scholarly journals Star Formation at High Redshift

1992 ◽  
Vol 45 (4) ◽  
pp. 389
Author(s):  
Colin A Norman
Keyword(s):  
Star Formation ◽  
Absorption Line ◽  
Galaxy Formation ◽  
Massive Star ◽  
High Redshift ◽  
Radio Galaxies ◽  
Starburst Galaxies ◽  
Active Galaxies ◽  
Massive Star Formation

The observations relevant to star formation at high redshift are reviewed including radio galaxies, quasars, IRAS objects, and QSO emission and absorption line regions. Low redshift counterparts associated with starburst galaxies are discussed. The relation of galaxy formation, starbursts, and active galaxies and quasars is briefly reviewed. The role of feedback in galaxy formation and massive star formation is briefly analysed.

Panchromatic Study of Nearby Ultraviolet-bright Starburst Galaxies: Implications for Massive Star Formation and High-Redshift Galaxies

2000 ◽  
Vol 119 (1) ◽  
pp. 79-93 ◽  
Author(s):  
Christopher J. Conselice ◽  
John S. Gallagher ◽  
Daniela Calzetti ◽  
Nicole Homeier ◽  
Anne Kinney
Keyword(s):  
Star Formation ◽  
Massive Star ◽  
High Redshift ◽  
Starburst Galaxies ◽  
Massive Star Formation ◽  
High Redshift Galaxies ◽  
Redshift Galaxies

scholarly journals Environmental effects in galaxies – searching for massive stars

1999 ◽  
Vol 193 ◽  
pp. 739-740
Author(s):  
Duíla F. de Mello ◽  
Marcio A.G. Maia ◽  
Daniel Schaerer ◽  
Claus Leitherer
Keyword(s):  
Star Formation ◽  
Environmental Effects ◽  
Massive Star ◽  
Massive Stars ◽  
Starburst Galaxies ◽  
High Density ◽  
Massive Star Formation ◽  
The Galaxy ◽  
Galaxy Population

In order to study the influence of the environment in galaxies we have selected a sample from the catalog by Maia et al. (1994) which contains objects in low and high density areas of the Southern sky. These samples have been observed with the Brazilian-ESO 1.52m telescope and long-slit spectra are being analyzed. With our database we will be able to investigate the role of the environment in the galaxy population. We will be able to search for WR features and massive stars. It is our goal to compare the general properties of these galaxies with typical starburst galaxies which are dominated by episodes of massive star formation.

scholarly journals Massive Star Formation in Metal-Enriched Haloes at High Redshift

2020 ◽  
Vol 3 (1) ◽  
Author(s):  
John A. Regan ◽  
Zoltán Haiman ◽  
John H. Wise ◽  
Brian W. O'Shea ◽  
Michael L. Norman
Keyword(s):  
Star Formation ◽  
Massive Star ◽  
High Redshift ◽  
Massive Star Formation

scholarly journals Line-driven ablation of circumstellar discs – IV. The role of disc ablation in massive star formation and its contribution to the stellar upper mass limit

2018 ◽  
Vol 483 (4) ◽  
pp. 4893-4900 ◽  
Author(s):  
Nathaniel Dylan Kee ◽  
Rolf Kuiper
Keyword(s):  
Star Formation ◽  
Massive Star ◽  
Loss Rate ◽  
Massive Stars ◽  
Mass Loss Rate ◽  
Ablation Rate ◽  
Massive Star Formation ◽  
Future Studies ◽  
Accretion Rates

Abstract Radiative feedback from luminous, massive stars during their formation is a key process in moderating accretion on to the stellar object. In the prior papers in this series, we showed that one form such feedback takes is UV line-driven disc ablation. Extending on this study, we now constrain the strength of this effect in the parameter range of star and disc properties appropriate to forming massive stars. Simulations show that ablation rate depends strongly on stellar parameters, but that this dependence can be parameterized as a nearly constant, fixed enhancement over the wind mass-loss rate, allowing us to predict the rate of disc ablation for massive (proto)stars as a function of stellar mass and metallicity. By comparing this to predicted accretion rates, we conclude that ablation is a strong feedback effect for very massive (proto)stars which should be considered in future studies of massive star formation.

scholarly journals Implications of Early Cooling Flows and Galactic Winds for the Evolution of Deuterium

2000 ◽  
Vol 198 ◽  
pp. 535-539
Author(s):  
Amancio C. S. Friaça
Keyword(s):  
Absorption Line ◽  
Galaxy Formation ◽  
Spatial Scales ◽  
High Redshift ◽  
Cooling Flows ◽  
Galactic Winds ◽  
Important Constraint

The deuterium abundances in high-redshift QSO absorption-line systems could be an important constraint in models of galaxy formation. Here we investigate the role of galactic winds and massive cooling flows present during the formation of galaxies on the evolution of deuterium abundance. Destruction factors are calculated and the time and spatial scales for the dispersal through galactic winds of the processed deuterium-depleted gas are presented and related to the D/H determinations for QSO absorption-line systems. The calculations are derived from a chemodynamical model within a scenario in which the absorbers are located inside the hot halo of a young galaxy.

scholarly journals The VLT-FLAMES Tarantula Survey

2018 ◽  
Vol 618 ◽  
pp. A73 ◽  
Author(s):  
F. R. N. Schneider ◽  
O. H. Ramírez-Agudelo ◽  
F. Tramper ◽  
J. M. Bestenlehner ◽  
N. Castro ◽  
...  
Keyword(s):  
Star Formation ◽  
Massive Star ◽  
Massive Stars ◽  
High Redshift ◽  
Large Magellanic Cloud ◽  
Giant Molecular Clouds ◽  
Stellar Content ◽  
Massive Star Formation ◽  
Hii Region ◽  
Mass Distributions

