BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//Osservatorio Astronomico di Roma - ECPv6.15.18//NONSGML v1.0//EN
CALSCALE:GREGORIAN
METHOD:PUBLISH
X-WR-CALNAME:Osservatorio Astronomico di Roma
X-ORIGINAL-URL:https://www.oa-roma.inaf.it
X-WR-CALDESC:Eventi per Osservatorio Astronomico di Roma
REFRESH-INTERVAL;VALUE=DURATION:PT1H
X-Robots-Tag:noindex
X-PUBLISHED-TTL:PT1H
BEGIN:VTIMEZONE
TZID:Europe/Rome
BEGIN:DAYLIGHT
TZOFFSETFROM:+0100
TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20150329T010000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+0200
TZOFFSETTO:+0100
TZNAME:CET
DTSTART:20151025T010000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+0100
TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20160327T010000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+0200
TZOFFSETTO:+0100
TZNAME:CET
DTSTART:20161030T010000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+0100
TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20170326T010000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+0200
TZOFFSETTO:+0100
TZNAME:CET
DTSTART:20171029T010000
END:STANDARD
END:VTIMEZONE
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161004T114500
DTEND;TZID=Europe/Rome:20161004T120000
DTSTAMP:20260404T192452
CREATED:20160713T095906Z
LAST-MODIFIED:20160713T095906Z
UID:1332-1475581500-1475582400@www.oa-roma.inaf.it
SUMMARY:Cosmic rays\, gamma-rays\, and neutrinos from AGN winds
DESCRIPTION:Galaxy scale outflows driven by active galactic nuclei (AGN) are likely to play a key role in the evolution of galaxies. In fact\, they can perturb and possibly expel most of the gas out of the galaxy\, offering a plausible physical origin for the close connection between the properties of black holes and their host galaxies. AGN-driven outflows can also induce shocks in the interstellar medium\, which\, in turn\, can accelerate relativistic particles.\nI will present a study of the non-thermal emissions produced by relativistic particles accelerated by the AGN-driven shocks in  NGC 1068.  NGC 1068 is a nearby prototypical Seyfert 2 galaxy which shows both starburst and nuclear activities in its central region. NGC 1068 is a strong gamma-ray emitter. It is the brightest of the few non-blazar galaxies  detected by the Fermi gamma-ray space telescope.\nI will show the gamma-ray and radio spectra predicted by the AGN outflow model\, and I will discuss how these results compare with those corresponding to other commonly assumed sources of gamma-ray and radio emissions\, like Supernova remnants or AGN jets.\nI will compare the neutrino flux expected in the AGN outflow model with constraints from current experiments\, and I will provide predictions for the detections by the  upcoming KM3NeT neutrino telescope.
URL:https://www.oa-roma.inaf.it/event/cosmic-rays-gamma-rays-and-neutrinos-from-agn-winds/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161004T114500
DTEND;TZID=Europe/Rome:20161004T120000
DTSTAMP:20260404T192452
CREATED:20160713T095906Z
LAST-MODIFIED:20160713T095906Z
UID:4672-1475581500-1475582400@www.oa-roma.inaf.it
SUMMARY:Cosmic rays\, gamma-rays\, and neutrinos from AGN winds
DESCRIPTION:Galaxy scale outflows driven by active galactic nuclei (AGN) are likely to play a key role in the evolution of galaxies. In fact\, they can perturb and possibly expel most of the gas out of the galaxy\, offering a plausible physical origin for the close connection between the properties of black holes and their host galaxies. AGN-driven outflows can also induce shocks in the interstellar medium\, which\, in turn\, can accelerate relativistic particles.\nI will present a study of the non-thermal emissions produced by relativistic particles accelerated by the AGN-driven shocks in  NGC 1068.  NGC 1068 is a nearby prototypical Seyfert 2 galaxy which shows both starburst and nuclear activities in its central region. NGC 1068 is a strong gamma-ray emitter. It is the brightest of the few non-blazar galaxies  detected by the Fermi gamma-ray space telescope.\nI will show the gamma-ray and radio spectra predicted by the AGN outflow model\, and I will discuss how these results compare with those corresponding to other commonly assumed sources of gamma-ray and radio emissions\, like Supernova remnants or AGN jets.\nI will compare the neutrino flux expected in the AGN outflow model with constraints from current experiments\, and I will provide predictions for the detections by the  upcoming KM3NeT neutrino telescope.
