2-6 September 2024
CJD Bonn Castell
Europe/Berlin timezone
- evn2024@mpifr.de
Support
Session XII: Young stellar objects -- Chair: Anna Bartkiewicz
Place
Location: CJD Bonn Castell
Address: Graurheindorfer Str. 149, 53117 Bonn
Date:
5 Sep 09:00 - 10:30
Description
30 min Invited Talk on YSOs
4x 15min Contributed Talk
Timetable | Contribution List
Displaying 5
contributions
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5
IRAS 20126+4104 (G78.122+3.633) is a well-studied high-mass protostar that still presents unanswered questions, such as the cause of 6.7 GHz methanol maser short-term fluctuations (ranging from 5 to 60 days) and how individual maser cloudlets respond to transitions from long low-activity periods to long high-intensity periods. To address these questions, we are utilizing combined 6.7 GHz methanol
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Presented by Artis ABERFELDS
on
5/9/2024
at
10:15
The formation process of high-mass stars (M > 8 Msun) is still unclear; this is mainly due to their fast evolution and large distances that make it very difficult to observe them in detail. However, many observational and theoretical efforts have been made in the last decades that have shed light on some aspects of the formation process. For instance, it has been shown that molecular outflows are
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Presented by Dr. Gabriele SURCIS
on
5/9/2024
at
7:00
Very Long Baseline Interferometry (VLBI) provides high angular resolution images and has been used for stellar astrometry for decades. In the DYNAMO-VLBA project, we utilize the Very Long Baseline Array (VLBA) to study tight binary and multiple pre-main-sequence stars, whose components have detectable radio emission and typical separations on the order of milli-arcseconds. Consequently, Gaia canno
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Presented by Jazmín ORDÓÑEZ-TORO
on
5/9/2024
at
9:30
Cosmic masers enable us to estimate the magnetic field via the Zeeman effect, especially in
high-mass star-forming regions where OH and methanol masers occur. We can measure the
Zeeman-splitting of the maser lines and, knowing the Landé g-factor, determine the strength
of the magnetic field. The g-factor is undoubtedly known for the excited OH maser, but for
methanol masers, it is still under
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Presented by Ms. Agnieszka KOBAK
on
5/9/2024
at
10:00
Magnetically active low-mass young stars can produce nonthermal radio emission with brightness temperatures well above 10**6 K, which can be detected with the VLBI technique. The Orion Nebula Cluster (ONC) contains a rich population of young stars, where thousands are low-mass stars. Radio observations have shown that in the core of the ONC about 600 of these low-mass stars are radio emitters. We
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Presented by Sergio Abraham DZIB QUIJANO
on
5/9/2024
at
9:45