BEGIN:VCALENDAR VERSION:2.0 PRODID:-//https://astronomia.uc.cl/2jucext1/institutoastrofisica///NONSGML kigkonsult.se iCalcreator 2.10.15// METHOD:PUBLISH BEGIN:VEVENT UID:20260518T143716-04-8559xUF2Um@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:Dynamics of Distant Milky Way Satellites: Orbital and Internal Evolution\nMatias Blaña\nMax Planck Institute for extraterrestrial Physics (MPE) and at the Munich University Observatory (USM).\n \;\nDetermini ng the orbital history of satellite galaxies in observed galaxy clusters a nd groups is fundamental to disentangle the environmental and the internal processes that shape galaxies. Here\, I present our orbital study of a sa mple of Milky Way satellites located beyond the virial radius of the Milky Way using our new semi-analytical orbital code Delorean\, and tested with full N-body simulations. We find that Phoenix is on its first infall\, wh ile Leo T\, Eridanus II and Cetus also agree with backsplash solutions\, i .e. satellites that could have entered and left the Milky Way halo in the past\, being now on their second infall (Blana et al 2020). Furthermore\, we now use this orbital information to constrain our new hydro-dynamical w ind tunnel simulations with Ramses to study in detail the process of ram p ressure gas stripping and quenching in dwarf galaxy satellites\, comparing with the HI observations of Leo T and Phoenix. https://astronomia.uc.cl/2 jucext1/institutoastrofisica/es/instituto/seminarios/evento/461-dynamics-o f-distant-milky-way-satellites-orbital-and-internal-evolution-matias-blana DTSTART:20201103T143000Z DTEND:20201103T150000Z LOCATION:Santiago Chile () SUMMARY: Dynamics of Distant Milky Way Satellites: Orbital and Internal Evo lution - Matias Blaña URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/461-dynamics-of-distant-milky-way-satellites-orbital-and-in ternal-evolution-matias-blana END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-85812RSx37@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:\n\n\n\nHow tidal forces &\; rotation show up on the “Hybrid ” pulsation of binary systems with intermediate-mass A/F-type companions\n Anya Samadi Ghadim \;\nUniversidad Diego Portales\n \;\nAsteroseis mology is a formidable tool in astrophysics\, which allows us to investiga te the interior structure of stars based on phenomena observed at their su rface. This knowledge is essential for a detailed understanding of both st ellar structure and stellar evolution. ? Dor/? Scuti variables\, two subgr oups of classical A/F-type pulsators\, are intriguing objects with regard to their stellar interior. They are located at the cross-section of the Ce pheid instability strip and the main sequence. “Hybrid” stars have both de tectable ? Dor (g modes) and detectable ? Scuti (p modes) pulsations in th eir Fourier spectrum. \; \;Pulsation study of these stars delivers very impressive information like the interior rotation rates and stratifi cation properties of stars\, only based on unprecedented light curves from space missions like Kepler (K2) and TESS. We expect that a significant fr action of the ? Dor/? Scuti stars resides in binary or multiple systems (M F ? 50%s). The detection of pulsations in binary systems not only provides an additional tool to derive stellar parameters in an independent way but is also the perfect laboratory to check the influence of binarity (e.g. e ccentricity\, tidal effects\, mass transfer\, chemical peculiarities\, pre sence of a third body on stellar structure\, stellar evolution and the exc ited oscillation modes. \;\n\n\n\n\n \;\n\n \;\n https://astro nomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/seminarios/evento/4 63-nuevo-eventohow-tidal-forces-rotation-show-up-on-the-hybrid-pulsation-o f-binary-systems-with-intermediate-mass-a-f-type-companions-anya-samadi-gh adim DTSTART:20200916T040000Z LOCATION:Santiago Chile () SUMMARY:Nuevo eventoHow tidal forces & rotation show up on the “Hybrid” pul sation of binary systems with intermediate-mass A/F-type companions - An ya Samadi Ghadim URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/463-nuevo-eventohow-tidal-forces-rotation-show-up-on-the-hy brid-pulsation-of-binary-systems-with-intermediate-mass-a-f-type-companion s-anya-samadi-ghadim END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-86056bJZIR@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:Currently\, there are approximately 20 circumbinary planetary s ystem detected. Most of them have only one single planet. Binary systems a re great scenarios to test planet formation theories and