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DTEND:20260709T101500Z
UID:746d13c027ed376ddaaf6ffc62d9b74b@physik.uni-heidelberg.de
DTSTAMP:20260709T214936Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:I will review the recent progress that we have made in understa
 nding nucleosynthesis in the Universe and the accretion history of the Milk
 y Way through chemodynamical analysis of the stellar halo. Over the last fi
 ve years\, we have been complementing the discoveries from the Gaia mission
  with high-resolution spectroscopic follow-ups of halo stars. These studies
  have provided detailed chemical abundances of stars in stellar streams\, r
 evealing the origins of these streams. There have also been serendipitous d
 iscoveries during these follow-ups leading to new insights into broader top
 ics in astrophysics\, such as the discovery of Li-rich stars in stellar str
 eams and the association of a 33 Msun solar mass black hole with a stellar 
 stream. After reviewing these discoveries\, I will discuss the future prosp
 ects of this field in light of the recently started spectroscopic surveys\,
  namely 4MOST and WEAVE\, hopefully with initial results from them by the t
 ime of the colloquium. Finally\, I will briefly introduce the next generati
 on spectroscopic facilities that are currently being discussed. In addition
  to these scientific topics\, I will also share my personal experience of b
 eing a Gliese fellow at ARI for three years and how it has impacted my care
 er.\n\nImported from https://www.physik.uni-heidelberg.de/hephysto/ (no war
 ranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12574
SUMMARY:ARI Institute Colloquium: Tadafumi Matsuno - Nucleosynthesis and th
 e Milky Way&apos\;s accretion history: What we have learned and what we wil
 l learn
DTSTART:20260709T091500Z
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DTEND:20260716T101500Z
UID:c2c1b7ed523319b204fbdc3d5819c3fa@physik.uni-heidelberg.de
DTSTAMP:20260709T214936Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:Westerlund 1 (Wd 1) is the most massive young stellar cluster i
 n the Galaxy\, and hosts a uniquely numerous\, diverse and nearby populatio
 n of evolved massive stars including 24 Wolf-Rayet stars\, several yellow a
 nd red supergiants\, a luminous blue variable and over 100 OB supergiants. 
 In this talk I will report on the supergiant B[e] star Wd1-9\, which we now
  know to be a recently stripped massive binary system deeply embedded in a 
 dense rotating circumstellar medium and bipolar photoevaporating outflow re
 miniscent of a protoplanetary disk wind. I will also detail how hydrodynami
 c simulations of outflows from massive stars coupled with EWOCS data can co
 nstrain supergiant evolutionary pathways in clusters. I will show how a rec
 ent (~10 kyr ago) non-conservative mass transfer event can explain the unus
 ual nebulosity around the WR+O binary system Wd1-72. I will also demonstrat
 e how the mysterious "pillar/rat" nebula in Wd 1 could have been produced b
 y the yellow supergiant Wd1-4 transitioning from a red supergiant in the pa
 st ~15 kyr\, and how similar models of cool supergiants in clusters have th
 e potential to robustly measure their uncertain mass-loss rates.\n\nImporte
 d from https://www.physik.uni-heidelberg.de/hephysto/ (no warranty for accu
 racy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12575
SUMMARY:ARI Institute Colloquium: Cormac Larkin - The EWOCS view of the mas
 sive stellar zoo Westerlund 1
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DTEND:20260723T101500Z
UID:6983b0f0140ba0a87b66af6485aea08f@physik.uni-heidelberg.de
DTSTAMP:20260709T214936Z
LOCATION:ARI\, Moenchhofstrasse 12-14\, Seminarraum 1.OG
DESCRIPTION:Hot\, massive stars are astrophysical keystones which shape the
 ir environment via mechanical and radiative feedback and chemically enrich 
 their cosmic neighborhood since the first generation of (very) massive star
 s. However\, turning this general textbook picture into quantitative predic
 tion remains an ongoing challenge. Recent discoveries\, such the surprising
 ly high metallicity and early nitrogen enrichment in high-redshift galaxies
  discovered by JWST\, put current descriptions and modelling approaches int
 o question\, illustrating that the complex puzzle of massive stars and thei
 r interplay is everything but complete.\n\nTo get a robust\, quantitative u
 nderstanding\, decoding and predicting the light of hot massive stars marks
  an astrophysical key technique. Revolving around via the development and a
 pplication of expanding stellar atmosphere models for hot stars\, I will pr
 esent a selection of recent research results from my group. A particular fo
 cus will be on star with strong stellar winds\, their enigmatic cosmic role
 \, and the challenge to get a coherent structural and evolutionary understa
 nding of these objects. Moreover\, I will present our recent discovery of a
 n unexpected direct transition in the Wolf-Rayet regime from WN to WO subty
 pe occuring at subsolar metallicity as well as ongoing and forthcoming effo
 rts in further developing atmosphere modelling and quantitative spectroscop
 y.\n\nImported from https://www.physik.uni-heidelberg.de/hephysto/ (no warr
 anty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12576
SUMMARY:ARI Institute Colloquium: Andreas Sander - Hot\, massive stars and 
 their winds: New insights and open puzzles
DTSTART:20260723T091500Z
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