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| Paper: |
X-rays from HH 154 |
| Volume: |
448, 16th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun |
| Page: |
729 |
| Authors: |
Schneider, P. C.; Günther, H. M.; Schmitt, J. H. M. M. |
| Abstract: |
Protostellar jets are observed during all stages of early stellar evolution. X-rays originating within these outflows have been observed only from ten such objects and require shock velocities of about 500 km s-1. L1551 IRS 5, the driving source of the Herbig-Haro object 154, is heavily absorbed. Therefore, one can study the outflow close to the launching zone without contaminating light from the power source.
We present a new third epoch Chandra observation of HH 154 which shows that the majority of the X-ray emission is concentrated within a small region close to the driving source over a timespan of 8 years. Reheating or replenishment of the plasma is required in order to explain the observations. The evolution of the temperature of the X-ray emitting plasma suggests that the heating occurs within the innermost region (∼150 AU) of the outflow. |
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