Publication

Molecular gas and dust influenced by massive protostars: spectral surveys in the far-infrared and submillimeter

van der Wiel, M. H. D., May-2011, [Groningen]: Rijksuniversiteit Groningen. 167 p.

Research output: ThesisThesis fully internal (DIV)Academic

APA

van der Wiel, M. H. D. (2011). Molecular gas and dust influenced by massive protostars: spectral surveys in the far-infrared and submillimeter. [Groningen]: Rijksuniversiteit Groningen.

Author

van der Wiel, Matthijs H. D.. / Molecular gas and dust influenced by massive protostars : spectral surveys in the far-infrared and submillimeter. [Groningen] : Rijksuniversiteit Groningen, 2011. 167 p.

Harvard

van der Wiel, MHD 2011, 'Molecular gas and dust influenced by massive protostars: spectral surveys in the far-infrared and submillimeter', Doctor of Philosophy, University of Groningen, [Groningen].

Standard

Molecular gas and dust influenced by massive protostars : spectral surveys in the far-infrared and submillimeter. / van der Wiel, Matthijs H. D.

[Groningen] : Rijksuniversiteit Groningen, 2011. 167 p.

Research output: ThesisThesis fully internal (DIV)Academic

Vancouver

van der Wiel MHD. Molecular gas and dust influenced by massive protostars: spectral surveys in the far-infrared and submillimeter. [Groningen]: Rijksuniversiteit Groningen, 2011. 167 p.


BibTeX

@phdthesis{d16511dc04414c24861f733eda8a14ee,
title = "Molecular gas and dust influenced by massive protostars: spectral surveys in the far-infrared and submillimeter",
abstract = "The interstellar gas from which new stars form is crucially influenced by these same protostars: gas particles are excited and heated by the protostar. At the same time, the star formation process depends on the gas reservoir: if gas is too warm or dynamically 'stirred', it will not accumulate and contribute to the final mass of the forming star. This issue is specifically important in the formation of massive stars (more than eight times the mass of the Sun), because these stars produce at least 1000 times more radiation, impeding the accretion of gas. In this thesis I analyze primarily spectroscopic observations in the far-infrared and submillimeter wavelength regimes. Molecular constituents of interstellar gas are detected in these observations with ground- and space-based telescopes. Comparisons with model simulations provide insight into the influence of massive protostars on the surrounding molecular gas, both from a physical and from a chemical point of view. The results of this research indicate inhomogeneity in the density structure of the gas reservoirs that surround protostars, both in small-scale 'clumpiness' and on larger scales, for example in the form of axi-symmetric, carved-out areas through which excess energy can escape. Other aspects of the research emphasize how exchange between the gas phase and the surfaces of dust grains affects the interstellar chemical balance, and the power of the simple methylidyne molecule as a tracer of dynamically quiet gas in the otherwise violent environment of young massive stars. Chapters: (1) Introduction; (2) Star formation activity in IRDC G48.65; (3) Physical structure of the molecular envelope of AFGL2591; (4) Highly excited molecular gas in AFGL2591; (5) Chemical stratification in the Orion Bar; (6) CH gas toward NGC6334I; (7) Summary and future directions.",
keywords = "stars: formation, ISM: clouds, molecules, structure, techniques: imaging spectroscopy, astrochemistry, submillimeter, far-infrared, ISM: individual objects: AFGL2591, Orion Bar, NGC6334I, MSXDC G048.65-00.29",
author = "{van der Wiel}, {Matthijs H. D.}",
note = "Relation: https://www.rug.nl/ Rights: University of Groningen",
year = "2011",
month = "5",
language = "English",
isbn = "9789036748872",
publisher = "Rijksuniversiteit Groningen",
school = "University of Groningen",

}

RIS

TY - THES

T1 - Molecular gas and dust influenced by massive protostars

T2 - spectral surveys in the far-infrared and submillimeter

AU - van der Wiel, Matthijs H. D.

N1 - Relation: https://www.rug.nl/ Rights: University of Groningen

PY - 2011/5

Y1 - 2011/5

N2 - The interstellar gas from which new stars form is crucially influenced by these same protostars: gas particles are excited and heated by the protostar. At the same time, the star formation process depends on the gas reservoir: if gas is too warm or dynamically 'stirred', it will not accumulate and contribute to the final mass of the forming star. This issue is specifically important in the formation of massive stars (more than eight times the mass of the Sun), because these stars produce at least 1000 times more radiation, impeding the accretion of gas. In this thesis I analyze primarily spectroscopic observations in the far-infrared and submillimeter wavelength regimes. Molecular constituents of interstellar gas are detected in these observations with ground- and space-based telescopes. Comparisons with model simulations provide insight into the influence of massive protostars on the surrounding molecular gas, both from a physical and from a chemical point of view. The results of this research indicate inhomogeneity in the density structure of the gas reservoirs that surround protostars, both in small-scale 'clumpiness' and on larger scales, for example in the form of axi-symmetric, carved-out areas through which excess energy can escape. Other aspects of the research emphasize how exchange between the gas phase and the surfaces of dust grains affects the interstellar chemical balance, and the power of the simple methylidyne molecule as a tracer of dynamically quiet gas in the otherwise violent environment of young massive stars. Chapters: (1) Introduction; (2) Star formation activity in IRDC G48.65; (3) Physical structure of the molecular envelope of AFGL2591; (4) Highly excited molecular gas in AFGL2591; (5) Chemical stratification in the Orion Bar; (6) CH gas toward NGC6334I; (7) Summary and future directions.

AB - The interstellar gas from which new stars form is crucially influenced by these same protostars: gas particles are excited and heated by the protostar. At the same time, the star formation process depends on the gas reservoir: if gas is too warm or dynamically 'stirred', it will not accumulate and contribute to the final mass of the forming star. This issue is specifically important in the formation of massive stars (more than eight times the mass of the Sun), because these stars produce at least 1000 times more radiation, impeding the accretion of gas. In this thesis I analyze primarily spectroscopic observations in the far-infrared and submillimeter wavelength regimes. Molecular constituents of interstellar gas are detected in these observations with ground- and space-based telescopes. Comparisons with model simulations provide insight into the influence of massive protostars on the surrounding molecular gas, both from a physical and from a chemical point of view. The results of this research indicate inhomogeneity in the density structure of the gas reservoirs that surround protostars, both in small-scale 'clumpiness' and on larger scales, for example in the form of axi-symmetric, carved-out areas through which excess energy can escape. Other aspects of the research emphasize how exchange between the gas phase and the surfaces of dust grains affects the interstellar chemical balance, and the power of the simple methylidyne molecule as a tracer of dynamically quiet gas in the otherwise violent environment of young massive stars. Chapters: (1) Introduction; (2) Star formation activity in IRDC G48.65; (3) Physical structure of the molecular envelope of AFGL2591; (4) Highly excited molecular gas in AFGL2591; (5) Chemical stratification in the Orion Bar; (6) CH gas toward NGC6334I; (7) Summary and future directions.

KW - stars: formation

KW - ISM: clouds

KW - molecules

KW - structure

KW - techniques: imaging spectroscopy

KW - astrochemistry

KW - submillimeter

KW - far-infrared

KW - ISM: individual objects: AFGL2591

KW - Orion Bar

KW - NGC6334I

KW - MSXDC G048.65-00.29

UR - http://adsabs.harvard.edu/abs/2011PhDT.........5V

M3 - Thesis fully internal (DIV)

SN - 9789036748872

PB - Rijksuniversiteit Groningen

CY - [Groningen]

ER -

ID: 14564908