URL:https://www.oa-roma.inaf.it/event/cosmic-rays-gamma-rays-and-neutrinos-from-agn-winds-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160927T114500
DTEND;TZID=Europe/Rome:20160927T124500
DTSTAMP:20260404T192452
CREATED:20160716T141755Z
LAST-MODIFIED:20160716T141755Z
UID:1334-1474976700-1474980300@www.oa-roma.inaf.it
SUMMARY:Indirect Dark Matter searches with the MAGIC telescopes and prospects with the ASTRI mini-array and the Cherenkov Telescope Array
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/indirect-dark-matter-searches-with-the-magic-telescopes-and-prospects-with-the-astri-mini-array-and-the-cherenkov-telescope-array/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160927T114500
DTEND;TZID=Europe/Rome:20160927T124500
DTSTAMP:20260404T192452
CREATED:20160716T141755Z
LAST-MODIFIED:20160716T141755Z
UID:4673-1474976700-1474980300@www.oa-roma.inaf.it
SUMMARY:Indirect Dark Matter searches with the MAGIC telescopes and prospects with the ASTRI mini-array and the Cherenkov Telescope Array
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/indirect-dark-matter-searches-with-the-magic-telescopes-and-prospects-with-the-astri-mini-array-and-the-cherenkov-telescope-array-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160913T114500
DTEND;TZID=Europe/Rome:20160913T124500
DTSTAMP:20260404T192452
CREATED:20160729T105120Z
LAST-MODIFIED:20160729T105120Z
UID:1348-1473767100-1473770700@www.oa-roma.inaf.it
SUMMARY:Gas accretion and star formation in disk galaxies
DESCRIPTION:Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the\nformation of disk galaxies. My presentation will summarize observational evidence\nfor this gas accretion process driving star formation. In particular\, I will discuss\na number of properties characterizing large samples of star-forming galaxies that\ncan be explained by metal-poor gas accretion (e.g.\, the fundamental metallicity relation\,\nor the relationship between galaxy morphology and metallicity). Some properties of the\n(neutral and ionized) gas around galaxies will be examined too. I will also review the\nproperties of the extremely metal poor galaxies. They show chemical and dynamical\ninhomogeneities that can be naturally explained as due to star-formation feeding from\ninfall of external metal-poor gas.
URL:https://www.oa-roma.inaf.it/event/gas-accretion-and-star-formation-in-disk-galaxies/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160913T114500
DTEND;TZID=Europe/Rome:20160913T124500
DTSTAMP:20260404T192452
CREATED:20160729T105120Z
LAST-MODIFIED:20160729T105120Z
UID:4677-1473767100-1473770700@www.oa-roma.inaf.it
SUMMARY:Gas accretion and star formation in disk galaxies
DESCRIPTION:Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the\nformation of disk galaxies. My presentation will summarize observational evidence\nfor this gas accretion process driving star formation. In particular\, I will discuss\na number of properties characterizing large samples of star-forming galaxies that\ncan be explained by metal-poor gas accretion (e.g.\, the fundamental metallicity relation\,\nor the relationship between galaxy morphology and metallicity). Some properties of the\n(neutral and ionized) gas around galaxies will be examined too. I will also review the\nproperties of the extremely metal poor galaxies. They show chemical and dynamical\ninhomogeneities that can be naturally explained as due to star-formation feeding from\ninfall of external metal-poor gas.