The 30 Doradus (30 Dor) nebula in the Large Magellanic Cloud (LMC) is the brightest HII region in the Local Group and a prototype starburst similar to those found in high redshift galaxies. It is thus a stepping stone to understand the complex formation processes of stars in starburst regions across the Universe. Here, we have studied the formation history of massive stars in 30 Dor using masses and ages derived for 452 mainly OB stars from the spectroscopic VLT-FLAMES Tarantula Survey (VFTS). We find that stars of all ages and masses are scattered throughout 30 Dor. This is remarkable because it implies that massive stars either moved large distances or formed independently over the whole field of view in relative isolation. We find that both channels contribute to the 30 Dor massive star population. Massive star formation rapidly accelerated about 8 Myr ago, first forming stars in the field before giving birth to the stellar populations in NGC 2060 and NGC 2070. The R136 star cluster in NGC 2070 formed last and, since then, about 1 Myr ago, star formation seems to be diminished with some continuing in the surroundings of R136. Massive stars within a projected distance of 8 pc of R136 are not coeval but show an age range of up to 6 Myr. Our mass distributions are well populated up to 200 M⊙. The inferred IMF is shallower than a Salpeter-like IMF and appears to be the same across 30 Dor. By comparing our sample of stars to stellar models in the Hertzsprung–Russell diagram, we find evidence for missing physics in the models above log L/L⊙ = 6 that is likely connected to enhanced wind mass loss for stars approaching the Eddington limit. Our work highlights the key information about the formation, evolution and final fates of massive stars encapsulated in the stellar content of 30 Dor, and sets a new benchmark for theories of massive star formation in giant molecular clouds.

scholarly journals The role of low-mass star clusters in massive star formation. The Orion case

2013 ◽  
Vol 554 ◽  
pp. A48 ◽  
Author(s):  
V. M. Rivilla ◽  
J. Martín-Pintado ◽  
I. Jiménez-Serra ◽  
A. Rodríguez-Franco
Keyword(s):  
Star Formation ◽  
Massive Star ◽  
Star Clusters ◽  
Mass Star ◽  
Massive Star Formation ◽  
Low Mass

scholarly journals Jet-Induced Star Formation

2004 ◽  
Vol 217 ◽  
pp. 472-479 ◽  
Author(s):  
Wil van Breugel ◽  
Chris Fragile ◽  
Peter Anninos ◽  
Stephen Murray
Keyword(s):  
Star Formation ◽  
Galaxy Formation ◽  
Positive Feedback ◽  
Formation Process ◽  
Radio Galaxy ◽  
Radio Galaxies ◽  
Observational Evidence ◽  
Active Galaxies ◽  
Induce Star Formation ◽  
The Galaxy

Jets from radio galaxies can have dramatic effects on the medium through which they propagate. We review observational evidence for jet-induced star formation in low (‘FR-I’) and high (‘FR-II’) luminosity radio galaxies, at low and high redshifts respectively. We then discuss numerical simulations which are aimed to explain a jet-induced starburst (‘Minkowski's Object’) in the nearby FR-I type radio galaxy NGC 541. We conclude that jets can induce star formation in moderately dense (10 cm−3), warm (104 K) gas; that this may be more common in the dense environments of forming, active galaxies; and that this may provide a mechanism for ‘positive’ feedback from AGN in the galaxy formation process.

scholarly journals Massive Star Formation and Evolution in Starburst Galaxies: Mid‐infrared Spectroscopy with theISOShort Wavelength Spectrometer

2000 ◽  
Vol 539 (2) ◽  
pp. 641-657 ◽  
Author(s):  
Michele D. Thornley ◽  
Natascha M. Forster Schreiber ◽  
Dieter Lutz ◽  
Reinhard Genzel ◽  
Henrik W. W. Spoon ◽  
...  
Keyword(s):  
Infrared Spectroscopy ◽  
Star Formation ◽  
Massive Star ◽  
Starburst Galaxies ◽  
Massive Star Formation ◽  
Mid Infrared ◽  
Mid Infrared Spectroscopy ◽  
Formation And Evolution

scholarly journals The Role of Massive Stars in Galactic Chemical Evolution

2007 ◽  
Vol 3 (S250) ◽  
pp. 391-400 ◽  
Author(s):  
Francesca Matteucci
Keyword(s):  
Star Formation ◽  
Galaxy Formation ◽  
Massive Stars ◽  
High Redshift ◽  
Morphological Type ◽  
Mass Relation ◽  
Delay Model ◽  
Galactic Winds ◽  
Dwarf Spheroidals

AbstractI will review the role of massive stars in galactic evolution both from the nucleosynthesis and energetics point of view. In particular, I will highlight some important observational facts explained by means of massive stars in galaxies of different morphological type: the Milky Way, ellipticals and dwarf spheroidals. I will describe first the time-delay model and its interpretation in terms of abundance ratios in galaxies, then I will discuss the importance of mass loss in massive stars to reproduce the data in the Galactic bulge and disk. I will discuss also how massive stars can be important producers of primary nitrogen if rotation in stellar models is taken into account. Concerning elliptical galaxies, I will show that to reproduce the observed [Mg/Fe] versus Mass relation in these galaxies it is necessary to assume a more important role of massive stars in more massive galaxies and that this can be achieved by means of downsizing in star formation. I will discuss how massive stars are responsible in triggering galactic winds both in ellipticals and dwarf spheroidals. These latter systems show a low overabundance of α-elements relative to Fe with respect to Galactic stars of the same [Fe/H]: this is interpreted as due to a slow star formation coupled with very efficient galactic winds. Finally, I will show a comparison between the predicted Type Ib/c rates in galaxies and the observed GRB rate and how we can impose constraints on the mechanism of galaxy formation by studying the GRB rate at high redshift.

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