5,898 research outputs found
Fire from Ice - Massive Star Birth from Infrared Dark Clouds
I review massive star formation in our Galaxy, focusing on initial conditions
in Infrared Dark Clouds (IRDCs), including the search for massive pre-stellar
cores (PSCs), and modeling of later stages of massive protostars, i.e., hot
molecular cores (HMCs). I highlight how developments in astrochemistry, coupled
with rapidly improving theoretical/computational and observational capabilities
are helping to improve our understanding of the complex process of massive star
formation.Comment: To appear in proceedings of IAU Symp. 322, Astrochemistry VII Through
the Cosmos from Galaxies to Planet
Astrochemistry of Sub-Millimeter Sources in Orion: Studying the Variations of Molecular Tracers with Changing Physical Conditions
Cornerstone molecules (CO, H_2CO, CH_3OH, HCN, HNC, CN, CS, SO) were observed
toward seven sub-millimeter bright sources in the Orion molecular cloud in
order to quantify the range of conditions for which individual molecular line
tracers provide physical and chemical information. Five of the sources observed
were protostellar, ranging in energetics from 1 - 500L_sun, while the other two
sources were located at a shock front and within a photodissociation region
(PDR).
Statistical equilibrium calculations were used to deduce from the measured
line strengths the physical conditions within each source and the abundance of
each molecule. In all cases except the shock and the PDR, the abundance of CO
with respect to H_2 appears significantly below (factor of ten) the general
molecular cloud value of 10^-4. {Formaldehyde measurements were used to
estimate a mean temperature and density for the gas in each source. Evidence
was found for trends between the derived abundance of CO, H_2CO, CH_3OH, and CS
and the energetics of the source, with hotter sources having higher
abundances.} Determining whether this is due to a linear progression of
abundance with temperature or sharp jumps at particular temperatures will
require more detailed modeling. The observed methanol transitions require high
temperatures (T>50 K), and thus energetic sources, within all but one of the
observed protostellar sources. The same conclusion is obtained from
observations of the CS 7-6 transition. Analysis of the HCN and HNC 4-3
transitions provides further support for high densities n> 10^7 cm^-3 in all
the protostellar sources.Comment: 36 pages, 8 figures, Astronomy and Astrophysics in pres
Astrochemistry: overview and challenges
This paper provides a brief overview of the journey of molecules through the
Cosmos, from local diffuse interstellar clouds and PDRs to distant galaxies,
and from cold dark clouds to hot star-forming cores, protoplanetary disks,
planetesimals and exoplanets. Recent developments in each area are sketched and
the importance of connecting astronomy with chemistry and other disciplines is
emphasized. Fourteen challenges for the field of Astrochemistry in the coming
decades are formulated.Comment: 20 pages, 5 figures, to appear in IAU Symposium 332 "Astrochemistry
VII: Through the Cosmos from Galaxies to Planets", eds. M. Cunningham, T.J.
Millar, Y. Aikaw
Astrochemistry of dust, ice and gas: introduction and overview
A brief introduction and overview of the astrochemistry of dust, ice and gas
and their interplay is presented, aimed at non-specialists. The importance of
basic chemical physics studies of critical reactions is illustrated through a
number of recent examples. Such studies have also triggered new insight into
chemistry, illustrating how astronomy and chemistry can enhance each other.
Much of the chemistry in star- and planet-forming regions is now thought to be
driven by gas-grain chemistry rather than pure gas-phase chemistry, and a
critical discussion of the state of such models is given. Recent developments
in studies of diffuse clouds and PDRs, cold dense clouds, hot cores,
protoplanetary disks and exoplanetary atmospheres are summarized, both for
simple and more complex molecules, with links to papers presented in this
volume. In spite of many lingering uncertainties, the future of astrochemistry
is bright: new observational facilities promise major advances in our
understanding of the journey of gas, ice and dust from clouds to planets.Comment: Introductory paper for Faraday Discussions 168 conference, April 201
Aromatic Hydrocarbons, Diamonds, and Fullerenes in Interstellar Space: Puzzles to be Solved by Laboratory and Theoretical Astrochemistry
New research is presented, and previous research is reviewed, on the emission
and absorption of interstellar aromatic hydrocarbons. Emission from aromatic
hydrocarbons dominate the mid-infrared emission of many galaxies, including our
own Milky Way galaxy. Only recently have aromatic hydrocarbons been observed in
absorption in the interstellar medium, along lines of sight with high column
densities of interstellar gas and dust. Much work on interstellar aromatics has
been done, with astronomical observations and laboratory and theoretical
astrochemistry. In many cases the predictions of laboratory and theoretical
work are confirmed by astronomical observations, but in other cases clear
discrepancies exist which provide problems to be solved by a combination of
astronomical observations, laboratory studies, and theoretical studies. The
emphasis of this paper will be on current outstanding puzzles concerning
aromatic hydrocarbons which require further laboratory and theoretical
astrochemistry to resolve. This paper will also touch on related topics where
laboratory and theoretical astrochemistry studies are needed to explain
astrophysical observations, such as a possible absorption feature due to
interstellar "diamonds" and the search for fullerenes in space.Comment: Spectrochimica Acta A, Feb. 2001, in press. 33 pages including 11
postscript figures, AASTeX format. Full postscript paper also available at
http://www.astronomy.ohio-state.edu/~sellgren/saa.htm
Astrochemistry and Astrophotonics for an Antarctic Observatory
Due to its location and climate, Antarctica offers unique conditions for
long-period observations across a broad wavelength regime, where important
diagnostic lines for molecules and ions can be found, that are essential to
understand the chemical properties of the interstellar medium. In addition to
the natural benefits of the site, new technologies, resulting from
astrophotonics, may allow miniaturised instruments, that are easier to
winterise and advanced filters to further reduce the background in the
infrared.Comment: 4 pages, to be published in EAS Publications Series, Vol. 40, Proc.
of 3rd ARENA conferenc
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