URL:https://www.oa-roma.inaf.it/event/gas-accretion-and-star-formation-in-disk-galaxies-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160630T114500
DTEND;TZID=Europe/Rome:20160630T124500
DTSTAMP:20260404T192452
CREATED:20160425T070945Z
LAST-MODIFIED:20160425T070945Z
UID:1123-1467287100-1467290700@www.oa-roma.inaf.it
SUMMARY:The Milky Way bulge: chemical content\, kinematics and 3D structure
DESCRIPTION:During the last decade large observational efforts have been focused on understanding the formation and evolution of the Milky Way bulge by studying the spectroscopic and photometric properties of its stellar population over large and unexplored regions.\nThe emerging picture is substantially different from what previously thought and by far more complicated.\nI will review the results obtained by the recent surveys focusing in particular on the observational evidences concerning the Bulge chemical content\, kinematics and 3D structure.
URL:https://www.oa-roma.inaf.it/event/the-milky-way-bulge-chemical-content-kinematics-and-3d-structure/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160630T114500
DTEND;TZID=Europe/Rome:20160630T124500
DTSTAMP:20260404T192452
CREATED:20160425T070945Z
LAST-MODIFIED:20160425T070945Z
UID:4667-1467287100-1467290700@www.oa-roma.inaf.it
SUMMARY:The Milky Way bulge: chemical content\, kinematics and 3D structure
DESCRIPTION:During the last decade large observational efforts have been focused on understanding the formation and evolution of the Milky Way bulge by studying the spectroscopic and photometric properties of its stellar population over large and unexplored regions.\nThe emerging picture is substantially different from what previously thought and by far more complicated.\nI will review the results obtained by the recent surveys focusing in particular on the observational evidences concerning the Bulge chemical content\, kinematics and 3D structure.
URL:https://www.oa-roma.inaf.it/event/the-milky-way-bulge-chemical-content-kinematics-and-3d-structure-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160614T114500
DTEND;TZID=Europe/Rome:20160614T124500
DTSTAMP:20260404T192452
CREATED:20160425T071635Z
LAST-MODIFIED:20160425T071635Z
UID:1124-1465904700-1465908300@www.oa-roma.inaf.it
SUMMARY:Stellar evolution modeling of low-mass stars with magnetic fields: advances and challenges
DESCRIPTION:Though magnetic fields are commonly believed to play an important role\non the structure and evolution of stars\, there have been few attempts so\nfar to include their effects on stellar evolution models. Specifically\nin the case of low-mass stars\, those effects could account for some\ndisparities between standard stellar models predictions and\nobservations\, such as their radii and effective temperatures. In this\ntalk I will briefly review the modeling techniques for considering the\nmagnetic field effects on 1-D evolution codes\, and also present some\nrecent results of those techniques as implemented in the ATON stellar\nevolution code. Some theoretical and observational challenges to those\nresults will also be highlighted.
URL:https://www.oa-roma.inaf.it/event/stellar-evolution-modeling-of-low-mass-stars-with-magnetic-fields-advances-and-challenges/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160614T114500
DTEND;TZID=Europe/Rome:20160614T124500
DTSTAMP:20260404T192452
CREATED:20160425T071635Z
LAST-MODIFIED:20160425T071635Z
UID:4668-1465904700-1465908300@www.oa-roma.inaf.it
SUMMARY:Stellar evolution modeling of low-mass stars with magnetic fields: advances and challenges
DESCRIPTION:Though magnetic fields are commonly believed to play an important role\non the structure and evolution of stars\, there have been few attempts so\nfar to include their effects on stellar evolution models. Specifically\nin the case of low-mass stars\, those effects could account for some\ndisparities between standard stellar models predictions and\nobservations\, such as their radii and effective temperatures. In this\ntalk I will briefly review the modeling techniques for considering the\nmagnetic field effects on 1-D evolution codes\, and also present some\nrecent results of those techniques as implemented in the ATON stellar\nevolution code. Some theoretical and observational challenges to those\nresults will also be highlighted.
