Stellar Populations and Mass Loss in M15: ASpitzer Space TelescopeDetection of Dust in the Intracluster Medium

Based on XMM-Newton observations of M 87 and the Centaurus cluster, abundance profiles of various elements of the intracluster medium (ICM) are derived. The abundances of Si and Fe show strong decreasing gradients. In contrast, the O and Mg abundances are about half of the Si abundance at the center.From the gas mass to stellar mass ratio and the comparison of Mg abundance with the stellar metallicity, the stellar mass loss from the central galaxies is indicated to be the main source of gas in the very central region of the clusters.The observed O, Si and Fe abundance pattern determines the contribution of supernova (SN) Ia and SN II, with the abundance pattern of ejecta of SN Ia. Most of the Si and Fe of the ICM in the central region of the clusters comes from SN Ia which occured in the central galaxies. In order to explain the observed O/Si ratio of a half solar, SN Ia products should have similar abundances of Si and Fe, which may reflect dimmer SN Ia observed in old stellar systems.

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Mass Loss of Different Stellar Populations in Globular Clusters: The Case of M4

The Astrophysical Journal ◽

10.3847/1538-4357/ab05cc ◽

2019 ◽

Vol 873 (2) ◽

pp. 123 ◽

Cited By ~ 7

Author(s):

M. Tailo ◽

A. P. Milone ◽

A. F. Marino ◽

F. D’Antona ◽

E. P. Lagioia ◽

...

Keyword(s):

Mass Loss ◽

Globular Clusters ◽

Stellar Populations

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Mass Loss from Cool Stars: Impact on the Evolution of Stars and Stellar Populations

Annual Review of Astronomy and Astrophysics ◽

10.1146/annurev.astro.38.1.573 ◽

2000 ◽

Vol 38 (1) ◽

pp. 573-611 ◽

Cited By ~ 188

Author(s):

Lee Anne Willson

Keyword(s):

Mass Loss ◽

Stellar Populations ◽

Cool Stars

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Mass-loss law for red giant stars in simple population globular clusters

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab568 ◽

2021 ◽

Vol 503 (1) ◽

pp. 694-703

Author(s):

M Tailo ◽

A P Milone ◽

E P Lagioia ◽

F D’Antona ◽

S Jang ◽

...

Keyword(s):

Mass Loss ◽

Stellar Evolution ◽

Globular Clusters ◽

Hubble Space Telescope ◽

Stellar Populations ◽

Chemical Compositions ◽

Multiple Populations ◽

Mass Losses ◽

Red Giant ◽

Stellar Masses

ABSTRACT The amount of mass lost by stars during the red-giant branch (RGB) phase is one of the main parameters to understand and correctly model the late stages of stellar evolution. Nevertheless, a fully comprehensive knowledge of the RGB mass-loss is still missing. Galactic Globular Clusters (GCs) are ideal targets to derive empirical formulations of mass-loss, but the presence of multiple populations with different chemical compositions has been a major challenge to constrain stellar masses and RGB mass-losses. Recent work has disentangled the distinct stellar populations along the RGB and the horizontal branch (HB) of 46 GCs, thus providing the possibility to estimate the RGB mass-loss of each stellar population. The mass-losses inferred for the stellar populations with pristine chemical composition (called first-generation or 1G stars) tightly correlate with cluster metallicity. This finding allows us to derive an empirical RGB mass-loss law for 1G stars. In this paper, we investigate seven GCs with no evidence of multiple populations and derive the RGB mass-loss by means of high-precision Hubble-Space Telescope photometry and accurate synthetic photometry. We find a cluster-to-cluster variation in the mass-loss ranging from ∼0.1 to ∼0.3 M⊙. The RGB mass-loss of simple-population GCs correlates with the metallicity of the host cluster. The discovery that simple-population GCs and 1G stars of multiple population GCs follow similar mass-loss versus metallicity relations suggests that the resulting mass-loss law is a standard outcome of stellar evolution.

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Star clusters as laboratories for stellar and dynamical evolution

Philosophical Transactions of The Royal Society A Mathematical Physical and Engineering Sciences ◽

10.1098/rsta.2009.0257 ◽

2010 ◽

Vol 368 (1913) ◽

pp. 755-782 ◽

Cited By ~ 14

Author(s):

Jason S. Kalirai ◽

Harvey B. Richer

Keyword(s):