to study the evol ution of the planets\, because the presence of the secondary companion inc rease the dynamic complexity. Several authors showed that planets can not be formed close to the binary star system because the relative velocities of the planetesimals\, precursors of future planets\, are high enough to c ause erosion\, fragmentation\, etc\, between them. Hydrodynamic simulation s suggest that planets could have formed at farther distances\, and in its interaction with the gas the planet migrates to the inner edge of the dis k (Pierens &\; Nelson 2007\, 2008\, Kley &\; Haguiguipour 2014\, 201 5). In the presence of two planets in interaction with the gas disk\, reso nance captures between the planets may occur depending on the considered p lanetary mass configuration of the system\, leading\, in some cases\, to t he ejection of one of the planets (Pierens &\; Nelson 2007).\nThe main objective of my PhD project is to study the dynamical evolution of planets in several resonances around binary star systems after the dissipation of the gas. In this presentation I will present the state of the art\, some results obtained so far and the next steps of the project. https://astrono mia.uc.cl/2jucext1/institutoastrofisica/es/instituto/seminarios/evento/399 -instability-in-resonant-planets-around-circumbinary-stars-matias-garcia-o bservatorio-nacional-rio-de-janeiro-brasil DTSTART:20191127T161500Z DTEND:20191127T164500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:Instability in resonant planets around circumbinary stars (Matias G arcia\; Observatório Nacional\, Rio de Janeiro\, Brasil) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/399-instability-in-resonant-planets-around-circumbinary-sta rs-matias-garcia-observatorio-nacional-rio-de-janeiro-brasil END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8628sDg2zu@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:{slider Slider Title 1}\nYour text...\n\n{slider Slider Title 2 }\n\nYour text...\n\n{/sliders}\nWe still have a considerable lack of unde rstanding about the constituents of our Universe\, and tensions are starti ng to arise between datasets as we reach subpercent precision constraints.  \; \;In this talk\, I will mention how we can use gravitational w aves as a new independent tool to learn about cosmology. I will discuss ho w we can set constraints on the current expansion rate of the Universe\,&n bsp\;H0\, \;as well as test the nature of dark energy with the observa tion of binary neutron star mergers. https://astronomia.uc.cl/2jucext1/ins titutoastrofisica/es/instituto/seminarios/evento/397-cosmology-in-the-mult i-messenger-era-dr-macarena-lagos-university-of-chicago DTSTART:20191125T161500Z DTEND:20191125T164500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY: Cosmology in the multi-messenger era (Dr. Macarena Lagos\; Univers ity of Chicago) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/397-cosmology-in-the-multi-messenger-era-dr-macarena-lagos- university-of-chicago END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8645aF5SvK@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:Last decade is a period of an extensive development of all-sky surveys\, which reveal discovery of new types of transients such as Super Luminous Supernovae\, Tidal Disruption Events and other rapidly evolving o bjects. In my talk I will present a brief review of this exciting topic. h ttps://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/seminar ios/evento/369-postponed-new-types-of-transients-in-the-era-of-all-sky-sur veys-dr-mariusz-gromadzki-university-of-warsaw DTSTART:20191120T161500Z DTEND:20191120T164500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:POSTPONED: New types of transients in the era of all-sky surveys (D r. Mariusz Gromadzki\; University of Warsaw) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/369-postponed-new-types-of-transients-in-the-era-of-all-sky -surveys-dr-mariusz-gromadzki-university-of-warsaw END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8659KjBU0u@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:Recent observations of protoplanetary discs have shown clear ev idence of warps and misalignments\, where the disc is best described with an orientation that changes as a function of the distance from the central star. A number of scenarios have been proposed to explain the origins of these misalignments\, including the presence of a hidden companion on an o rbit that is misaligned with respect to the outermost disc. By introducing such a misaligned body we need to consider the potential