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New Aspects of the Formation of the β Pictoris Moving Group
In a previous work, we explored the possibility that the β Pictorismoving group (BPMG), consisting of low-mass post-T Tauri stars, wasformed near the Scorpius-Centaurus OB association. The cause of theformation could be a Type II supernova exploding either in LowerCentaurus Crux (LCC) or the Upper Centaurus Lupus (UCL), the two oldersubgroups of that association. Here we present new results for BPMG. Amore detailed analysis of the orbit confinement in this group leads to astar distribution pattern at birth that can be considered as arepresentation of the density distribution in the natal cloud. We alsopropose a plausible origin for the supernova that could have triggeredthe star formation in BPMG by finding the past position of the runawaystar HIP 46950. We find that this scenario is capable of explaining theorigin of all the members of BPMG proposed by Zuckerman and coworkersand by Song and coworkers, with the exception of HIP 79881, which isprobably an old main-sequence interloper.
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| Takýmyýldýz: | Okcuk |
| Sað Açýklýk: | 19h18m30.25s |
| Yükselim: | +17°44'09.7" |
| Görünürdeki Parlaklýk: | 9.344 |
| özdevim Sað Açýklýk: | 0.1 |
| özdevim Yükselim: | -7.2 |
| B-T magnitude: | 9.818 |
| V-T magnitude: | 9.384 |
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