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Prof. Paola Caselli (Max Planck Institute for Extraterrestrial Physics)06/05/2025, 09:30Review/Invited talk
Extremely low temperatures and relatively low densities characterize the interstellar clouds precursors of stars and planets. In these early stages, fundamental chemical and physical processes affect each other, ultimately regulating clouds' dynamical evolution toward the formation of stellar systems like ours, where at least one habitable planet is present. Here, I'll present a journey from...
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Dr Hsien Shang (Institute of Astronomy and Astrophysics, Academia Sinica)06/05/2025, 10:00Review/Invited talk
A plethora of new enigmatic phenomena in the innermost parts of protostellar systems associated with jets and outflows have been revealed by ALMA and JWST. These jets and outflows, along with the streamers from their magnetically collapsing prenatal envelopes, are integral parts of the physical processes that assemble the systems. We review the characteristics of these enigmatic, powerful...
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Mario Tafalla (Observatorio Astronomico Nacional (Spain))06/05/2025, 10:20Review/Invited talk
Characterizing the molecular emission from whole molecular clouds is critical to identify the physical and chemical processes that act at different spatial scales and lead to the formation of stars. It is also needed to connect spatially-resolved observations of galactic clouds with extragalactic observations that do not resolve the clouds.
The traditional approach of characterizing the...
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06/05/2025, 10:40Poster
Marie-Anne Carpine, Alessandro Coletta (Davide Elia), Leonardo Berti, Alice Nucara (Patrick Hennebelle)
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Alberto Sanna (Istituto Nazionale di Astrofisica (INAF))06/05/2025, 11:20Contributed talk
Located at the edge of the Cepheus Bubble, the massive star-forming region Cepheus A hosts HW2, a very young star growing more than dozen times the mass of our Sun - and the second closest of its kind to us. Using sensitive VLA observations, we have finally imaged its debated accretion disk in hot ammonia at centimeter wavelengths. We have resolved the accretion disk within a few hundred au of...
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Valentin Le Gouellec (ICE-CSIC)06/05/2025, 11:40Contributed talk
Sun-like stars are thought to accrete most of their final mass during the protostellar phase, where the protostellar embryo is surrounded by an infalling dense envelope. The so-called Class 0 phase designates the youngest protostellar stage, where the accretion is the most vigorous. Because these objects are highly embedded, it is difficult to retrieve direct diagnostics from the accretion,...
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Alvaro Sanchez-Monge (Institute of Space Sciences (ICE, CSIC))06/05/2025, 12:00Contributed talk
Stars form preferentially in clusters deeply embedded inside massive molecular clouds. Some of these clusters contain high-mass stars that influence their immediate environment through gravitational, mechanical and radiative interactions, and eventually through supernova explosions. Therefore, a comprehensive understanding of star formation requires characterizing the formation and early...
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Griselda Arroyo-Chavez (Steward Observatory - University of Arizona)06/05/2025, 12:20Contributed talk
For many years, evidence of large-scale velocity gradients has been found in molecular clouds and filaments, which are commonly associated with rotation. It is known that during the collapse and fragmentation of these structures, a process of redistribution and loss of angular momentum is involved, such that the fragments possess less angular momentum per unit of mass than their parent...
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06/05/2025, 12:40Poster
Adnan Ali Ahmad, Valentin Vallucci-Goy, Chiara Mininni (Davide Elia)
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Pierre Dumond (ENS Lyon)Poster
Explaining the universality of the peak of the Core Mass Function is a major unsolved problem in astrophysics. Recently, Jaupart & Chabrier (2021) suggested that this universality can be related to a mass invariant M_inv first derived by Chandrasekhar (1951) based on several assumptions, namely the statistical homogeneity of the turbulent density field.
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This invariant depends on the variance... -
Valentin Vallucci-Goy (CEA Saclay)Poster
Dust grains plays an essential role in many fields of astrophysics. In particular, they are the main charge carriers during the protostellar collapse and as such, control the evolution of angular momentum [1,2]. In addition, they are the fondamental bricks for the formation of planetesimals and planets [3].
Firstly, we perform single-zone simulations including a complex chemical network to...
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Dr Ilseung Han (Institut de Ciències de l'Espai, CSIC)Poster
We present high-resolution (0.05"; 8 au) dust continuum and molecular line observations toward the Class I protostellar system IRAS 04169+2702 in the Taurus B213 region ($d$ = 156 pc), as part of the ALMA Large Program Early Planet Formation in Embedded Disks (eDisk). The 1.3-mm dust continuum emission traces a circumstellar disk with a central depression toward the protostar. Our...
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Marie-Anne CARPINE (CEA/DRF/DAp - AIM)Poster
The characterisation of cosmic dust properties is key for understanding, among other things, star and planet formation processes. Astronomical observations provide us information from which it is possible, but not trivial, to deduce physical properties of cosmic dust. For instance, recent observations of 12 young protostars found dust emissivity indices with values β < 1 [Maury et al. 2019,...
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Noé Brucy (ENS Lyon)Poster
Several attempts have been made to build analytical model for galactic star formation rates. This models prove extremely useful in many contexts, from cosmological and galactic simulations to the interpretation of observations.
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In this talk I will present a set of numerical simulations that challenge the existing analytical models for high-Mach numbers. I will then present a set of conceptual... -
Dr Pedro R. Rivera-Ortiz (Institute of Radioastronomy and Astrophysics UNAM)Poster
Theoretical models suggest that jet-driven bow shocks govern Class 0/I molecular outflow morphologies extending up to $10^{4-5}$ au, with additional modifications arising from binary motion, precession, and ambient interactions due to other outflows produced by clustered or binary protostars. Previous studies have demonstrated that outflow interactions in clustered environments are common,...
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Ashley Bemis (Waterloo Centre for Astrophysics)Poster
Regions with higher star formation rates are thought to have more dense, molecular gas that serves as the direct fuel for star formation. However, resolved studies of nearby galaxies find systematic variations in the star formation efficiency of dense gas (SFEdense) with local galactic environment. One physical explanation for this behaviour is the suppression of star formation in dense...
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Adnan Ali Ahmad (CRAL - ENS LYON)Poster
Describing the collapse of a gravitationaly unstable cloud core to stellar densities requires one to tackle a huge dynamical range, where a first core in hydrostatic equilibrium forms, which then collapses again following the dissociation of H$_2$ to form a protostar. Since R. Larson's (Larson 1969) pioneering work, second-collapse calculations have advanced significantly by incorporating...
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Alvaro Sanchez-Monge (Institute of Space Sciences (ICE, CSIC))Contributed talk
The giant molecular cloud Sagittarius B2 (hereafter SgrB2) is the most massive region with ongoing high-mass star formation in the Galaxy. In the southern half of the 20-pc large envelope of SgrB2, we encounter the SgrB2(DS) region which hosts more than 60 high-mass proto-stellar cores distributed in an arc shape around an extended HII region. We use the Very Large Array in its CnB and D...
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