of disc precessi on\, inclination damping and alignment time-scales. I will show how an und erstanding of these effects can allow us to infer what is happening in the se systems with observed misalignments and the implications for their long term evolution. This tour will include applications to TW Hya (a rapidly moving shadow)\, misalignments induced by a flyby\, HH30 (with a wiggling jet) and HD100453 (with a strongly misaligned inner disc). https://astrono mia.uc.cl/2jucext1/institutoastrofisica/es/instituto/seminarios/evento/365 -canceled-misalignments-precession-and-shadows-in-protoplanetary-discs-dr- rebecca-nealon-university-of-leicester DTSTART:20191113T161500Z DTEND:20191113T164500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:CANCELED: Misalignments\, precession and shadows in protoplanetary discs (Dr. Rebecca Nealon\; University of Leicester) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/365-canceled-misalignments-precession-and-shadows-in-protop lanetary-discs-dr-rebecca-nealon-university-of-leicester END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8679iD9RN2@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:\nAll evolved stars of up to 2 solar masses undergo a helium co re flash at the end of their first stage as a giant star. Although theoret ically predicted more than 50 years ago\, this core flash phase has yet to be observationally probed. We show here that gravity modes stochastically excited by helium-flash-driven convection are able to reach the stellar s urface and induce periodic photometric variabilities in hot subdwarf stars with amplitudes of the order of a few thousandths of a magnitude. As such \, they can now be detected by space-based photometry with the Transiting Exoplanet Survey Satellite in relatively bright stars (for example\, Johns on–Cousins magnitudes of IC???13?mag). The range of predicted periods span s from a few thousand seconds to tens of thousands of seconds\, depending on the details of the excitation region. In addition\, we find that stocha stically excited pulsations reproduce the pulsations observed in a few hel ium-rich hot subdwarf stars. These stars\, particularly the future Transit ing Exoplanet Survey Satellite target Feige 46\, are the most promising ca ndidates to probe the helium core flash for the first time.\n \; https ://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/seminarios/ evento/393-asteroseismic-signatures-of-the-helium-core-flash-dr-marcelo-m- miller-bertolami-instituto-de-astrofisica-de-la-plata-unlp-conicet DTSTART:20191111T161500Z DTEND:20191111T164500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:Asteroseismic signatures of the helium core flash (Dr. Marcelo M. M iller Bertolami\; Instituto de Astrofisica de La Plata -- UNLP-CONICET) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/393-asteroseismic-signatures-of-the-helium-core-flash-dr-ma rcelo-m-miller-bertolami-instituto-de-astrofisica-de-la-plata-unlp-conicet END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-87004Uofwk@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:Up to date more than 4\,000 known exoplanets have been detected . The characterization of their atmospheres is a natural step to learn mor e about their diversity especially from the atmospheres of rocky exoplanet s. They can potentially host bio-signature gases\, notably molecular oxyge n (O2). When observed through transmission spectroscopy\, it is possible t hat the star-planet configuration allows us to sample only low pressure la yers\, and therefore the absorption lines will be very narrow\, and we wil l need extreme high resolution to fully resolve the lines. Higher resoluti on allows us to disentangle actual signal and telluric lines in our own at mosphere. Recent studies show that O2 is best observed from ground with up coming Extremely Large Telescopes. The spectral resolutions of 300\,000 - 400\,000 are optimal to detect O2 in the atmosphere of an earth analog. Ho wever\, typical high-resolution spectrographs have resolutions around 100\ ,000. In order to increase detection capabilities\, we have developed a Fa bry Perot Interferometer for Oxygen Searches (FIOS)\, an interferometer ar ray coupled to a high-resolution spectrograph. FIOS can achieve a spectral resolution of 500\,000 at the O2A-band (760 nm). I will describe the inst rument concept\, a simulation of its sensitivity\, and preliminary results from our lab prototype. https://astronomia.uc.cl/2jucext1/institutoastrof isica/es/instituto/seminarios/evento/395-canceled-the-next-leap-to-charact