114 research outputs found
The Effects of Radiation Feedback on Early Fragmentation and Multiplicity
Forming stars emit a significant amount of radiation into their natal
environment. While the importance of radiation feedback from high-mass stars is
widely accepted, radiation has generally been ignored in simulations of
low-mass star formation. I use ORION, an adaptive mesh refinement (AMR)
three-dimensional gravito-radiation-hydrodynamics code, to model low-mass star
formation in a turbulent molecular cloud. I demonstrate that including
radiation feedback has a profound effect on fragmentation and protostellar
multiplicity. Although heating is mainly confined within the core envelope, it
is sufficient to suppress disk fragmentation that would otherwise result in
low-mass companions or brown dwarfs. As a consequence, turbulent fragmentation,
not disk fragmentation, is likely the origin of low-mass binaries.Comment: 4 pages, 2 figures, to appear in the Proceedings of IAU Symposium
270: Computational Star Formatio
SABOCA 350-micron and LABOCA 870-micron dust continuum imaging of IRAS 05399-0121: mapping the dust properties of a pre- and protostellar core system
We present a 350 micron APEX/SABOCA map of IRAS 05399-0121/SMM 1, which is a
dense double-core system in Orion B9. We combined these data with our previous
LABOCA 870-micron data. The spatial resolution of the new SABOCA image, ~3400
AU, is about 2.6 times better than provided by LABOCA. We also make use of
Spitzer infrared observations to characterise the star-formation activity in
the source. The source is filamentary and remains a double-core system on the
3400 AU scale probed here, where the projected separation between IRAS 05399
and SMM 1 is 0.14 pc. The broadband spectral energy distribution of IRAS 05399
suggests that it is near the Stage 0/I borderline. A visual inspection of the
Spitzer/IRAC images provides hints of a quadrupolar-like jet morphology around
IRAS 05399, supporting the possibility that it is a binary system. The
temperature map reveals warm spots towards IRAS 05399 and the southeastern tip
of the source. These features are likely to be imprints of protostellar or
shock heating, while external heating could be provided by the nearby high-mass
star-forming region NGC 2024. A simple analysis suggests that the density
profile at the position of SMM 1 has the form ~r^-(2.3_{-0.9}^{+2.2}). The
source splitting into two subcores along the long axis can be explained by
cylindrical Jeans-type fragmentation but the steepness of the density profile
is shallower than what is expected for an isothermal cylinder. The difference
between the evolutionary stages of IRAS 05399 (protostellar) and SMM 1
(starless) suggests that the former has experienced a phase of rapid mass
accretion, supported by the very long outflow it drives. The protostellar jet
from IRAS 05399 might have influenced the nearby core SMM 1.Comment: A&A, in press; 14 pages, 7 figures, 3 tables; very minor language
corrections+revised arXiv abstrac
An Alternative Accurate Tracer of Molecular Clouds: The "-Factor"
We explore the utility of CI as an alternative high-fidelity gas mass tracer
for Galactic molecular clouds. We evaluate the X-factor for the 609
m carbon line, the analog of the CO X-factor, which is the ratio of the
H column density to the integrated CO(1-0) line intensity. We use
3D-PDR to post-process hydrodynamic simulations of turbulent, star-forming
clouds. We compare the emission of CI and CO for model clouds irradiated by 1
and 10 times the average background and demonstrate that CI is a comparable or
superior tracer of the molecular gas distribution for column densities up to cm. Our results hold for both reduced and full chemical
networks. For our fiducial Galactic cloud we derive an average of
cmKkms and of cmKkms.Comment: 5 pages, 4 figures, 1 table, accepted to MNRAS Letter
The Kinematics of Molecular Cloud Cores in the Presence of Driven and Decaying Turbulence: Comparisons with Observations
In this study we investigate the formation and properties of prestellar and
protostellar cores using hydrodynamic, self-gravitating Adaptive Mesh
Refinement simulations, comparing the cases where turbulence is continually
driven and where it is allowed to decay. We model observations of these cores
in the CO, NH, and NH lines, and from
the simulated observations we measure the linewidths of individual cores, the
linewidths of the surrounding gas, and the motions of the cores relative to one
another. Some of these distributions are significantly different in the driven
and decaying runs, making them potential diagnostics for determining whether
the turbulence in observed star-forming clouds is driven or decaying. Comparing
our simulations with observed cores in the Perseus and Ophiuchus clouds
shows reasonably good agreement between the observed and simulated core-to-core
velocity dispersions for both the driven and decaying cases. However, we find
that the linewidths through protostellar cores in both simulations are too
large compared to the observations. The disagreement is noticably worse for the
decaying simulation, in which cores show highly supersonic infall signatures in
their centers that decrease toward their edges, a pattern not seen in the
observed regions. This result gives some support to the use of driven
turbulence for modeling regions of star formation, but reaching a firm
conclusion on the relative merits of driven or decaying turbulence will require
more complete data on a larger sample of clouds as well as simulations that
include magnetic fields, outflows, and thermal feedback from the protostars.Comment: 18 pages, 12 figures, accepted to A
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