Ruprecht-Karls-Universität Heidelberg

Events, Seminars, Talks

A list of all Physics & Astronomy talks and seminars taking place in Heidelberg can be found at HePhySTO.


Upcoming events


2021-11-30
16:00
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Gas dynamics, inflow and star formation in the innermost 3 kpc of the Milky Way
Dr Mattia Sormani (ITA/ZAH, University of Heidelberg)
Heidelberg Joint Astronomical Colloquium ( Home pageHephysto link )
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I will give an introduction to gas dynamics and star formation in the central region (R<3kpc) of the Milky Way. This region is dominated by the strongly non-axisymmetric gravitational potential of the Galactic bar. After reviewing the basic theoretical tools, I will discuss several topics including (i) how to interpret the observed longitude-velocity maps of CO, HI and other interstellar gas tracers; (ii) how we can use the gas dynamics to constrain the properties of the Galactic bar; (iii) how the gas is driven inwards from the Galactic disc (R~3kpc) down to the Central Molecular Zone (CMZ, R~120pc) and then to the central black hole SgrA*; (iv) the spatial and temporal distribution of star formation in the Galactic centre. Finally, I will highlight some open questions and directions of future research.

2021-12-02
11:15
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Populations of satellite galaxies with the IllustrisTNG simulations: from galaxy clusters to the Local Group
Christoph Engler (ARI)
ARI Institute Colloquium ( Hephysto link )
ARI, Moenchhofstrasse 12-14, Seminarraum 1, 1.OG
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I present populations of satellite galaxies in a Lambda-CDM context using the IllustrisTNG suite of cosmological magneto-hydrodynamical simulations. Utilising the entire range of IllustrisTNG allows for an unprecedented combination of statistical sample size and numerical resolution, resulting in mass ranges that cover multiple orders of magnitude for both host and satellites samples, as well as the first statistical sample of 198 high-resolution Milky Way-/Andromeda-like (MW/M31) hosts. I discuss the galaxy-halo connection for satellite and central galaxies across the mass spectrum in the stellar-to-halo mass relation as the most fundamental relationship of galaxy evolution in the cosmological standard model. I analyse the abundance of past and present-day satellite and subhalo populations around MW/M31-like hosts, find a remarkable degree of diversity, and put them into context with both observational surveys and previous simulations of similar systems. Their satellites become increasingly quenched towards smaller stellar masses as they lose their gas reservoirs more easily after infall. Thus, I not only give a detailed view on the evolution of satellite galaxies after infall and the environmental effects they experience but overcome one of the remaining challenges to the Lambda-CDM model: there is no missing satellites problem according to IllustrisTNG.

2021-12-03
15:00
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TBD
Sara Rezaei Kh. (MPIA)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2021-12-03
15:00
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3D structures of the local molecular clouds and their implications for star formation
Sara Rezaei Kh. (MPIA)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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The unprecedented astrometry from the Gaia mission has opened a new door to studying the solar neighbourhood in great detail. In order to get the wealth of information in this data, we have developed a state-of-the-art, three-dimensional dust mapping technique using Gaussian process, that provides detailed 3D maps of the Milky Way. We obtain the 3D positions of stars from Gaia, and their individual extinction using multi-band photometry, which are then used as the input for our model. Taking into account both distance and extinction uncertainties, together with the 3D spatial correlation between neighbouring points, we produce 3D maps of the local molecular clouds, revealing the 3D structures of individual clouds in fine detail.
In this talk, I will start by introducing dust and why it is an important component of the interstellar medium, followed by some of the most recent literature works in the field. Then I will introduce you to our Gaussian-process-based technique and its application to mapping the star-forming regions in the Milky Way. I will finish by showing some of our latest results on the important role of the 3D shape in star formation properties of the molecular clouds.

2021-12-07
16:00
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Ten months of Perseverance on Mars
Prof. Kenneth Farley (California Institute of Technology & Jet Propulsion Laboratory, USA)
Heidelberg Joint Astronomical Colloquium ( Home pageHephysto link )
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The Perseverance rover landed on Mars on February 18, 2021 on the floor of a crater that held a deep lake about 3.5 billion years ago. The mission's goals are to interpret the rocks deposited on the crater floor, seek evidence of possible ancient life recorded in those rocks, and prepare a collection of rock samples for possible return to Earth by future missions. I am Project Scientist for the mission, and in this talk I'll explain this mission's motivations, activities, and discoveries in its first nine months.