erize-exoplanet-atmosphere-in-the-elts-era-surangkhana-rukdee-center-for-a strophysics-harvard-smithsonian DTSTART:20191106T161500Z DTEND:20191106T164500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:CANCELED: The next leap to characterize exoplanet atmosphere in the ELTs era (Surangkhana Rukdee\; Center for Astrophysics | Harvard & Smiths onian) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/395-canceled-the-next-leap-to-characterize-exoplanet-atmosp here-in-the-elts-era-surangkhana-rukdee-center-for-astrophysics-harvard-sm ithsonian END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8724CVk9lL@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:In this talk\, I will discuss some aspects of non-linear struct ure formation. The calculation of the bispectrum usually involves linear p hysics on large scales and non-linear (but Newtonian) physics on small sca les. However\, in the squeezed limit\, the bispectrum (unlike the power sp ectrum) couples large scales with small scales. I will present the calcula tion of the non-linear relativistic corrections to the dynamics of dark ma tter perturbations. They are of the same order of magnitude\, in the squee zed limit\, than a primordial local non-Gaussianity signal. Such signal is expected to be within the accuracy of the next generation of LSS surveys. https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/semin arios/evento/367-postponed-relativistic-cosmological-large-scale-structure s-at-one-loop-dr-clement-stahl-pontificia-universidad-catolica-de-valparai so DTSTART:20191028T161500Z DTEND:20191028T164500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:POSTPONED: Relativistic cosmological large scale structures at one- loop (Dr. Clément Stahl\; Pontificia Universidad Católica de Valparaíso) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/367-postponed-relativistic-cosmological-large-scale-structu res-at-one-loop-dr-clement-stahl-pontificia-universidad-catolica-de-valpar aiso END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8742EBisAX@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:Fomalhaut is a nearby stellar system and has been found to be a triple based on astrometric observations. With new radial velocity and as trometric data\, we study the association between Fomalhaut A\, B\, and C in a Bayesian framework\, finding that the system is gravitationally bound or at least associated. Based on simulations of the system\, we find that Fomalhaut C can be easily destabilized through combined perturbations fro m the Galactic tide and stellar encounters. Considering that observing the disruption of a triple is probably rare in the solar neighbourhood\, we c onclude that Fomalhaut C is a so-called ‘gravitational pair’ of Fomalhaut A and B. Like the Cooper pair mechanism in superconductors\, this phenomen on only appears once the orbital energy of a component becomes comparable with the energy fluctuations caused by the environment. Based on our simul ations\, we find (1) an upper limit of 8 km/s velocity difference is appro priate when selecting binary candidates\, and (2) an empirical formula for the escape radius\, which is more appropriate than tidal radius when meas uring the stability of wide binaries. https://astronomia.uc.cl/2jucext1/in stitutoastrofisica/es/instituto/seminarios/evento/361-understanding-fomalh aut-as-a-cooper-pair-dr-fabo-feng-carnegie-department-of-terrestrial-magne tism DTSTART:20190823T171500Z DTEND:20190823T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:Understanding Fomalhaut as a Cooper pair (Dr. Fabo Feng\; Carnegie Department of Terrestrial Magnetism) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/361-understanding-fomalhaut-as-a-cooper-pair-dr-fabo-feng-c arnegie-department-of-terrestrial-magnetism END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8762PWpKnl@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:Nuclear star clusters (NSCs) are found in at least 70% of all g alaxies\; however\, despite their abundance it is still debated how they f orm. The currently discussed scenarios propose that NSCs could either form from infalling gas directly at the galactic center or through the accreti on of globular clusters (GCs) that spiral inwards due to dynamical frictio n\, but also a composite scenario is possible. In the GC accretion scenari o\, the NSC would reflect the low angular momentum and low metallicities o f the surrounding GC population\, whereas the in-situ scenario would lead to a higher angular momentum and higher metallicities from subsequent star bursts.