Mass Loss ◽

Stellar Evolution ◽

First Generation ◽

Main Sequence ◽

Star Clusters ◽

Dynamical Evolution ◽

Stellar Populations ◽

Stellar Mass ◽

Theoretical Studies ◽

Chemical Enrichment

Open and globular star clusters have served as benchmarks for the study of stellar evolution owing to their supposed nature as simple stellar populations of the same age and metallicity. After a brief review of some of the pioneering work that established the importance of imaging stars in these systems, we focus on several recent studies that have challenged our fundamental picture of star clusters. These new studies indicate that star clusters can very well harbour multiple stellar populations, possibly formed through self-enrichment processes from the first-generation stars that evolved through post-main-sequence evolutionary phases. Correctly interpreting stellar evolution in such systems is tied to our understanding of both chemical-enrichment mechanisms, including stellar mass loss along the giant branches, and the dynamical state of the cluster. We illustrate recent imaging, spectroscopic and theoretical studies that have begun to shed new light on the evolutionary processes that occur within star clusters.

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Mass loss of different stellar populations in globular clusters

Proceedings of the International Astronomical Union ◽

10.1017/s1743921319006720 ◽

2019 ◽

Vol 14 (S351) ◽

pp. 341-345

Author(s):

Marco Tailo

Keyword(s):

Mass Loss ◽

Globular Clusters ◽

State Of The Art ◽

Stellar Populations ◽

Horizontal Branch ◽

Horizontal Branch Stars ◽

Colour Distribution ◽

Chromosome Maps ◽

First Time

AbstractOnce the age and metallicity are fixed, the colour distribution of horizontal branch stars in a globular cluster depends on few parameters: the helium abundance of the population and the mass lost during the pre-HB stages. These parameters are usually derived from the HB itself, hence they are degenerate. Breaking this degeneracy and understanding their role is a tricky and challenging problem that no study has solved yet. Combining the information obtained from the chromosome maps and the analysis of multi-band photometry with state of the art stellar evolution models, we can obtain a solid estimate of Y for the various stellar populations in a GC. We will then have, for the first time, the possibility to break the parameters’ degeneracy on the HB, understand the role of the mass loss, and lay the foundation to build another piece of the multiple populations mosaic.

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Local environments of SNe Ic and Ic-BL

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316005342 ◽

2015 ◽

Vol 11 (A29B) ◽

pp. 278-279

Author(s):

Jonatan Selsing ◽

Lise Christensen ◽

Christina Thöne ◽

Maryam Modjaz

Keyword(s):

Mass Loss ◽

Stellar Populations ◽

Initial Mass ◽

Stellar Winds ◽

Sample Type ◽

Companion Star ◽

Physical Conditions ◽

Local Environments ◽

Local Explosion ◽

Dependent Mass

AbstractWe have observed the local explosion environments of a sample Type Ic and Type Ic-BL Supernove (SNe) selected from both targeted and non-targeted surveys using VLT/VIMOS in IFU-mode. It is believed that by probing the local surroundings of the parent stellar populations of these types of SNe, valuable information can be gained about the physical conditions, which affect the type of SNe produced. The different kinds of SNe produced are determined by the initial mass and metallicity of the stellar progenitor, as well as by the metallicity-dependent mass loss in the stellar winds at the end phase of their evolution and the interaction with a sufficiently close companion star.

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The Effect of Tidal Stripping on Composite Stellar Populations in Dwarf Spheroidal Galaxies

Advances in Astronomy ◽

10.1155/2010/194345 ◽

2010 ◽

Vol 2010 ◽

pp. 1-14 ◽

Cited By ~ 12

Author(s):

Laura V. Sales ◽

Amina Helmi ◽

Giuseppina Battaglia

Keyword(s):

Dark Matter ◽

Mass Loss ◽

Milky Way ◽

Velocity Dispersion ◽

Local Group ◽

Stellar Populations ◽

Dwarf Spheroidal Galaxies ◽

Stellar Component ◽

Dwarf Spheroidals ◽

Matter Component

We use N-body simulations to study the effects of tides on the kinematical structure of satellite galaxies orbiting a Milky Way-like potential. Here we focus on the evolution of a spherical, dark matter dominated satellite, which is modelled with two stellar components set ab initio to be spatially and kinematically segregated, in a way that resembles the configuration of the metal poor and metal rich stellar populations in several dwarf spheroidals of the Local Group. We find that an important attenuation of the initial differences in the distribution of the two stellar components occurs for orbits with small pericentric radii. This is mainly due to (i) the loss of the gravitational support provided by the dark matter component after tidal stripping takes place and (ii) tides preferentially affect the more extended stellar component, leading to a net decrease in its velocity dispersion as a response for the mass loss, which thus shrinks the kinematical gap. We apply these ideas to the Sculptor and Carina dwarf spheroidals. Differences in their orbits might help to explain why in the former a clear kinematical separation between metal poor and metal rich stars is apparent, while in Carina this segregation is significantly more subtle.

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