2021-12-09
11:15
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An update of the Milky Way disk model and its application: Age-metallicity relation from 4 to 14 kpc based on the JJ model and APOGEE data
Kseniia Sysoliatina (ARI)
ARI Institute Colloquium ( Hephysto link )
ARI, Moenchhofstrasse 12-14, Seminarraum 1, 1.OG
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The semi-analytic Just-Jahreiss (JJ) model of the Galactic disk has been recently calibrated by us in the Solar neighborhood against the Gaia DR2 stars. We identified two star formation (SF) bursts that happened during the recent 4 Gyr. Now we present a global version of the JJ model applicable to a wide range of Galactocentric distances. This generalized JJ model includes exponential thin and thick disk and also atomic and molecular gas layers, as well as the flattened stellar halo and DM halo in the form of a cored isothermal sphere. The overall thickness of the thin disk is assumed constant at all radii, but flaring can be also modeled. The radial variation of the thin-disk star formation rate (SFR) reflects the expected inside-out disk growth scenario. Motivated by our findings for the Solar neighborhood, we allow the smooth power-law SFR to be modified by an arbitrary number of additional Gaussian peaks. Also, the vertical kinematics of the stellar populations associated with these episodes of the SF excess can differ from the kinematics prescribed by the age-velocity dispersion relation for the thin-disk populations of the same age. Using the observed metallicity distributions of the APOGEE Red Clump giants, we constrained the thin- and thick-disk age-metallicity relation for the distances 4 - 14 kpc. The public code of the JJ model is complemented by the two sets of isochrones, PARSEC and MIST. The generalized JJ model is a new stellar population synthesis tool that can be useful for a variety of tasks of Galactic archaeology, including the reconstruction of the Milky-Way disk formation history.

2021-12-10
15:00
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TBD
Heidelberg-Harvard participant (?)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2021-12-10
15:00
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Heidelberg-Harvard participant (?)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2021-12-10
15:00
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Finding Relativistic Stellar Explosions Using Optical Time-Domain Surveys
Anna Ho (UCB)
Königstuhl Kolloquium ( Home pageHephysto link )
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Decades of observations of long-duration gamma-ray bursts (GRBs), attributed to relativistic jets launched in the collapse of massive stars, have yielded important insights on massive-star evolution, compact-object formation, and the physics of relativistic outflows. A major outstanding mystery is whether GRBs---occurring at only 0.1% of the supernova rate---simply represent the tip of the iceberg in a vast landscape of phenomena. To answer this question, with the Zwicky Transient Facility (ZTF) we are conducting a systematic exploration of the rest of the iceberg via searches for fast (hour to day) optical transients. In the past few years our searches yielded several orphan afterglows (afterglows without detected GRBs) at cosmological distances, supernovae with luminous X-ray and radio emission, and mildly relativistic explosions in dense circumstellar matter. Understanding the origin of these events and their relation to GRBs will require coordinated observations between high-cadence optical surveys, wide-field X-ray monitors, and millimeter and radio observatories. This will be possible in the next few years with the launch of the Space-based multi-band astronomical Variable Objects Monitor (SVOM), the enhanced cadence of ZTF Phase II, and sensitive millimeter-band facilities like the Atacama Large Millimeter Array (ALMA).

