scholarly journals Gone with the wind: Where is the missing stellar wind energy from massive star clusters?

2014 ◽  
Vol 442 (3) ◽  
pp. 2701-2716 ◽  
Author(s):  
Anna L. Rosen ◽  
Laura A. Lopez ◽  
Mark R. Krumholz ◽  
Enrico Ramirez-Ruiz
Keyword(s):  
Wind Energy ◽  
Stellar Wind ◽  
Massive Star ◽  
Star Clusters ◽  
Gone With The Wind

scholarly journals Stellar wind retention and expulsion in massive star clusters

2018 ◽  
Vol 478 (2) ◽  
pp. 2794-2811 ◽  
Author(s):  
J P Naiman ◽  
E Ramirez-Ruiz ◽  
D N C Lin
Keyword(s):  
Stellar Wind ◽  
Massive Star ◽  
Star Clusters

scholarly journals From young massive star clusters to old globulars: long-term survival chances

2006 ◽  
Vol 2 (S237) ◽  
pp. 408-408
Author(s):  
Richard de Grijs
Keyword(s):  
Galaxy Formation ◽  
Massive Star ◽  
Cluster Formation ◽  
Star Clusters ◽  
Term Survival ◽  
Star Forming ◽  
Distant Galaxies ◽  
Wide Range ◽  
Galaxy Collisions

Young, massive star clusters (YMCs) are the most notable and significant end products of violent star-forming episodes triggered by galaxy collisions and close encounters. The question remains, however, whether or not at least a fraction of the compact YMCs seen in abundance in extragalactic starbursts, are potentially the progenitors of (≳10 Gyr) old globular cluster (GC)-type objects. If we could settle this issue convincingly, one way or the other, the implications of such a result would have far-reaching implications for a wide range of astrophysical questions, including our understanding of the process of galaxy formation and assembly, and the process and conditions required for star (cluster) formation. Because of the lack of a statistically significant sample of YMCs in the Local Group, however, we need to resort to either statistical arguments or to the painstaking approach of case-by-case studies of individual objects in more distant galaxies.

scholarly journals Red Supergiants as Cosmic Abundance Probes: Massive Star Clusters in M83 and the Mass–Metallicity Relation of Nearby Galaxies

2017 ◽  
Vol 847 (2) ◽  
pp. 112 ◽  
Author(s):  
Ben Davies ◽  
Rolf-Peter Kudritzki ◽  
Carmela Lardo ◽  
Maria Bergemann ◽  
Emma Beasor ◽  
...  
Keyword(s):  
Massive Star ◽  
Star Clusters ◽  
Cosmic Abundance ◽  
Red Supergiants ◽  
Nearby Galaxies

scholarly journals Using young massive star clusters to understand star formation and feedback in high-redshift-like environments

2015 ◽  
Vol 75-76 ◽  
pp. 43-48
Author(s):  
S. Longmore ◽  
A. Barnes ◽  
C. Battersby ◽  
J. Bally ◽  
J.M. Diederik Kruijssen ◽  
...  
Keyword(s):  
Star Formation ◽  
Massive Star ◽  
High Redshift ◽  
Star Clusters

scholarly journals THE EVOLUTIONARY TRACKS OF YOUNG MASSIVE STAR CLUSTERS

2014 ◽  
Vol 794 (2) ◽  
pp. 147 ◽  
Author(s):  
S. Pfalzner ◽  
G. Parmentier ◽  
M. Steinhausen ◽  
K. Vincke ◽  
K. Menten
Keyword(s):  
Massive Star ◽  
Star Clusters

scholarly journals THE PREVALENCE AND IMPACT OF WOLF–RAYET STARS IN EMERGING MASSIVE STAR CLUSTERS