\nConstraining NSC formation in galaxies therefore requires a comp lete view of both the kinematics and chemical properties of the host galax y\, the NSC and the GC system. To achieve this task\, we use IFU data from the MUSE instrument of the early-type galaxy FCC47\, which has a remarkab ly large NSC (Reff ~ 66 pc) and a very rich GC system.\nIn addition to an analysis of the galaxy light kinematics and stellar population properties\ , we extract optical spectra of the GCs to determine radial velocities and metallicities. In combination with a dynamical model\, our panoramic view of the galaxy and its star clusters allows to put constraints on the form ation of FCC47’s massive NSC. https://astronomia.uc.cl/2jucext1/institutoa strofisica/es/instituto/seminarios/evento/363-constraining-the-formation-o f-the-large-nuclear-star-cluster-of-fcc47-with-muse-ao-katja-fahrion-europ ean-southern-observatory-garching DTSTART:20190821T171500Z DTEND:20190821T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:Constraining the formation of the large Nuclear Star Cluster of FCC 47 with MUSE + AO (Katja Fahrion\; European Southern Observatory\, Garchin g) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/363-constraining-the-formation-of-the-large-nuclear-star-cl uster-of-fcc47-with-muse-ao-katja-fahrion-european-southern-observatory-ga rching END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8785lWD9Wl@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:As a veteran of 34 total solar eclipses and 70 solar eclipses i n all\, I will summarize our recent scientific work at eclipses. We have h igh resolution images\, comparison of images with theoretical predictions based on magnetic-field measurements\, emission spectra of high ionization lines\, and radio observations. As chair of the working group on solar ec lipses of the International Astronomical Union\, I will describe internati onal coordination.\nPrevious eclipses that I observed from Chile include t he 1994 totality from the mountains above Arica\, at which we worked with University of Chile professor Hector Alvarez\, and the 2010 eclipse from E aster Island. I will describe our plans for the forthcoming eclipse\, for which I just received a research grant from the US National Science Founda tion\, and for eclipses thereafter. On July 2\, I will have one group of r esearchers and students observing from the centerline north of La Serena\, and four of our team observing from the Cerro Tololo Inter-American Obser vatory\, as well as related instrumentation on a plane flying out of Easte r Island. https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instit uto/seminarios/evento/359-this-solar-eclipse-and-others-science-and-specta cle-prof-jay-pasachoff-williams-college-williamstown-massachusetts-usa DTSTART:20190627T171500Z DTEND:20190627T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:This Solar Eclipse\, and Others: Science and Spectacle (Prof. Jay P asachoff\; Williams College\, Williamstown\, Massachusetts\, USA) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/359-this-solar-eclipse-and-others-science-and-spectacle-pro f-jay-pasachoff-williams-college-williamstown-massachusetts-usa END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8806wctnpa@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:It is well known that when a fluid is thermally unstable\, conv ection can be the most efficient mechanism for mixing and energy transport . However\, the presence of a stable composition gradient can counteract a nd inhibit convection\, giving rise to an interesting phenomenon called do uble-diffusive convection - or semi-convection - which is characterized by layers of convective and diffusive zones. In this seminar\, I will discus s some of the main properties of semi-convection and its relevance to gas giant planets. Finally\, I will show 2D hydrodynamical simulations of this process. https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instit uto/seminarios/evento/357-hydrodynamics-of-double-diffusive-convection-jos e-rafael-fuentes-mcgill-university DTSTART:20190621T171500Z DTEND:20190621T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:Hydrodynamics of double-diffusive convection (José Rafael Fuentes\; McGill University) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/357-hydrodynamics-of-double-diffusive-convection-jose-rafae l-fuentes-mcgill-university END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8822p3bIvf@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:The study of Planetary Nebulae (PNe) provides vital clues for u nderstanding late stage stellar evolution and stellar mass loss. Despite t heir significance\, various issues concerning these objects remain unsolve d. Interstellar extinction by dust hampers the detection of many Galactic PNe at optical wavelengths while their largely unknown distances and proge nitor masses are two key parameters that hamper deeper understanding.  \; Identification of dust obscured PNe can be partially solved with observ ations at longer wavelengths where extinction effects are less serious and by multi-wavelength techniques proposed for their detection. Here\, the e fficacy of these methods is evaluated for identification of new Galactic P N candidates. \; PNe in Galactic star clusters have distances and prog enitor masses determined independently from cluster color-magnitude diagra ms. Here\, we study the first confirmed PN-open cluster pair (PHR1315-6555 – AL 1) identifying its central star and measuring its physical propertie s. We also demonstrate in detail the physical association of PN BMP J1613- 5406 with Galactic open cluster NGC 6067. The PN’s progenitor mass is ~5.6 Msun. Finally\, we provide preliminary details on several additional case s of possible PN-cluster associations we have uncovered. Our new PN-open c luster associations contribute to the improvement of the initial-to-final mass relation and our multi-wavelength study suggests that a new era begin s for the identification of Galactic PNe hidden by dust. https://astronomi a.uc.cl/2jucext1/institutoastrofisica/es/instituto/seminarios/evento/355-g alactic-planetary-nebulae-with-emphasis-on-those-that-are-members-of-open- star-clusters-vasiliki-fragkou-university-of-hong-kong DTSTART:20190606T171500Z DTEND:20190606T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:Galactic Planetary Nebulae with Emphasis on those that are Members of Open Star Clusters (Vasiliki Fragkou\; University of Hong Kong) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/355-galactic-planetary-nebulae-with-emphasis-on-those-that- are-members-of-open-star-clusters-vasiliki-fragkou-university-of-hong-kong END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8844iN1D2f@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:I will talk about the work done during my PhD. This was centere d on the accretion into compact object inside the framework of the induced gravitational collapse (IGC) scenario\, proposed to explain the origin fo r the long-duration gamma-ray burst (GRBs) associated with supernovae type Ic. \; In this one\, a carbon-oxygen core explodes in a Type Ib/c SN in presence of a close neutron star (NS) companion. The SN \; triggers an hypercritical accretion into the NS and if the accretion rate is enoug h high\, the NS can reach its critical mass\, and collapses to a black hol e (BH)\, emitting a GRB . Otherwise\, the system gives place to a x-ray fl ash (XRF). \; With the aim to identify the separatrix of systems in wh ich a BH is formed and characterize the observational signatures of each p rocess\, it was formulated an analytical model based in the Bondy-Hoyle ac cretion formalism. We also performed 3D-SPH numerical simulations of the S N expansion under the presence of the NS companion and explored a wide ran ge of the initial parameter space. https://astronomia.uc.cl/2jucext1/insti tutoastrofisica/es/instituto/seminarios/evento/353-accretion-onto-compact- objects-in-the-induced-gravitational-collapse-scenario-dr-laura-becerra-pu c DTSTART:20190529T171500Z DTEND:20190529T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:Accretion onto compact objects in the induced gravitational collaps e scenario (Dr. Laura Becerra\; PUC) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/353-accretion-onto-compact-objects-in-the-induced-gravitati onal-collapse-scenario-dr-laura-becerra-puc END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8862s2Ozv1@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:The Southern Photometric Local Universe Survey (S-PLUS) is a Br azilian-led project that comprises imaging 9300 square degrees of the cele stial sphere in twelve optical bands using a dedicated 0.8m robotic telesc ope\, T80-South\, at Cerro Tololo\, Chile. \; The telescope is equippe d with a large-format camera\, with a field-of-view of 2 square degrees\, with a plate scale of 0.55'/pixel. The survey consists of (1) two non-cont iguous fields at high Galactic latitudes\, which together cover an area of 8000 sq. degrees and (2) \; two areas of the Galactic Plane and Bulge (for an additional 1300 square degrees). S-PLUS uses the Javalambre 12-ba nd magnitude system which