2021-12-14
16:00
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Weaving the Milky Way tapestry
Dr. Ana Bonaca (Carnegie Observatories, USA)
Heidelberg Joint Astronomical Colloquium ( Home pageHephysto link )
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2021-12-16
11:15
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The cloud-scale baryon cycle across the nearby galaxy population
Melanie Chevance (ARI)
ARI Institute Colloquium ( Hephysto link )
ARI, Moenchhofstrasse 12-14, Seminarraum 1, 1.OG
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The cycling of matter in galaxies between molecular clouds, stars and feedback is a major driverof galaxy evolution. However, it remains a major challenge to derive a theory of how galaxies turn their gasinto stars and how stellar feedback affects the subsequent star formation on the cloud scale, as a functionof the galactic environment. Star formation in galaxies is expected to be highly dependent on the galacticstructure and dynamics, because it results from a competition between mechanisms such as gravitationalcollapse, shear, spiral arm passages, cloud-cloud collisions, and feedback processes such as supernovae, stellarwinds, photoionization and radiation pressure. A statistically representative sample of galaxies is thereforeneeded to probe the wide range of conditions under which stars form. I will present the first systematiccharacterisation of the evolutionary timeline of the giant molecular cloud (GMC) lifecycle, star-formation andfeedback in the PHANGS sample of star-forming disc galaxies. I will show that GMC are short-lived (10-30Myr) and are dispersed after about one dynamical timescale by stellar feedback, between 1 and 5 Myr aftermassive stars emerge. Although the coupling efficiency of early feedback mechanisms such as photoionisationand stellar winds is limited to a few tens of percent, it is sufficient to disperse the parent molecular cloudprior to supernova explosions. This limits the integrated star formation efficiencies of GMCs to 2 to 10 percent. These findings reveal that star formation in galaxies is fast and inefficient, and is governed by cloud-scale, environmentally-dependent, dynamical processes. These measurements constitute a fundamental testfor numerical sub-grid recipes of star-formation and feedback in simulations of galaxy formation and evolution.

2021-12-17
15:00
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TBD
Leonardo Testi (ESO)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2021-12-17
15:00
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Leonardo Testi (ESO)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2021-12-21
16:00
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The assembly history and evolution of the Milky Way as seen through the lens of asteroseismic ages
Prof. Andrea Miglio
Heidelberg Joint Astronomical Colloquium ( Home pageHephysto link )
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2022-01-11
16:00
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Stellar Interactions & Transients
Prof. Silvia Toonen (University of Amsterdam)
Heidelberg Joint Astronomical Colloquium ( Home pageHephysto link )
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The advent and development of large-scale time domain surveys are revealing the existence of a large and diverse zoo of transients; common transients that can be used as tools to constrain GR or cosmological parameters, and rare & exotic transients that are observed for the first time. The origin of the transients is often unknown, but linked to stellar systems and interactions. In this talk I will show novel channels to induce stellar interactions and subsequent transients -in electromagnetic radiation as well as gravitational waves, ranging from stellar mergers to gravitational wave sources. Amongst others I will discuss the potential of triple stars as GW progenitors: while triple star systems are common (even more common than binaries for massive stars!), our understanding of their evolution has lagged behind compared to single and binary stars. Prof. Toonen will be hosted by Fabian Schneider (fabian.schneider@h-its.org)

2022-01-13
11:15
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More than a million stars - past, present, and future of direct N-body simulations
Rainer Spurzem (ARI)
ARI Institute Colloquium ( Hephysto link )
ARI, Moenchhofstrasse 12-14, Seminarraum 1, 1.OG
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Direct N-body computer simulations of the evolution of star clusters take into account all necessary - strong and soft - gravitational encounters between stars in the system. Since the times of von Hoerner and Wielen the ARI has been a place of cutting edge research in this topic. After a brief historic introduction I will introduce the current state of direct N-body simulation at the example of our mostly used code NBODY6++GPU, which is a research instrument having for our team the similar role as an observing instrument. Since a full simulation of a globular cluster over its lifetime of 12 billion years takes as many floating operations as the largest cosmological N-body runs, this is also partly a story of development of supercomputers and general purpose computing on graphics cards (GPU). The current record are models of star clusters with one million bodies (DRAGON simulations). Ideas are discussed how we will proceed in the future and why we need even more particles, e.g. to do proper modeling of nuclear star clusters. Depending on time one or two fields of current applications, done within our local and international team, will be shown and discussed: (i) evolution of black holes, their relativistic dynamics, and (ii) bound and free-floating planets in star clusters.

2022-01-18
16:00
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Title to be announced
Prof. Roger Blandford (Stanford University, USA)
Heidelberg Joint Astronomical Colloquium ( Home pageHephysto link )
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2022-01-20
11:15
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Can velocity fields explain the Wolf-Rayet radius problem?
Roel Lefever (ARI)
ARI Institute Colloquium ( Hephysto link )
ARI, Moenchhofstrasse 12-14, Seminarraum 1, 1.OG
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Massive stars play a dominant role in the energetics of their host galaxies, primarily by their radiation-driven winds enriching their local stellar environments and by ionizing radiation. A subset of the massive stars, the Wolf-Rayet stars, which are direct progenitors of stellar-mass black holes, have particularly strong stellar winds. These winds are so powerful that they effectively push away the outer layers of the Wolf-Rayet star, obscuring it from sight. Hence, only the stellar wind can be observed from Earth. To infer stellar parameters, one needs to rely on a proper modelling of the winds of these stars. In this talk, I will show the deficiencies of the current wind modelling for Wolf-Rayet stars along with accompanying uncertainties on stellar parameters with solutions to construct more accurate models.