2016 ◽  
Vol 826 (2) ◽  
pp. 194 ◽  
Author(s):  
Kimberly R. Sokal ◽  
Kelsey E. Johnson ◽  
Rémy Indebetouw ◽  
Philip Massey
Keyword(s):  
Massive Star ◽  
Star Clusters

scholarly journals AGB winds in interacting binary stars

2020 ◽  
Vol 493 (2) ◽  
pp. 2606-2617 ◽  
Author(s):  
Luis C Bermúdez-Bustamante ◽  
G García-Segura ◽  
W Steffen ◽  
L Sabin
Keyword(s):  
Radiation Pressure ◽  
Stellar Wind ◽  
Binary Stars ◽  
Massive Star ◽  
Density Ratio ◽  
Asymptotic Giant Branch ◽  
Surface Layers ◽  
Outflow Velocity ◽  
Analytical Formulae ◽  
Set Up

ABSTRACT We perform numerical simulations to investigate the stellar wind from interacting binary stars. Our aim is to find analytical formulae describing the outflow structure. In each binary system the more massive star is in the asymptotic giant branch (AGB) and its wind is driven by a combination of pulsations in the stellar surface layers and radiation pressure on dust, while the less massive star is in the main sequence. Time averages of density and outflow velocity of the stellar wind are calculated and plotted as profiles against distance from the centre of mass and colatitude angle. We find that mass is lost mainly through the outer Lagrangian point L2. The resultant outflow develops into a spiral at low distances from the binary. The outflowing spiral is quickly smoothed out by shocks and becomes an excretion disc at larger distances. This leads to the formation of an outflow structure with an equatorial density excess, which is greater in binaries with smaller orbital separation. The pole-to-equator density ratio reaches a maximum value of ∼105 at Roche lobe overflow state. We also find that the gas stream leaving L2 does not form a circumbinary ring for stellar mass ratios above 0.78, when radiation pressure on dust is taken into account. Analytical formulae are obtained by curve fitting the two-dimensional, azimuthally averaged density and outflow velocity profiles. The formulae can be used in future studies to set-up the initial outflow structure in hydrodynamic simulations of common-envelope evolution and formation of planetary nebulae.

scholarly journals The search for multiple populations in Magellanic Clouds clusters – V. Correlation between cluster age and abundance spreads

2019 ◽  
Vol 487 (4) ◽  
pp. 5324-5334 ◽  
Author(s):  
S Martocchia ◽  
E Dalessandro ◽  
C Lardo ◽  
I Cabrera-Ziri ◽  
N Bastian ◽  
...  
Keyword(s):  
Significant Role ◽  
Massive Star ◽  
Milky Way ◽  
Star Clusters ◽  
Magellanic Clouds ◽  
Key Factors ◽  
Strong Function ◽  
Combining Data ◽  
Chemical Anomalies ◽  
Cluster Age

ABSTRACT In our HST photometric survey, we have been searching for multiple stellar populations (MPs) in Magellanic Clouds (MCs) massive star clusters which span a significant range of ages (∼1.5–11 Gyr). In the previous papers of the series, we have shown that the age of the cluster represents one of the key factors in shaping the origin of the chemical anomalies. Here, we present the analysis of four additional clusters in the MCs, namely Lindsay 38, Lindsay 113, NGC 2121, and NGC 2155, for which we recently obtained new UV HST observations. These clusters are more massive than ∼104 M⊙ and have ages between ∼2.5 and ∼6 Gyr, i.e. located in a previously unexplored region of the cluster age/mass diagram. We found chemical anomalies, in the form of N spreads, in three out of four clusters in the sample, namely in NGC 2121, NGC 2155, and Lindsay 113. By combining data from our survey and HST photometry for three additional clusters in the Milky Way (namely 47 Tuc, M15, and NGC 2419), we show that the extent of the MPs in the form of N spread is a strong function of age, with older clusters having larger N spreads with respect to the younger ones. Hence, we confirm that cluster age plays a significant role in the onset of MPs.

The Stellar Population of Embedded Galactic Massive Star Clusters

2003 ◽  
pp. 121-126
Author(s):  
A. Damineli ◽  
R. D. Blum ◽  
P. S. Conti ◽  
E. Figuerêdo ◽  
C. L. Barbosa
Keyword(s):  
Massive Star ◽  
Stellar Population ◽  
Star Clusters
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