includes ugriz broad-band filters and 7 narrow-b and filters centred on prominent stellar spectral features: [OII]\, Ca H+K \, Hdelta\, G-band\, Mgb triplet\, Halpha and Ca triplet. The combination of a Wide FoV telescope+camera and choice of filters will allow the study of a large number of scientific topics\, from Solar System to Cosmology. I n particular\, S-PLUS will deliver accurate photo-zs\, providing a map of the local universe. It will also allow the study of star formation and ste llar populations in and around the Milky Way and nearby galaxies and searc h for quasars\, variable sources\, and low-metallicity and carbon-enhanced metal-poor stars. In this talk\, I will present the survey and I will hig hlight its usefulness for different science topics of interest to the comm unity. https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto /seminarios/evento/339-postponed-the-southern-photometric-local-universe-s urvey-s-plus-dr-fabio-herpich-university-of-sao-paulo DTSTART:20190523T171500Z DTEND:20190523T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:POSTPONED: The Southern Photometric Local Universe Survey (S-PLUS) (Dr. Fábio Herpich\; University of Sao Paulo) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/339-postponed-the-southern-photometric-local-universe-surve y-s-plus-dr-fabio-herpich-university-of-sao-paulo END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8884DjnFdg@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:Variability is ubiquitous in active galactic nuclei (AGN) and c an be observed or inferred at all timescales\, from hours to billions of y ears. In this talk I will first illustrate how spatially resolved optical spectroscopy\, combined with high quality X-ray data\, can be used to prob e AGN variability on >\; 10^4 yr timescales. I will then present a compi lation of variability measurements\, covering many orders of magnitude bot h in time lags and variability amplitude\, which provides an overview of t he variabiltiy phenomena. This compilation includes ensemble studies\, whi ch characterise the mean variability among the AGN population\, as well as measurements for single objects such as the changing look AGN\, the Voorw erpjes galaxies\, and our own Sagittarius A*. Finally\, I will present a f ramework which allows us to test if and how variability in different AGN a nd at different timescales can be linked and explained based on the distri bution of the Eddington ratio (ER) among the galaxy population. At the end of the talk I will also discuss possible applications of our model\, e.g. for understanding extreme variable AGN or planning future time domain sur veys such as LSST. https://astronomia.uc.cl/2jucext1/institutoastrofisica/ es/instituto/seminarios/evento/351-a-study-of-active-galactic-nuclei-varia bility-on-multiple-timescales-lia-sartori-eth-zurich DTSTART:20190508T171500Z DTEND:20190508T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:A study of active galactic nuclei variability on multiple timescale s (Lia Sartori\; ETH Zurich) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/351-a-study-of-active-galactic-nuclei-variability-on-multip le-timescales-lia-sartori-eth-zurich END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8904C7e3nU@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:One of the main predictions derived from ?-CDM cosmology is tha t structure grows hierarchically as consequence of the gravity-driven asse mbly of dark matter halos and the galaxies they host\, making galaxy merge rs a fundamental element within the current framework of galaxy evolution. Despite this\, the specific role that galaxy mergers play in the differen t processes observed in galaxy evolution along with the rates that are est imated\, from either observations or simulations\, remain not fully unders tood. In that regard\, the development of accurate methods to detect galax y mergers is something extremely relevant in order to improve our comprehe nsion of the merging process\, but also to bring into agreement galaxy for mation models with the available observational data.\nInspired by the rece nt success of multiple deep learning techniques used to address different astrophysical problems\, we present a novel method based on the utilizatio n of Convolutional Neural Networks (CNNs) and the Horizon-AGN cosmological simulation for identifying galaxy mergers in an automated and accurate ma nner. The main idea behind this method consists on generating large traini ng sets of HST-like multiband mock observations of mergers\, isolated gala xies (no-mergers) and projection effects (fake-mergers) employing as input the virtual galaxies of the Horizon-AGN simulation\, which then are used to train a CNN that is able of identifying galaxy mergers. These mock obse rvations are generated considering massive galaxies (M_star <\;= 10^10 M _sun) in the redshift range 0.5 <\; z <\; 3.5\, and in the case of gal axy mergers\, only those that correspond to major ones (stellar mass ratio <\;= 1:4) are taken into account.