No abstract

No abstract

The collapse and fragmentation of molecular cloud cores is examined numerically with unprecedentedly high spatial resolutions, using the publicly released code GADGET-2. As templates for the model clouds we use the ''standard isothermal test case'' in the variant calculated by Burkert & Bodenheimer in 1993 and the centrally condensed, Gaussian cloud advanced by Boss in 1991. A barotropic equation of state is used to mimic the nonisothermal collapse. We investigate both the sensitivity of fragmentation to thermal retardation and the level of resolution needed by smoothed particle hydrodynamics (SPH ) to achieve convergence to existing Jeans-resolved, finite-difference ( FD) calculations. We find that working with 0.6Y1.2 million particles, acceptably good convergence is achieved for the standard test model. In contrast, convergent results for the Gaussian-cloud model are achieved using from 5 to 10 million particles. If the isothermal collapse is prolonged to unrealistically high densities, the outcome of collapse for the Gaussian cloud is a central adiabatic core surrounded by dense trailing spiral arms, which in turn may fragment in the late evolution. If, on the other hand, the barotropic equation of state is adjusted to mimic the rise of temperature predicted by radiative transfer calculations, the outcome of collapse is a protostellar binary core. At least, during the early phases of collapse leading to formation of the first protostellar core, thermal retardation not only favors fragmentation but also results in an increased number of fragments, for the Gaussian cloud.

No abstract

The physical mechanisms that cause the heating of the solar corona are still far from being completely understood. However, recent highly resolved observations with the current solar missions have shown clear evidence of frequent and very localized heating events near the chromosphere that may be responsible for the observable high temperatures of the coronal plasma. In this paper, we perform one-dimensional hydrodynamic simulations of the evolution of a hypothetical loop model undergoing impulsive heating through the release of localized Gaussian energy pulses near the loop's footpoints. We find that when a discrete number of randomly spaced pulses is released, loops of length L ¼ 5 and 10 Mm heat up and stay at coronal temperatures for the whole duration of the impulsive heating stage, provided that the elapsed time between successive heat injections is P175 and P215 s, respectively. The precise value of the critical elapsed time is sensitive to the loop length. In particular, we find that for increased loop lengths of 20 and 30 Mm, the critical elapsed time rises to about 240 and 263 s, respectively. For elapsed times longer than these critical values, coronal temperatures can no longer be maintained at the loop apex in spite of continued impulsive heating. As a result, the loop apex undergoes runaway cooling well below the initial state, reaching chromospheric temperatures ($10 4 K) and leading to the typical hot-cool temperature profile characteristic of a cool condensation. For a large number of pulses (up to $1000) having a fully random spatiotemporal distribution, the variation of the temperature along the loop is highly sensitive to the spatial distribution of the heating. As long as the heating concentrates more and more at the loop's footpoints, the temperature variation is seen to make a transition from that of a uniformly heated loop to a flat, isothermal profile along the loop length. Concentration of the heating at the footpoints also results in a more frequent appearance of rapid and significant depressions of the apex temperature during the loop evolution, most of them ranging from $1:5 ; 10 6 to $10 4 K and lasting from about 3 to 10 minutes. This behavior bears a tight relation with the strong variability of coronal loops inferred from SOHO observations in active regions of the solar atmosphere.