scholarly journals Recipes for ULX formation: necessary ingredients and garnishments

2006 ◽  
Vol 2 (S238) ◽  
pp. 235-240
Author(s):  
Roberto Soria
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Molecular Cloud ◽  
Star Clusters ◽  
Metal Abundance ◽  
Super Star Clusters ◽  
Fundamental Physical

AbstractWe summarize the main observational features that seem to recur more frequently in the ULX population. We speculate that low metal abundance, and clustered star formation triggered by molecular cloud collisions are two fundamental physical requirements for ULX formation. In this scenario, most ULXs are formed from recent stellar processes, have black hole (BH) masses <100 M⊙, and do not require merger processes in super-star-clusters.

scholarly journals Magnifying the Early Episodes of Star Formation: Super Star Clusters at Cosmological Distances

2017 ◽  
Vol 842 (1) ◽  
pp. 47 ◽  
Author(s):  
E. Vanzella ◽  
M. Castellano ◽  
M. Meneghetti ◽  
A. Mercurio ◽  
G. B. Caminha ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Clusters ◽  
Super Star Clusters

scholarly journals The star formation histories of two Wolf-Rayet galaxies: NGC 1741 and He2-10. Two butterflies in a collection

1999 ◽  
Vol 193 ◽  
pp. 517-522
Author(s):  
Kelsey E. Johnson
Keyword(s):  
Star Formation ◽  
Spatial Resolution ◽  
High Spatial Resolution ◽  
Dwarf Galaxy ◽  
Broad Band ◽  
Star Clusters ◽  
Environmental Parameters ◽  
Super Star Clusters ◽  
Star Formation Histories ◽  
Compare And Contrast

In an effort to better understand how the properties of star formation in starburst galaxies depend on various environmental parameters, I present a comparison between two well-known WR galaxies: the interacting galaxy system NGC 1741 in the Hickson Compact Group 31, and the dwarf galaxy He2-10. The high spatial resolution of HST has allowed identification of a large number of starburst knots, or ‘super star clusters’ in these WR galaxies. Broad-band photometry and the latest stellar synthesis models are used to estimate the ages and masses of the super star clusters. The properties of the clusters are then used to compare and contrast the overall star-formation histories in the two WR galaxies.

scholarly journals Tidal dwarf galaxies as laboratories of star formation and cosmology

2006 ◽  
Vol 2 (S237) ◽  
pp. 323-330 ◽  
Author(s):  
Pierre-Alain Duc ◽  
Frédéric Bournaud ◽  
Médéric Boquien
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Numerical Simulations ◽  
Dwarf Galaxies ◽  
Star Clusters ◽  
Dense Core ◽  
Multi Wavelength ◽  
Interacting Systems ◽  
Super Star Clusters ◽  
Tidal Tails

AbstractStar formation may take place in a variety of locations in interacting systems: in the dense core of mergers, in the shock regions at the interface of the colliding galaxies and even within the tidal debris expelled into the intergalactic medium. Along tidal tails, objects may be formed with masses ranging from those of super-star clusters to dwarf galaxies: the so-called Tidal Dwarf Galaxies (TDGs). Based on a set of multi-wavelength observations and extensive numerical simulations, we show how TDGs may simultaneously be used as laboratories to study the process of star-formation (SFE, IMF) in a specific environment and as probes of various cosmological properties, such as the distribution of dark matter and satellites around galaxies.

scholarly journals Theory of Young Clusters

2004 ◽  
Vol 221 ◽  
pp. 257-264
Author(s):  
Matthew R. Bate ◽  
Ian A. Bonnell
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Initial Conditions ◽  
Star Clusters ◽  
Brown Dwarfs ◽  
Mass Function ◽  
Large Cluster ◽  
Close Binaries ◽  
Stellar Clusters ◽  
Small Clusters

We review recent results from hydrodynamical calculations of the formation of young stellar clusters. The calculations present a highly dynamical picture of star formation where the mass function of stars originates from competitive accretion between protostars and dynamical ejections which halt accretion. Large star clusters form hierarchically; a molecular cloud forms many small clusters that later merge into one large cluster, erasing the initial substructure. Using calculations that resolve fragmentation down to the opacity limit, we examine the implications of dynamical star formation for the IMF, the formation of brown dwarfs and close binaries, and the sizes of protoplanetary discs. Finally, we discuss the dependence of the results on the initial conditions.

scholarly journals Colliding galaxies and the rapid assembly of clouds into proto-super star clusters

2009 ◽  
Vol 5 (S266) ◽  
pp. 64-68
Author(s):  
Guillermo Tenorio-Tagle ◽  
Enrique Pérez ◽  
Casiana Muñoz-Tuñón ◽  
Sergiy Silich ◽  
Jan Palouš
Keyword(s):  
Star Formation ◽  
Star Clusters ◽  
Radiative Cooling ◽  
Feedback Effects ◽  
Physical Mechanisms ◽  
Short Summary ◽  
Hydrodynamic Calculations ◽  
Super Star Clusters ◽  
Enhanced Surface ◽  
Intercloud Medium

AbstractWe present a short summary of several 2D hydrodynamic calculations that suggest that upon the collision of galaxies two physical mechanisms lead to the formation of proto-super star clusters. These are condensation, induced by radiative cooling, and implosion caused by the shocked intercloud medium. Even in the absence of gravity, these lead to storage and compression of the dense cloud component into massive and compact gravitationally unstable condensations. The resulting entities exhibit enhanced surface densities that are several hundred times higher than their initial values. These are here postulated as the cradles of very efficient and rapid star-formation episodes, able to withstand the negative feedback effects associated with star formation, while leading to the formation of massive and compact super star clusters.

scholarly journals Two‐dimensional Hydrodynamic Models of Super Star Clusters with a Positive Star Formation Feedback

2008 ◽  
Vol 683 (2) ◽  
pp. 683-692 ◽  
Author(s):  
R. Wünsch ◽  
G. Tenorio‐Tagle ◽  
J. Palouš ◽  
S. Silich
Keyword(s):  
Star Formation ◽  
Star Clusters ◽  
Two Dimensional ◽  
Hydrodynamic Models ◽  
Super Star Clusters

scholarly journals Tidally-induced Super Star Clusters in M82

2002 ◽  
Vol 207 ◽  
pp. 477-478
Author(s):  
R. de Grijs ◽  
R.W O'Connell ◽  
J.S. Gallagher
Keyword(s):  
Star Formation ◽  
Cluster Formation ◽  
Age Distribution ◽  
Star Clusters ◽  
Starburst Galaxy ◽  
Super Star Clusters ◽  
Disk Region

Using new HST imaging, we identify a large, evolved system of super star clusters in a disk region just outside the starburst core in the prototypical starburst galaxy M82, “M82 B.” This region has been suspected to be a fossil starburst site in which an intense episode of star formation occurred over 100 Myr ago, which is now confirmed by our derived age distribution. It suggests steady, continuing cluster formation at a modest rate at early times (> 2 Gyr ago), followed by a concentrated formation episode ∼ 600 Myr ago and more recent suppression of cluster formation. The peak episode coincides with independent dynamical estimates for the last tidal encounter with M81.

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