\nThe performance exhibited by this ne w method outperforms not only the classic approaches based on non-parametr ic morphologies employed for identifying galaxy mergers\, such as CAS and G-M20\, but also the extended and improved versions of these methods that rely on the utilization of machine learning. Moreover\, the use of a simul ated training set allowed us to relate the observability timescales of the different methods analyzed with the actual timescales of the galaxy merge rs selected from the simulation. https://astronomia.uc.cl/2jucext1/institu toastrofisica/es/instituto/seminarios/evento/347-automated-detection-of-ga laxy-mergers-using-cosmological-simulations-and-deep-learning-dr-fernando- caro-lerma-observatoire-de-paris DTSTART:20190401T171500Z DTEND:20190401T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:Automated Detection of Galaxy Mergers using Cosmological Simulation s and Deep Learning (Dr. Fernando Caro\; LERMA\, Observatoire de Paris) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/347-automated-detection-of-galaxy-mergers-using-cosmologica l-simulations-and-deep-learning-dr-fernando-caro-lerma-observatoire-de-par is END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8933uPewA3@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:From June to November of 2018 I did a research internship at th e Institut für Geophysik und extraterrestrische Physik (IGeP) in Braunschw eig (Germany)\, carrying out impact experiments in their laboratories unde r the direction of Dr. Jürgen Blum. The research project consisted of two stages\, the first one was to generate compact dust samples by high speed impacts and the second stage consisted in performing the 'Brazilian Disk T est' with these samples. With the first experiment we calculated the relat ion between the impact velocity and the compaction of the samples and with the second one\, the relation between the tensile strength of the samples and their compaction. The main objective of this work is to find a relati onship between the speed at which the samples were compacted and the energ y that characterizes the collisions to be able to implement it in the futu re to the model of formation of giant planets. https://astronomia.uc.cl/2j ucext1/institutoastrofisica/es/instituto/seminarios/evento/343-laboratory- experience-at-igep-tensile-strength-of-compact-dust-samples-irina-l-san-se bastian-universidad-nacional-de-la-plata DTSTART:20190327T171500Z DTEND:20190327T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:Laboratory experience at IGeP: Tensile strength of compact dust sam ples (Irina L. San Sebastián\; Universidad Nacional de La Plata) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/343-laboratory-experience-at-igep-tensile-strength-of-compa ct-dust-samples-irina-l-san-sebastian-universidad-nacional-de-la-plata END:VEVENT BEGIN:VEVENT UID:20260518T143716-04-8953L5buOn@https://astronomia.uc.cl/2jucext1/institu toastrofisica/ DTSTAMP:20260518T183716Z DESCRIPTION:The first object of unambiguously interstellar origin\, 'Oumuam ua\, passed through the inner Solar System in 2017. The existence of inter stellar objects is an inevitable consequence of planet formation\, but the estimated abundance and individual properties of 'Oumuamua pose many puzz les. I will discuss some of the mysteries\, and the prospects for using mo re such objects as a new probe of planet formation. https://astronomia.uc. cl/2jucext1/institutoastrofisica/es/instituto/seminarios/evento/345-oumuam ua-the-first-interstellar-visitor-prof-phil-armitage-stony-brook-universit y-and-the-flatiron-institute DTSTART:20190322T171500Z DTEND:20190322T174500Z LOCATION:Seminar Room (Instituto de Astrofísica\, Pontificia Universidad Ca tólica\, Vicuña Mackenna 4860\, Santiago\, Chile) SUMMARY:'Oumuamua: The First Interstellar Visitor (Prof. Phil Armitage\; St ony Brook University and the Flatiron Institute) URL:https://astronomia.uc.cl/2jucext1/institutoastrofisica/es/instituto/sem inarios/evento/345-oumuamua-the-first-interstellar-visitor-prof-phil-armit age-stony-brook-university-and-the-flatiron-institute END:VEVENT END:VCALENDAR