346,158 research outputs found
Laboratory Astrophysics and the State of Astronomy and Astrophysics
Laboratory astrophysics and complementary theoretical calculations are the
foundations of astronomy and astrophysics and will remain so into the
foreseeable future. The impact of laboratory astrophysics ranges from the
scientific conception stage for ground-based, airborne, and space-based
observatories, all the way through to the scientific return of these projects
and missions. It is our understanding of the under-lying physical processes and
the measurements of critical physical parameters that allows us to address
fundamental questions in astronomy and astrophysics. In this regard, laboratory
astrophysics is much like detector and instrument development at NASA, NSF, and
DOE. These efforts are necessary for the success of astronomical research being
funded by the agencies. Without concomitant efforts in all three directions
(observational facilities, detector/instrument development, and laboratory
astrophysics) the future progress of astronomy and astrophysics is imperiled.
In addition, new developments in experimental technologies have allowed
laboratory studies to take on a new role as some questions which previously
could only be studied theoretically can now be addressed directly in the lab.
With this in mind we, the members of the AAS Working Group on Laboratory
Astrophysics, have prepared this State of the Profession Position Paper on the
laboratory astrophysics infrastructure needed to ensure the advancement of
astronomy and astrophysics in the next decade.Comment: Position paper submitted by the AAS Working Group on Laboratory
Astrophysics (WGLA) to the State of the Profession (Facilities, Funding and
Programs Study Group) of the Astronomy and Astrophysics Decadal Survey
(Astro2010
The VLT-FLAMES survey of massive stars: Wind properties and evolution of hot massive stars in the LMC
[Abridged] We have studied the optical spectra of 28 O- and early B-type
stars in the Large Magellanic Cloud, 22 of which are associated with the young
star-forming region N11. Stellar parameters are determined using an automated
fitting method, combining the stellar atmosphere code FASTWIND with the
genetic-algorithm optimisation routine PIKAIA. Results for stars in the LH9 and
LH10 associations of N11 are consistent with a sequential star formation
scenario, in which activity in LH9 triggered the formation of LH10. Our sample
contains four stars of spectral type O2, of which the hottest is found to be
~49-54 kK (cf. ~45-46 kK for O3 stars). The masses of helium-enriched dwarfs
and giants are systematically lower than those implied by non-rotating
evolutionary tracks. We interpret this as evidence for efficient
rotationally-enhanced mixing, leading to the surfacing of primary helium and to
an increase of the stellar luminosity. This result is consistent with findings
for SMC stars by Mokiem et al. For bright giants and supergiants no such
mass-discrepancy is found, implying that these stars follow tracks of modestly
(or non-)rotating objects. Stellar mass-loss properties were found to be
intermediate to those found in massive stars in the Galaxy and the SMC, and
comparisons with theoretical predictions at LMC metallicity yielded good
agreement over the luminosity range of our targets, i.e. 5.0 < log L/L(sun) <
6.1
Nuclear Astrophysics
Nuclear physics has a long and productive history of application to
astrophysics which continues today. Advances in the accuracy and breadth of
astrophysical data and theory drive the need for better experimental and
theoretical understanding of the underlying nuclear physics. This paper will
review some of the scenarios where nuclear physics plays an important role,
including Big Bang Nucleosynthesis, neutrino production by our sun,
nucleosynthesis in novae, the creation of elements heavier than iron, and
neutron stars. Big-bang nucleosynthesis is concerned with the formation of
elements with A <= 7 in the early Universe; the primary nuclear physics inputs
required are few-nucleon reaction cross sections. The nucleosynthesis of
heavier elements involves a variety of proton-, alpha-, neutron-, and
photon-induced reactions, coupled with radioactive decay. The advent of
radioactive ion beam facilities has opened an important new avenue for studying
these processes, as many involve radioactive species. Nuclear physics also
plays an important role in neutron stars: both the nuclear equation of state
and cooling processes involving neutrino emission play a very important role.
Recent developments and also the interplay between nuclear physics and
astrophysics will be highlighted.Comment: To be published in the Proceedings of 19th Lake Louise Winter
Institute (15-21 February 2004). 9 pages, 3 figure
Astrophysics
Historical account of astrophysics development based on photometry and spectroscop
X-ray Sources and their Optical Counterparts in the Globular Cluster M4
We report on the Chandra X-ray Observatory ACIS-S3 imaging observation of the
Galactic globular cluster M4 (NGC 6121). We detect 12 X-ray sources inside the
core and 19 more within the cluster half-mass radius. The limiting luminosity
of this observation is Lx~10e29 erg/sec for sources associated with the
cluster, the deepest X-ray observation of a globular cluster to date. We
identify 6 X-ray sources with known objects and use ROSAT observations to show
that the brightest X-ray source is variable. Archival data from the Hubble
Space Telescope allow us to identify optical counterparts to 16 X-ray sources.
Based on the X-ray and optical properties of the identifications and the
information from the literature, we classify two (possibly three) sources as
cataclysmic variables, one X-ray source as a millisecond pulsar and 12 sources
as chromospherically active binaries. Comparison of M4 with 47 Tuc and NGC 6397
suggests a scaling of the number of active binaries in these clusters with the
cluster (core) mass.Comment: 11 pages, 6 figures, accepted for publication in ApJ. Figure 1 and 5
are of reduced qualit
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