Ultraviolet Spectra of Star‐forming Galaxies with Time‐dependent Dust Obscuration

We present a new approach to probe the properties of the most massive, ionizing stars with respect to the less massive, non-ionizing stars. The new technique utilizes stellar-wind lines, instead of the previously employed nebular lines. This allows us to probe the timescale of the dust dispersal in a very young obscured starburst from purely stellar diagnostics.

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An atlas of ultraviolet spectra of star-forming galaxies

The Astrophysical Journal Supplement Series ◽

10.1086/191771 ◽

1993 ◽

Vol 86 ◽

pp. 5 ◽

Cited By ~ 192

Author(s):

A. L. Kinney ◽

R. C. Bohlin ◽

D. Calzetti ◽

N. Panagia ◽

Rosemary F. G. Wyse

Keyword(s):

Star Forming ◽

Ultraviolet Spectra

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Two Types of Jet in Cepheus A

International Astronomical Union Colloquium ◽

10.1017/s0252921100045851 ◽

1998 ◽

Vol 164 ◽

pp. 345-346

Author(s):

V. A. Hughes

Keyword(s):

Young Star ◽

Time Dependent ◽

Star Forming ◽

Cepheus A

AbstractThe young star forming region, Cepheus A, has been monitored since 1981, and shows four new types of time-dependent events. Two of these are briefly described.

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Optical to ultraviolet spectra of sandwiches of benzene and transition metal atoms: Time dependent density functional theory and many-body calculations

The Journal of Chemical Physics ◽

10.1063/1.3300129 ◽

2010 ◽

Vol 132 (4) ◽

pp. 044314 ◽

Cited By ~ 33

Author(s):

J. I. Martínez ◽

J. M. García-Lastra ◽

M. J. López ◽

J. A. Alonso

Keyword(s):

Density Functional Theory ◽

Transition Metal ◽

Density Functional ◽

Time Dependent ◽

Many Body ◽

Functional Theory ◽

Ultraviolet Spectra ◽

Metal Atoms ◽

Transition Metal Atoms ◽

Dependent Density

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A 2D hydrodynamic simulation coupled to chemical evolution around star forming region: A time dependent study

10.1063/1.4812619 ◽

2013 ◽

Author(s):

Liton Majumdar ◽

Ankan Das ◽

Sandip K. Chakrabarti ◽

Sonali Chakrabarti

Keyword(s):

Chemical Evolution ◽

Time Dependent ◽

Hydrodynamic Simulation ◽

Star Forming

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Chemical Tracers of Pre-Brown Dwarf Cores Formed Through Turbulent Fragmentation

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316007961 ◽

2015 ◽

Vol 11 (S315) ◽

Author(s):

Jonathan Holdship ◽

Serena Viti

Keyword(s):

Molecular Cloud ◽

Brown Dwarfs ◽

Step Change ◽

Time Dependent ◽

Formation Mechanisms ◽

Brown Dwarf ◽

Star Forming ◽

Chemical Tracers ◽

Fractional Abundance ◽

Chemical Code

AbstractA gas-grain time dependent chemical code, UCL_CHEM, has been used to investigate the possibility of using chemical tracers to differentiate between the possible formation mechanisms of brown dwarfs. We model the formation of a pre-brown dwarf core through turbulent fragmentation by following the depth-dependent chemistry in a molecular cloud through the step change in density associated with an isothermal shock and the subsequent freefall collapse once a bound core is produced. Trends in the fractional abundance of molecules commonly observed in star forming cores are then explored to find a diagnostic for identifying brown dwarf mass cores formed through turbulence. We find that the cores produced by our models would be bright in CO and NH3 but not in HCO+. This differentiates them from models using purely freefall collapse as such models produce cores that would have detectable transitions from all three molecules.

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