URL:https://www.oa-roma.inaf.it/event/stellar-evolution-modeling-of-low-mass-stars-with-magnetic-fields-advances-and-challenges-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160609T114500
DTEND;TZID=Europe/Rome:20160609T124500
DTSTAMP:20260404T192452
CREATED:20160506T044143Z
LAST-MODIFIED:20160506T044143Z
UID:1130-1465472700-1465476300@www.oa-roma.inaf.it
SUMMARY:The two-families scenario of compact stars: signatures and implications on GRBs
DESCRIPTION:In the last years the possibility of discriminating between the various theoretically possible compositions of a compact “neutron” star has become more and more convincing and it is based on the measure of a few fundamental quantities\, such as the radii (NICER\, LOFT)\, the moment of inertia (SKA) and/or the gravitational wave signal before and after the merging of two compact stars (VIRGO\, LIGO).\nI will outline the so-called two-families scenario in which both stars having very small radii (of the order of about 10.5 km) and stars having very large masses (of the order or larger than about 2 Ms) can exist. In that scenario very dense stars\, having small radii\, are made of neutron\, protons\, hyperons and other hadronic resonances\, while the most massive stars are strange-quark stars\, i.e. objects entirely made of deconfined quark matter. I will discuss the implications of the two-families scenario on short and long Gamma Ray Bursts within the proto-magnetar model of GRBs\, showing that quark deconfinement can be responsible both of the rapid termination of the prompt emission in short GRBs and of late time activity in long GRBs.
URL:https://www.oa-roma.inaf.it/event/the-two-families-scenario-of-compact-stars-signatures-and-implications-on-grbs/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160609T114500
DTEND;TZID=Europe/Rome:20160609T124500
DTSTAMP:20260404T192452
CREATED:20160506T044143Z
LAST-MODIFIED:20160506T044143Z
UID:4669-1465472700-1465476300@www.oa-roma.inaf.it
SUMMARY:The two-families scenario of compact stars: signatures and implications on GRBs
DESCRIPTION:In the last years the possibility of discriminating between the various theoretically possible compositions of a compact “neutron” star has become more and more convincing and it is based on the measure of a few fundamental quantities\, such as the radii (NICER\, LOFT)\, the moment of inertia (SKA) and/or the gravitational wave signal before and after the merging of two compact stars (VIRGO\, LIGO).\nI will outline the so-called two-families scenario in which both stars having very small radii (of the order of about 10.5 km) and stars having very large masses (of the order or larger than about 2 Ms) can exist. In that scenario very dense stars\, having small radii\, are made of neutron\, protons\, hyperons and other hadronic resonances\, while the most massive stars are strange-quark stars\, i.e. objects entirely made of deconfined quark matter. I will discuss the implications of the two-families scenario on short and long Gamma Ray Bursts within the proto-magnetar model of GRBs\, showing that quark deconfinement can be responsible both of the rapid termination of the prompt emission in short GRBs and of late time activity in long GRBs.
URL:https://www.oa-roma.inaf.it/event/the-two-families-scenario-of-compact-stars-signatures-and-implications-on-grbs-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160531T114500
DTEND;TZID=Europe/Rome:20160531T124500
DTSTAMP:20260404T192452
CREATED:20160216T154112Z
LAST-MODIFIED:20160216T154112Z
UID:452-1464695100-1464698700@www.oa-roma.inaf.it
SUMMARY:Dust-driven stellar winds in stellar evolution models
DESCRIPTION:Mass loss from stars during their evolution in the HR-diagram is an essential ingredient in stellar evolution models. Mass loss on the AGB is of particular interest when dust production is included in the model\, since it is well established that the winds of AGB stars are largely dust driven. For practical reasons\, the wind models adopted in stellar evolution codes are relatively simplistic: the actual mass-loss rate is prescribed and net effect of thermal gas pressure is usually not taken into account. In this talk I will discuss how wind these models can be improved without turning them into inhibiting computational challenges. I will also discuss (or speculate about) the effects such an improved wind model can have on the resultant dust yields for AGB stars.
