17,415 research outputs found
Early-stage star forming cloud cores in GLIMPSE Extended Green Objects (EGOs) as traced by organic species
In order to investigate the physical and chemical properties of massive star
forming cores in early stages, we analyse the excitation and abundance of four
organic species, CH3OH, CH3OCH3, HCOOCH3 and CH3CH2CN, toward 29 Extended Green
Object (EGO) cloud cores that were observed by our previous single dish
spectral line survey. The EGO cloud cores are found to have similar methanol
J_3-J_2 rotation temperatures of ~44 K, a typical linear size of ~0.036 pc, and
a typical beam averaged methanol abundance of several 10^(-9) (the beam
corrected value could reach several 10^(-7)). The abundances of the latter
three species, normalized by that of methanol, are found to be correlated also
across a large variety of clouds such as EGO cloud cores, hot corinos, massive
hot cores and Galactic Center clouds. The chemical properties of the EGO cloud
cores lie between that of hot cores and hot corinos. However, the abundances
and abundance ratios of the four species can not be satisfactorily explained by
recent chemical models either among the EGO cloud cores or among the various
types of cloud cores from literature
3E: Energy-Efficient Elastic Scheduling for Independent Tasks in Heterogeneous Computing Systems
Reducing energy consumption is a major design constraint for modern heterogeneous computing systems to minimize electricity cost, improve system reliability and protect environment. Conventional energy-efficient scheduling strategies developed on these systems do not sufficiently exploit the system elasticity and adaptability for maximum energy savings, and do not simultaneously take account of user expected finish time. In this paper, we develop a novel scheduling strategy named energy-efficient elastic (3E) scheduling for aperiodic, independent and non-real-time tasks with user expected finish times on DVFS-enabled heterogeneous computing systems. The 3E strategy adjusts processors’ supply voltages and frequencies according to the system workload, and makes trade-offs between energy consumption and user expected finish times. Compared with other energy-efficient strategies, 3E significantly improves the scheduling quality and effectively enhances the system elasticity
Effects of turbulent dust grain motion to interstellar chemistry
Theoretical studies have revealed that dust grains are usually moving fast
through the turbulent interstellar gas, which could have significant effects
upon interstellar chemistry by modifying grain accretion. This effect is
investigated in this work on the basis of numerical gas-grain chemical
modeling. Major features of the grain motion effect in the typical environment
of dark clouds (DC) can be summarised as follows: 1) decrease of gas-phase
(both neutral and ionic) abundances and increase of surface abundances by up to
2-3 orders of magnitude; 2) shifts of the existing chemical jumps to earlier
evolution ages for gas-phase species and to later ages for surface species by
factors of about ten; 3) a few exceptional cases in which some species turn out
to be insensitive to this effect and some other species can show opposite
behaviors too. These effects usually begin to emerge from a typical DC model
age of about 10^5 yr. The grain motion in a typical cold neutral medium (CNM)
can help overcome the Coulomb repulsive barrier to enable effective accretion
of cations onto positively charged grains. As a result, the grain motion
greatly enhances the abundances of some gas-phase and surface species by
factors up to 2-6 or more orders of magnitude in the CNM model. The grain
motion effect in a typical molecular cloud (MC) is intermediate between that of
the DC and CNM models, but with weaker strength. The grain motion is found to
be important to consider in chemical simulations of typical interstellar
medium.Comment: 20 pages, 10 figures and 2 table
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