2022-01-21
11:00
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TBD
Sascha Quanz (ETH)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-01-21
15:00
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Sascha Quanz (ETH)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-01-21
15:00
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Sascha Quanz (ETH)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-01-25
16:00
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Stellar feedback: from stars to galaxies, and back again
Dr. Anna McLeod (University of Durham, UK)
Heidelberg Joint Astronomical Colloquium ( Home pageHephysto link )
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2022-01-27
11:15
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The tale of the long uphill struggle of GBOT
Martin Altmann (ARI)
ARI Institute Colloquium ( Hephysto link )
ARI, Moenchhofstrasse 12-14, Seminarraum 1, 1.OG
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The highly praised ESA Gaia satellite mission has already provided the astronomic communitywith high quality astrometric, photometric and other data for almost 2 billion stars, and will continue to do sofor the next years. As time goes by, the precision of the astrometry increases with the number of measurementsand the time-span during which these are obtained, growing. Thus the correction of systematic effects in thedata, such as aberration need to be corrected to a point, where the conventional means do not suffice anymore.To accomplish this, a programme was conceived, to track the satellite with highly precise (20 mas) groundbased astrometry to deliver the required data for the optimisation of Gaia’s accuracy, called Ground BasedOptical Tracking (GBOT). This programme has faced many challenges and uncertainties, as well as set backs,but finally GBOT has come to the point, where its data are being included in the processing of the Gaiaastrometry, since 2020.This presentation will give an overview of the history of GBOT, and the steps taken to ensure final success,after many years of challenges. I will also report on a project searching for asteroids on the existing GBOTdata, which has lead to observations of about 42,000 objects, of which about 18,000 were previously unknown.

2022-01-28
11:00
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Jan-Torge Schindler (Leiden Obs./MPIA)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-01-28
15:00
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Jan-Torge Schindler (Leiden Observatory)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-01-28
15:00
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Jan-Torge Schindler (Leiden Obs./MPIA)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-01-28
15:00
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Jan-Torge Schindler (Leiden Obs./MPIA)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-02-01
16:00
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Unveiling the early stages of planet formation
Dr. Myriam Benisty (Institute for Planetary sciences and Astrophysics, Grenoble, France)
Heidelberg Joint Astronomical Colloquium ( Home pageHephysto link )
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2022-02-03
11:15
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Dust Traffic Jams in Inclined Circumbinary Protoplanetary Discs
Hossam Aly (ARI)
ARI Institute Colloquium ( Hephysto link )
ARI, Moenchhofstrasse 12-14, Seminarraum 1, 1.OG
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Gas and dust in inclined orbits around binaries experience precession induced by the binary gravitational torque. The difference in precession between gas and dust alters the radial drift of weakly coupled dust and leads to the formation of dust traffic jams where the radial drift is minimised. I explore this new phenomenon using 3D SPH simulations and investigate its dependence on disc initial inclination and binary eccentricity. I will then present a new dust evolution model that takes the mutual gas and dust inclination into account and reproduce the SPH results, which provides a straightforward way to understanding dust traffic jams as a consequence of the drag torque exerted by the gas on the dust. Finally, I will present the results of radiative transfer post-processing of the hydro simulations and discuss possible observational implications of these dust traffic jams.