URL:https://www.oa-roma.inaf.it/event/dust-driven-stellar-winds-in-stellar-evolution-models/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160531T114500
DTEND;TZID=Europe/Rome:20160531T124500
DTSTAMP:20260404T192452
CREATED:20160216T154112Z
LAST-MODIFIED:20160216T154112Z
UID:4654-1464695100-1464698700@www.oa-roma.inaf.it
SUMMARY:Dust-driven stellar winds in stellar evolution models
DESCRIPTION:Mass loss from stars during their evolution in the HR-diagram is an essential ingredient in stellar evolution models. Mass loss on the AGB is of particular interest when dust production is included in the model\, since it is well established that the winds of AGB stars are largely dust driven. For practical reasons\, the wind models adopted in stellar evolution codes are relatively simplistic: the actual mass-loss rate is prescribed and net effect of thermal gas pressure is usually not taken into account. In this talk I will discuss how wind these models can be improved without turning them into inhibiting computational challenges. I will also discuss (or speculate about) the effects such an improved wind model can have on the resultant dust yields for AGB stars.
URL:https://www.oa-roma.inaf.it/event/dust-driven-stellar-winds-in-stellar-evolution-models-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160524T114500
DTEND;TZID=Europe/Rome:20160524T124500
DTSTAMP:20260404T192452
CREATED:20160405T045612Z
LAST-MODIFIED:20160405T045612Z
UID:1047-1464090300-1464093900@www.oa-roma.inaf.it
SUMMARY:The square kilometre array
DESCRIPTION:Building on the major scientific achievements of the current generation of centimetre and metre-wavelength telescopes\, phase 1 of the Square Kilometre Array (SKA1) will be the next global radio astronomy observatory. It is currently being designed by engineers and scientists from around the world\, with the aim of beginning construction in 2018 and early science operations in 2020. SKA1 will conduct key tests of general relativity through surveys and timing of pulsars in our Galaxy. It will help answer fundamental questions related to the evolution of atomic Hydrogen in the Universe\, from the present day back to the Cosmic Dawn. I will give an overview of the wide breadth of science objectives that could be addressed by SKA1\, along with a description of the planned telescopes and the sites that will host them
URL:https://www.oa-roma.inaf.it/event/the-square-kilometre-array/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160524T114500
DTEND;TZID=Europe/Rome:20160524T124500
DTSTAMP:20260404T192452
CREATED:20160405T045612Z
LAST-MODIFIED:20160405T045612Z
UID:4664-1464090300-1464093900@www.oa-roma.inaf.it
SUMMARY:The square kilometre array
DESCRIPTION:Building on the major scientific achievements of the current generation of centimetre and metre-wavelength telescopes\, phase 1 of the Square Kilometre Array (SKA1) will be the next global radio astronomy observatory. It is currently being designed by engineers and scientists from around the world\, with the aim of beginning construction in 2018 and early science operations in 2020. SKA1 will conduct key tests of general relativity through surveys and timing of pulsars in our Galaxy. It will help answer fundamental questions related to the evolution of atomic Hydrogen in the Universe\, from the present day back to the Cosmic Dawn. I will give an overview of the wide breadth of science objectives that could be addressed by SKA1\, along with a description of the planned telescopes and the sites that will host them
URL:https://www.oa-roma.inaf.it/event/the-square-kilometre-array-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160520T200000
DTEND;TZID=Europe/Rome:20160520T230000
DTSTAMP:20260404T192452
CREATED:20160511T143021Z
LAST-MODIFIED:20160511T143021Z
UID:1149-1463774400-1463785200@www.oa-roma.inaf.it
