Calendar
Mar
8
mer
Mar 8@16:00–17:00
It is debated whether the long and intense flares observed on the PMS stars in Orion involve single and very long magnetic channels or much flatter loop arcades. This question is important because the long flaring channels may be so long as to connect the star to the circumstellar disk. In this work a new method solves the question …. (suspence is left on purpose).
Mar
10
ven
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Mar
15
mer
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Mar
17
ven
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Mar
23
gio
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Apr
20
gio
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Mag
2
mar
Mag 2@15:30–16:30
ABSTRACT:
Orion is a forgery of young stars, composed of several groups and associations that span different ages (1-15 Myr) distances (350-450 pc) and masses (from BDs to O type stars). X-rays can be used to infer distances of groups of young stars and thus the spatial structure of the Orion complex. Exploring the synergy of IR and X-ray observations, I present the first results from a recent XMM observation of a group
of young stellar objects around V1818 Ori. This is a follow up devoted to explore the eastern edge of a ring of dust around Kappa Ori(a B0 V star) that embeds groups of YSOs to the west of the star itself. My preliminary analysis shows that also the group of V1818 Ori belongs to the Kappa Ori cluster at 250 pc and is unrelated to the Mon R2 region to which it has been associated so far.
of young stellar objects around V1818 Ori. This is a follow up devoted to explore the eastern edge of a ring of dust around Kappa Ori(a B0 V star) that embeds groups of YSOs to the west of the star itself. My preliminary analysis shows that also the group of V1818 Ori belongs to the Kappa Ori cluster at 250 pc and is unrelated to the Mon R2 region to which it has been associated so far.
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