Stellar Feedback Through Cosmic Time: Starbursts & Superwinds

AbstractThroughout cosmic time, the feedback of massive star winds and supernova explosions has been instrumental in determining the phase structure of the interstellar medium, controlling important aspects of both the formation and evolution of galaxies, producing galactic winds and enriching the intergalactic medium with heavy elements. In this paper, I review progress made in our theoretical understanding of how these feedback processes have operated throughout cosmic time from the epoch of the first stars through to the present day.

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A Review of the Theory of Galactic Winds Driven by Stellar Feedback

Galaxies ◽

10.3390/galaxies6040114 ◽

2018 ◽

Vol 6 (4) ◽

pp. 114 ◽

Cited By ~ 19

Author(s):

Dong Zhang

Keyword(s):

Galaxy Formation ◽

Mass Function ◽

Future Research ◽

Star Forming ◽

Stellar Feedback ◽

Galactic Winds ◽

Galaxy Formation And Evolution ◽

Supernova Explosions ◽

Formation And Evolution ◽

Magnetohydrodynamic Simulations

Galactic winds from star-forming galaxies are crucial to the process of galaxy formation and evolution, regulating star formation, shaping the stellar mass function and the mass-metallicity relation, and enriching the intergalactic medium with metals. Galactic winds associated with stellar feedback may be driven by overlapping supernova explosions, radiation pressure of starlight on dust grains, and cosmic rays. Galactic winds are multiphase, the growing observations of emission and absorption of cold molecular, cool atomic, ionized warm and hot outflowing gas in a large number of galaxies have not been completely understood. In this review article, I summarize the possible mechanisms associated with stars to launch galactic winds, and review the multidimensional hydrodynamic, radiation hydrodynamic and magnetohydrodynamic simulations of winds based on various algorithms. I also briefly discuss the theoretical challenges and possible future research directions.

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The influence of feedback from massive stars on the formation and emergence of massive clusters

Proceedings of the International Astronomical Union ◽

10.1017/s1743921315009734 ◽

2015 ◽

Vol 12 (S316) ◽

pp. 177-183

Author(s):

James E. Dale

Keyword(s):

Large Scale ◽

Massive Star ◽

Massive Stars ◽

Cluster Structure ◽

Star Clusters ◽

Stellar Feedback ◽

Making Sense ◽

Formation Efficiency ◽

Massive Clusters ◽

Made In

AbstractMassive star clusters are of fundamental importance both observationally, since they are visible at such great distances, and theoretically, because of their influence on the large–scale ISM. Understanding stellar feedback is a prerequisite for making sense of their formation and early evolution, since feedback influences cluster structure, star formation efficiency, and sets the timescales on which clusters emerge from their parent clouds to become optically visible. I review the progress made in understanding these issues from a numerical perspective.

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From Gas to Stars Over Cosmic Time

Science ◽

10.1126/science.1229229 ◽

2013 ◽

Vol 340 (6140) ◽

pp. 1229229 ◽

Cited By ~ 5

Author(s):

Mordecai-Mark Mac Low

Keyword(s):

Star Formation ◽

Star Formation Rate ◽

Formation Rate ◽

Cosmic Time ◽

First Stars ◽

Initial Rise ◽

Stellar Radiation ◽

History Of ◽

Supernova Explosions ◽

The Universe

From the time the first stars formed over 13 billion years ago to the present, star formation has had an unexpectedly dynamic history. At first, the star-formation rate density increased dramatically, reaching a peak 10 billion years ago of more than 10 times the present-day value. Observations of the initial rise in star formation remain difficult, poorly constraining it. Theoretical modeling has trouble predicting this history because of the difficulty in following the feedback of energy from stellar radiation and supernova explosions into the gas from which further stars form. Observations from the ground and space with the next generation of instruments should reveal the full history of star formation in the universe, and simulations appear poised to accurately predict the observed history.

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Stars from Craddle to Grave: Powerful Factories of Chemical Elements

Vestnik RFFI ◽

10.22204/2410-4639-2019-101-01-70-86 ◽

2019 ◽

pp. 70-86

Author(s):

Alexander A. Lutovinov

Keyword(s):

Neutron Stars ◽

Periodic Table ◽

Chemical Elements ◽

Superheavy Elements ◽

Heavy Elements ◽

Death Process ◽

Production Rates ◽

First Stars ◽

Supernova Explosions ◽

The Universe

The first elements of the Periodic Table – hydrogen, helium and partly lithium - appeared in the first seconds after the birth of the Universe. The first stars “gathered” from these materials are the natural factories of the synthesis of heavier elements, not only throughout their lives, but even during their death process, during Supernova explosions. Supernova explosions, in their turn, are powerful factories for the production of heavy elements. Modern instruments allow scientists not only to register such events, but also to determine how many different chemical elements were formed during such events. The recent discovery of the merging neutron stars and subsequent studies of their afterglow allowed us to clarify the process of formation of superheavy elements in the Universe up to the gold and uranium. Thus, astrophysical observations give scientists the most important information about the “production rates” of elements in the nature, and their abundance in the Universe.

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The First Galaxies in the Universe

10.23943/princeton/9780691144917.001.0001 ◽

2013 ◽

Author(s):

Abraham Loeb ◽

Steven R. Furlanetto

Keyword(s):

Galaxy Evolution ◽

Big Bang ◽

First Stars ◽

Distant Galaxies ◽

Formation And Evolution ◽

Early Galaxies ◽

First Galaxies ◽

Large Telescopes ◽

New Generation ◽

The Big Bang

This book provides a comprehensive, self-contained introduction to one of the most exciting frontiers in astrophysics today: the quest to understand how the oldest and most distant galaxies in our universe first formed. Until now, most research on this question has been theoretical, but the next few years will bring about a new generation of large telescopes that promise to supply a flood of data about the infant universe during its first billion years after the big bang. This book bridges the gap between theory and observation. It is an invaluable reference for students and researchers on early galaxies. The book starts from basic physical principles before moving on to more advanced material. Topics include the gravitational growth of structure, the intergalactic medium, the formation and evolution of the first stars and black holes, feedback and galaxy evolution, reionization, 21-cm cosmology, and more.