SUMMARY:Serata Estiva
DESCRIPTION:Birra e astronomia
URL:https://www.oa-roma.inaf.it/event/serata-estiva/
LOCATION:OAR Monte Porzio Catone\, Via Frascati\, 33\, Monte Porzio Catone \, RM\, 00040\, Italia
CATEGORIES:Evento Pubblico
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160520T200000
DTEND;TZID=Europe/Rome:20160520T230000
DTSTAMP:20260404T192452
CREATED:20160511T143021Z
LAST-MODIFIED:20160511T143021Z
UID:4670-1463774400-1463785200@www.oa-roma.inaf.it
SUMMARY:Serata Estiva
DESCRIPTION:Birra e astronomia
URL:https://www.oa-roma.inaf.it/event/serata-estiva-2/
LOCATION:OAR Monte Porzio Catone\, Via Frascati\, 33\, Monte Porzio Catone \, RM\, 00040\, Italia
CATEGORIES:Evento Pubblico
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160517T114500
DTEND;TZID=Europe/Rome:20160517T124500
DTSTAMP:20260404T192452
CREATED:20160405T045745Z
LAST-MODIFIED:20160405T045745Z
UID:1048-1463485500-1463489100@www.oa-roma.inaf.it
SUMMARY:Evolution of close binary systems
DESCRIPTION:A general outlook of the evolution of close binary stars and of population synthesis as a method of their study will be presented. I will pay special attention to the evolution of low- and intermediate-mass stars (M < (8-10) solar) and to formation of different still hypothetical progenitors of SNe Ia. Next\, I will consider evolution of massive binaries with an accent on scenarii of evolution leading to the recently discovered gravitational waves burst GW150914
URL:https://www.oa-roma.inaf.it/event/evolution-of-close-binary-systems/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160517T114500
DTEND;TZID=Europe/Rome:20160517T124500
DTSTAMP:20260404T192452
CREATED:20160405T045745Z
LAST-MODIFIED:20160405T045745Z
UID:4665-1463485500-1463489100@www.oa-roma.inaf.it
SUMMARY:Evolution of close binary systems
DESCRIPTION:A general outlook of the evolution of close binary stars and of population synthesis as a method of their study will be presented. I will pay special attention to the evolution of low- and intermediate-mass stars (M < (8-10) solar) and to formation of different still hypothetical progenitors of SNe Ia. Next\, I will consider evolution of massive binaries with an accent on scenarii of evolution leading to the recently discovered gravitational waves burst GW150914
URL:https://www.oa-roma.inaf.it/event/evolution-of-close-binary-systems-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160510T114500
DTEND;TZID=Europe/Rome:20160510T124500
DTSTAMP:20260404T192452
CREATED:20160406T140237Z
LAST-MODIFIED:20160406T140237Z
UID:1066-1462880700-1462884300@www.oa-roma.inaf.it
SUMMARY:A closer look at the reionization sources: clustering\, line emission and feedback
DESCRIPTION:The epoch of reionization marks a major phase transition of the Universe\,\nduring which the intergalactic medium became transparent to UV photons.\nOver the last few years\, searches have intensified to identify the\npopulation of high redshift galaxies that might be responsible for this\nprocess and to constrain their properties. In this talk I will discuss\nrecent efforts to address the open problems in our understanding of the\nsources of reionization. I will present the results from a deep HST\nimaging program providing the first observational match to the theoretical\nprediction that reionization fronts are generated within significant\noverdensities of faint galaxies. I will show our ongoing analysis of the\nHST Frontier Fields survey and the resulting limits on the cut-off\nimprinted by photo-ionization feedback on the UV luminosity function at\nhigh redshift. Finally\, I will discuss a multi-band study of z~7 galaxies\nproviding evidence for strong line emission in the optical rest-frame\nregion and the first constraints on the escape fraction of ionizing\nphotons from these early galaxies.