2022-02-04
15:00
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Ugne Dudzeviciute (MPIA)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)

2022-02-04
15:00
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Ugne Dudzeviciute (MPIA)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)

2022-02-08
16:00
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Barred galaxies in LambdaCDM: Deciphering the formation history and dark matter content of Milky Way-type galaxies
Dr. Francesca Fragkoudi (European Southern Observatory)
Heidelberg Joint Astronomical Colloquium ( Home pageHephysto link )
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2022-02-10
11:15
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Environmental dependence of the matter cycle from cloud evolution to star formation and feedback in 54 main sequence galaxies
Jaeyeon Kim (ARI)
ARI Institute Colloquium ( Hephysto link )
ARI, Moenchhofstrasse 12-14, Seminarraum 1, 1.OG
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The processes of star formation and feedback take place on the cloud scale (~100pc) within galaxies and play a major role in governing galaxy evolution. The properties of the clouds in which stars form are set by the large scale environment of their host galaxies, directly linking the initial conditions of star formation to galactic-scale properties. In turn, the energy, momentum,and mass deposited by stellar feedback drive the continuous evolution of the interstellar medium at large. Characterising the physical mechanisms regulating this multi-scale cycle is therefore crucial to understand the evolution of galaxies. By applying a new statistical method to the high-resolution CO and narrowband-Halpha imaging from the PHANGS survey, we systematically measure the evolutionary timeline from molecular clouds to exposed young stellar regions on the scales of giant molecular clouds across an unprecedented sample of 54 main sequence galaxies. We find that clouds live for about one dynamical time (8-30 Myr) and are efficiently dispersed by stellar feedback within 1.2-5.1 Myr after the star-forming region has become partially exposed. These ranges do not indicate uncertainties, but reflect physical galaxy-to-galaxy variation, implying an important dependence of these timescales on the local conditions, shaped by the galactic environment. The statistically representative PHANGS sample covers a large range of galaxy properties and morphologies, which allows us, for the first time, to quantitatively link galactic-scale environmental properties to the small-scale evolutionary cycle of molecular clouds, star-formation, and feedback. I will present the first census of these multi-scale trends. These results enable the characterisation of the physical mechanisms regulating cloud assembly, star formation, and cloud disruption, which eventually participate in driving galaxy evolution, as a function of the galactic environment.

2022-02-11
11:00
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Stefan Kraus (University of Exeter)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-02-11
15:00
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Stefan Kraus (University of Exeter)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-02-11
15:00
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Stefan Kraus (University of Exeter)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-02-15
16:00
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The Physics and Astrophysics of Extreme Particle Accelerators
Prof. Felix Aharonian (Max-Planck-Institut fuer Kernphysik, Heidelberg and Dublin Institute for Advanced Studies)
Heidelberg Joint Astronomical Colloquium ( Home pageHephysto link )
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2022-02-17
11:15
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B Supergiants: Atmospheres and Physical Properties
Matheus Bernini Peron (ARI)
ARI Institute Colloquium ( Hephysto link )
ARI, Moenchhofstrasse 12-14, Seminarraum 1, 1.OG
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High-mass stars are very important to many areas of Astronomy. These objects deeply impact their surroundings through their powerful winds and their deaths as supernovae. Therefore,understanding the behavior of such stars is essential to understand their impacts on their hostgalaxies' properties and history.The aim of this research project is to analyze the atmospheres of B supergiants (BSGs, evolvedmassive stars) using the CMFGEN (Hillier & Miller 1998), a 1D, non-LTE atmosphere code — which is one of the state-of-the art tools used to analyze hot stars. The focus of the project is to investigate whether more recent models (e.g., the inclusion of x-rays, clumping, more recent atomic data) can better explain the optical and UV observed spectra of these stars, since previous studies failed to model several important UV lines (Crowther et al. 2006; Searle et al. 2008).As results we obtained (i) an overall improved agreement between BSGs observed and model spectra at the UV considering the effects of clumping and x-rays in the wind. Also we noticed (ii)important differences in their properties between hot (B1 – B0) and warm (B2 - B5) BSGs were also found, and it is in agreement with recent hydrodynamical simulations, such as Driessen et al.(2019). Beyond that, (iii), we have found a general trend of the CNO abundances for BSGs compatible with previous works in the literature and to the current high-mass stellar evolutionpredictions. However, (iv) despite a decrease in terminal velocity at the Bi-Stability Jump, we found no increase in mass-loss, instead, we have found a slightly decreasing trend towards later spectral types.

2022-06-03
11:00
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Ilaria Pascucci (LPL, Tuscon)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-06-03
11:00
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Ilaria Pascucci (LPL, Tuscon)
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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2022-11-25
11:00
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Award celebration
Patzer colloquium
Königstuhl Kolloquium ( Home pageHephysto link )
Max-Planck-Institut für Astronomie, Level 3 Lecture Hall (301)
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The award winner will present their work.

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