diagram of the galaxy stellar content. Our goal is to reach a simple and qualitative description of these complicated phenomena.Methods. We develop an analytical and numerical...

EvoL: the new Padova Tree-SPH parallel code for cosmological simulations - I. Basic code: gravity and hydrodynamics

core of the old Pd -Tsph code was written during the ’90s by C. Chiosi, G. Carraro, C. Lia and C. Dalla Vecchia (Carraro et al. 1998; Lia et al. 2002) . Over the years, many researchers added their

Orbital evolution of the Carina dwarf galaxy and self-consistent determination of star formation history

, AJ, 139, 59 Burkert, A. 1997, ApJ, 474, L99 Cannon, R. D., Hawarden, T. G., & Tritton, S. B. 1977, MNRAS, 180, 81P Carpintero, D. D., & Aguilar, L. A. 1998, MNRAS, 298, 1 Carraro, G., Lia, C., & Chiosi

Morphological evolution of dwarf galaxies in the Local Group

. , & Lia , C. 2001 , MNRAS, 327 , 69 Carraro , G. , Lia , C. , & Chiosi , C. 1998 , MNRAS, 297 , 1021 Chandraseckhar , S. 1941 , ApJ, 93 , 285 Chandraseckhar , S. 1941 , ApJ, 93 , 30 Chandraseckhar , S. 1941

Kinematics and stellar content of the Milky Way populations toward the North Galactic Pole

Aims.The formation and evolution of galaxies is one of the forefront problems of Astrophysics. Detailed studies of our own Galaxy are the first step to understand these complex processes. In this paper we discuss the stellar populations and kinematics toward the North Galactic Pole (NGP) using data taken from the Guide Star Catalog II.Methods.The Padova Galaxy model has been...

The Galaxy Evolution Explorer UV emission in shell galaxies: tracing galaxy ‘rejuvenation’ episodes

We present the Galaxy Evolution Explorer (GALEX) far-ultraviolet (FUV) and near-ultraviolet (NUV) imaging of three nearby shell galaxies, namely NGC 2865, NGC 5018 and NGC 7135 located in low-density environments. The system of shells and fine structures visible in the optical is detected in the NUV image of NGC 2865 and in both NUV and FUV images of NGC 7135. The NUV image of...

Zero-metallicity stars - I. Evolution at constant mass

We present extensive evolutionary models of stars with initial zero-metallicity, covering a large range of initial masses (i.e. ). Calculations are carried out at constant mass, with updated input physics, and applying an overshooting scheme to convective boundaries. The nuclear network includes all the important reactions of the p-p chain, CNO-cycle and α-captures, and is solved...

HST photometry: Can UV colors probe the galaxy ages?

| galaxies; ellipticals | galaxies; evolution | ultraviolet; galaxies - Send o print requests to: C. Chiosi source, i.e either P-AGB or P-AGB plus H-HB and AGBmanque stars (see below for details) and the

Star formation history of early-type galaxies in low density environments - I. Nuclear line–strength indices

This paper is the first of a series (Longhetti et al. 1997a,b) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or signatures of interaction. It presents nuclear line–strength indices for a sample composed of 21 shell galaxies, from the the Malin & Carter (1983) southern survey, and 30 members of isolated interacting pairs...

Star formation history of early-type galaxies in low density environments - II. Kinematics

The present paper is a companion of two others dedicated one to the measurement of the line–strength indices (Longhetti et al. 1997a) and the second to trace back the star formation history of a sample of early–type galaxies by comparing observed indices to the predictions of new spectro–photometric models (Longhetti et al. 1997b). The sample of 51 early-type galaxies in low...

Star formation history of early-type galaxies in low density environments - II. Kinematics

The present paper is a companion of two others dedicated one to the measurement of the line–strength indices (Longhetti et al. 1997a) and the second to trace back the star formation history of a sample of early–type galaxies by comparing observed indices to the predictions of new spectro–photometric models (Longhetti et al. 1997b). The sample of 51 early-type galaxies in low...

Evolutionary sequences of stellar models with new radiative opacities. VI.

We present a large grid of stellar evolutionary models with the initial chemical composition . These tracks are conceived to extend the grid of stellar models described in the previous papers of this series, and are computed with the new radiative opacities by Iglesias et al. (1992) and convective overshoot. The tracks span the range of initial masses from to , and extend from...