URL:https://www.oa-roma.inaf.it/event/sodium-abundances-in-gc-agb-stars-what-do-they-tell-us/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160510T114500
DTEND;TZID=Europe/Rome:20160510T124500
DTSTAMP:20260404T192452
CREATED:20160406T140237Z
LAST-MODIFIED:20160406T140237Z
UID:4666-1462880700-1462884300@www.oa-roma.inaf.it
SUMMARY:A closer look at the reionization sources: clustering\, line emission and feedback
DESCRIPTION:The epoch of reionization marks a major phase transition of the Universe\,\nduring which the intergalactic medium became transparent to UV photons.\nOver the last few years\, searches have intensified to identify the\npopulation of high redshift galaxies that might be responsible for this\nprocess and to constrain their properties. In this talk I will discuss\nrecent efforts to address the open problems in our understanding of the\nsources of reionization. I will present the results from a deep HST\nimaging program providing the first observational match to the theoretical\nprediction that reionization fronts are generated within significant\noverdensities of faint galaxies. I will show our ongoing analysis of the\nHST Frontier Fields survey and the resulting limits on the cut-off\nimprinted by photo-ionization feedback on the UV luminosity function at\nhigh redshift. Finally\, I will discuss a multi-band study of z~7 galaxies\nproviding evidence for strong line emission in the optical rest-frame\nregion and the first constraints on the escape fraction of ionizing\nphotons from these early galaxies.
URL:https://www.oa-roma.inaf.it/event/sodium-abundances-in-gc-agb-stars-what-do-they-tell-us-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160503T114500
DTEND;TZID=Europe/Rome:20160503T124500
DTSTAMP:20260404T192452
CREATED:20160403T173151Z
LAST-MODIFIED:20160403T173151Z
UID:993-1462275900-1462279500@www.oa-roma.inaf.it
SUMMARY:The dawn of star formation: a local perspective
DESCRIPTION:At the end of the Dark Ages gravity began to make matter\ncollapse around over-densities\, resulting in the formation\nof the first stars\, the Pop III. These stars are very important in the\ncosmological context\, the most massive ones contributed ionizing\nphotons that played a role in the reionization of the Universe\nand synthetised the first metals. We know that the formation mode\nof these first stars was different than the one operating today.\nThe lack of metals implies it is difficult to cool a contracting cloud\,\nwhich would argue for a preferential formation of massive or very massive\nstars. However from the theoretical point of view it is not yet possible\nto determine the initial mass function of the first stars. Simulations\nshow that\, even in the absence of metals\, a collapsing cloud may fragment\ninto smaller clouds giving rise to stars that span a range of masses\, even\nsub-solar. Once the first metals begin to be shed in the clouds cooling\nbecomes possible\, either through atomic lines or through dust. It is likely\nthat there is a transition from Pop III to “normal” Pop II star formation\nat some critical metallicity\, however the precise value of this critical\nmetallicity cannot be presently determined theoretically.\nIn this seminar I will describe the observational efforts that our group\nis conducting in the local Universe\, in order to derive as many constraints\nas possible on the nature of the Pop III stars. These include searches\nof the most metal-poor stars\, and their chemical characterization.\nBoth the metallicity distribution function and the chemical pattern\nof the most metal-poor stars contain precious information of the first stars.