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Most of the cool CGM of star-forming galaxies is not produced by supernova feedback

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3759 ◽

2020 ◽

Author(s):

Andrea Afruni ◽

Filippo Fraternali ◽

Gabriele Pezzulli

Keyword(s):

Galaxy Evolution ◽

Cosmic Time ◽

Energy Coupling ◽

High Energy ◽

Parametric Models ◽

Star Forming ◽

Galaxy Halos ◽

The Galaxy ◽

Supernova Explosions ◽

Cool Gas

Abstract The characterization of the large amount of gas residing in the galaxy halos, the so called circumgalactic medium (CGM), is crucial to understand galaxy evolution across cosmic time. We focus here on the the cool (T ∼ 104 K) phase of this medium around star-forming galaxies in the local universe, whose properties and dynamics are poorly understood. We developed semi-analytical parametric models to describe the cool CGM as an outflow of gas clouds from the central galaxy, as a result of supernova explosions in the disc (galactic wind). The cloud motion is driven by the galaxy gravitational pull and by the interactions with the hot (T ∼ 106 K) coronal gas. Through a bayesian analysis, we compare the predictions of our models with the data of the COS-Halos and COS-GASS surveys, which provide accurate kinematic information of the cool CGM around more than 40 low-redshift star-forming galaxies, probing distances up to the galaxy virial radii. Our findings clearly show that a supernova-driven outflow model is not suitable to describe the dynamics of the cool circumgalactic gas. Indeed, to reproduce the data, we need extreme scenarios, with initial outflow velocities and mass loading factors that would lead to unphysically high energy coupling from the supernovae to the gas and with supernova efficiencies largely exceeding unity. This strongly suggests that, since the outflows cannot reproduce most of the cool gas absorbers, the latter are likely the result of cosmological inflow in the outer galaxy halos, in analogy to what we have previously found for early-type galaxies.

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On the origin of the helium-rich population in the peculiar globular cluster Omega Centauri

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310004114 ◽

2009 ◽

Vol 5 (S268) ◽

pp. 187-188

Author(s):

Donatella Romano ◽

M. Tosi ◽

M. Cignoni ◽

F. Matteucci ◽

E. Pancino ◽

...

Keyword(s):

Chemical Composition ◽

Globular Cluster ◽

Main Sequence ◽

Milky Way ◽

Dwarf Galaxy ◽

Potential Well ◽

Galactic Winds ◽

Supernova Explosions

AbstractIn this contribution we discuss the origin of the extreme helium-rich stars which inhabit the blue main sequence (bMS) of the Galactic globular cluster Omega Centauri. In a scenario where the cluster is the surviving remnant of a dwarf galaxy ingested by the Milky Way many Gyr ago, the peculiar chemical composition of the bMS stars can be naturally explained by considering the effects of strong differential galactic winds, which develop owing to multiple supernova explosions in a shallow potential well.

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Core Collapse Supernova Models and Nucleosynthesis

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313009198 ◽

2013 ◽

Vol 9 (S296) ◽

pp. 27-36

Author(s):

Ken'ichi Nomoto

Keyword(s):

Big Bang ◽

Elemental Abundance ◽

Core Collapse ◽

Solar Abundance ◽

First Stars ◽

Abundance Pattern ◽

Core Collapse Supernova ◽

Abundance Patterns ◽

Supernova Explosions ◽

The Big Bang

AbstractAfter the Big Bang, production of heavy elements in the early Universe takes place in the first stars and their supernova explosions. The nature of the first supernovae, however, has not been well understood. The signature of nucleosynthesis yields of the first supernovae can be seen in the elemental abundance patterns observed in extremely metal-poor stars. Interestingly, those abundance patterns show some peculiarities relative to the solar abundance pattern, which should provide important clues to understanding the nature of early generations of supernovae. We review the recent results of the nucleosynthesis yields of massive stars. We examine how those yields are affected by some hydrodynamical effects during the supernova explosions, namely, explosion energies from those of hypernovae to faint supernovae, mixing and fallback of processed materials, asphericity, etc. Those parameters in the supernova nucleosynthesis models are constrained from observational data of supernovae and metal-poor stars.

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Molecular Transport Junctions: An Introduction

MRS Bulletin ◽

10.1557/mrs2004.119 ◽

2004 ◽

Vol 29 (6) ◽

pp. 376-384 ◽

Cited By ~ 29

Author(s):

Cherie R. Kagan ◽

Mark A. Ratner

Keyword(s):

Thin Film ◽

Charge Transport ◽

Single Molecule ◽

Molecular Transport ◽

Molecular Junction ◽

Theoretical Understanding ◽

Future Directions ◽

Molecular Scale ◽

Molecular Charge ◽

Made In

AbstractThis issue of MRS Bulletin on molecular transport junctions highlights the current experimental and theoretical understanding of molecular charge transport and its extension to the rapidly growing areas of molecular and carbon nanotube electronics. This introduction will outline the progress that has been made in understanding the mechanisms of molecular junction transport and the challenges and future directions in exploring charge transport on the molecular scale. In spite of the substantial challenges, molecular charge transport is of great interest for its intrinsic importance to potential single-molecule electronic, thin-film electronic, and optoelectronic applications.

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