Browse Dept. of Astronomy by Title

• (2002)
Proto-planetary nebulae (PPNs) are evolved, intermediate initial mass (0.8--8 solar masses) stars that are in rapid transition from the asymptotic giant branch (AGB) phase into the planetary nebula (PN) phase. Largely ...

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• (2012-02-01)
This thesis presents observations and modeling of nearby embedded sources in the earliest stage of protostellar evolution, i.e., Class 0 young stellar objects, using interferometric data of the Berkeley-Illinois-Maryland ...

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• (2010-01-06)
Physical properties of the three main structures in young stellar objects (YSOs), envelopes, bipolar outflows, and circumstellar disks, have been studied using radio interferometers: the Berkeley-Illinois-Maryland ...

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• (Department of Astronomy. College of Liberal Arts and Sciences. University of Illinois at Urbana-Champaign, 1999-10)
The astronomical study of molecules has been an essential research field since the development of radio astronomy. Presently nearly 120 molecules have been identified in interstellar and circumstellar environments. The ...

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• (2000)
In Chapter 5, we show that HCOOH appears to exist ubiquitously in dense molecular cores in either solid or gas phase. The detected HCOOH sources are good candidate targets for future acetic acid and glycine searches. ...

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• (1996)
Glycine $\rm(NH\sb2CH\sb2COOH)$ is the smallest amino acid. Detecting interstellar glycine could shed light on the presolar nebular chemistry and its possible role in seeding newly formed planets with the building blocks ...

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• (2011-08-26)
A new class of wide-field, repeated-scan optical sky surveys, such as LSST, is coming online, and will map the sky in the time domain with unprecedented depth, completeness, and dynamic range. A main science goal of LSST ...

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• (1996)
Several three dimensional, multi-species, cosmological hydrodynamic simulations of the formation and evolution of Ly$\alpha$ forest absorbers were performed in three CDM-like cosmological models: the standard CDM model ...

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• (2012-06-27)
Two types of dust disks have been discovered around white dwarfs (WDs): small dust disks within the Roche limits of their WDs, and a large dust disk around the hot central WD of the Helix planetary nebula (PN), possibly ...

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• (1973)

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• (1991)
Observations of pulsar timing suggest that glitches and post-glitch behavior are due to variable coupling between the superfluid and normal components in neutron stars. A rotating superfluid is threaded by quantized vortex ...

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• (1968)

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• (1993)
In this thesis, I have studied the dynamics of the inflationary universe and the possible cosmological consequences of a series of phase transitions which the universe may have undergone. Specially, I have studied the ...

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• (2011-01-21)
In an era of precision cosmology, clusters of galaxies are the natural consequences under the hierarchical scenario, within which clusters directly encapsulate the history of structure formation. Thus, determining the mass ...

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• (1969)

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• (2002)
As part of an effort to understand how the solar wind is energized, the so-determined electron density is used to interpret O VI lambda1032, 1037 A spectra taken with UVCS. The spectra are interpreted in terms of empirical ...

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• (2014-01-16)
Throughout the entire lifetime of a star, it continuously alters the environment. Diverse processes are involved which complicates studies of stellar interaction. This thesis focuses on two different physical phenomena ...

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• (2000)
The subject of this thesis is the equilibria, stability and nonlinear dynamics of magnetically-sheared atmospheres as they relate to magnetic flux emergence and the structure and disruption of magnetic arcades of the sun. ...

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• (Department of Astronomy. College of Liberal Arts and Sciences. University of Illinois at Urbana-Champaign., 2000-04)
The subject of this thesis is the equilibria, stability and nonlinear dynamics of magnetically-sheared atmospheres as they relate to magnetic flux emergence and the structure and disruption of magnetic arcades of the sun. ...

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• (1981)
We have studied the evolution of 15, 30, and 40 M(,(CIRCLE)) stars with compositions Y = 0.28 and Z = 0.02, 0.01, 0.001 and 0.0002, and of 50 M(,(CIRCLE)) stars with Y = 0.28, Z = 0.0002. These models have been evolved ...

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