URL:https://www.oa-roma.inaf.it/event/the-dawn-of-star-formation-a-local-perspective/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160503T114500
DTEND;TZID=Europe/Rome:20160503T124500
DTSTAMP:20260404T192452
CREATED:20160403T173151Z
LAST-MODIFIED:20160403T173151Z
UID:4661-1462275900-1462279500@www.oa-roma.inaf.it
SUMMARY:The dawn of star formation: a local perspective
DESCRIPTION:At the end of the Dark Ages gravity began to make matter\ncollapse around over-densities\, resulting in the formation\nof the first stars\, the Pop III. These stars are very important in the\ncosmological context\, the most massive ones contributed ionizing\nphotons that played a role in the reionization of the Universe\nand synthetised the first metals. We know that the formation mode\nof these first stars was different than the one operating today.\nThe lack of metals implies it is difficult to cool a contracting cloud\,\nwhich would argue for a preferential formation of massive or very massive\nstars. However from the theoretical point of view it is not yet possible\nto determine the initial mass function of the first stars. Simulations\nshow that\, even in the absence of metals\, a collapsing cloud may fragment\ninto smaller clouds giving rise to stars that span a range of masses\, even\nsub-solar. Once the first metals begin to be shed in the clouds cooling\nbecomes possible\, either through atomic lines or through dust. It is likely\nthat there is a transition from Pop III to “normal” Pop II star formation\nat some critical metallicity\, however the precise value of this critical\nmetallicity cannot be presently determined theoretically.\nIn this seminar I will describe the observational efforts that our group\nis conducting in the local Universe\, in order to derive as many constraints\nas possible on the nature of the Pop III stars. These include searches\nof the most metal-poor stars\, and their chemical characterization.\nBoth the metallicity distribution function and the chemical pattern\nof the most metal-poor stars contain precious information of the first stars.
URL:https://www.oa-roma.inaf.it/event/the-dawn-of-star-formation-a-local-perspective-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160426T114500
DTEND;TZID=Europe/Rome:20160426T124500
DTSTAMP:20260404T192452
CREATED:20160403T173332Z
LAST-MODIFIED:20160403T173332Z
UID:995-1461671100-1461674700@www.oa-roma.inaf.it
SUMMARY:Machine learning search for gamma-ray burst afterglows in optical images
DESCRIPTION:Thanks to the rapid advances in robotic telescopes and wide field surveys\, the time domain astronomy reveals a huge number of transient detections every night. Therefore\,  automatic classification of sources in the optical images is essential. A special attention is brought to the identification of gamma-ray burst afterglows using the combined observational data from the GROND telescope and the SDSS survey. Their successful identification can lead to further follow-up observations by dedicated telescopes and for statistical studies of these transients.
URL:https://www.oa-roma.inaf.it/event/machine-learning-search-for-gamma-ray-burst-afterglows-in-optical-images/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160426T114500
DTEND;TZID=Europe/Rome:20160426T124500
DTSTAMP:20260404T192452
CREATED:20160403T173332Z
LAST-MODIFIED:20160403T173332Z
UID:4662-1461671100-1461674700@www.oa-roma.inaf.it
SUMMARY:Machine learning search for gamma-ray burst afterglows in optical images
DESCRIPTION:Thanks to the rapid advances in robotic telescopes and wide field surveys\, the time domain astronomy reveals a huge number of transient detections every night. Therefore\,  automatic classification of sources in the optical images is essential. A special attention is brought to the identification of gamma-ray burst afterglows using the combined observational data from the GROND telescope and the SDSS survey. Their successful identification can lead to further follow-up observations by dedicated telescopes and for statistical studies of these transients.
URL:https://www.oa-roma.inaf.it/event/machine-learning-search-for-gamma-ray-burst-afterglows-in-optical-images-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160412T114500
DTEND;TZID=Europe/Rome:20160412T124500
DTSTAMP:20260404T192452
CREATED:20160405T045429Z
LAST-MODIFIED:20160405T045429Z
UID:1046-1460461500-1460465100@www.oa-roma.inaf.it
SUMMARY:Escape of Lyman photons from galaxies
DESCRIPTION:One of the key questions in observational cosmology is the identification of the sources responsible for cosmic\nreionization. The general consensus is that a population of faint low-mass galaxies must be responsible for the\nbulk of the ionizing photons. However\, until recently\, attempts at identifying individual galaxies showing\nLyman continuum (LyC) leakage have only found very few such galaxies\, both at high and low redshifts.\nWe recently proposed a new indirect diagnostic for LyC leakage based on the shape of the Lyman-alpha line\,\nthat I will first review (Verhamme+15).\nA breakthrough was recently achieved by our team (Izotov et al. 2016a\,b)\, detecting LyC emission in\nlow-redshift (z~0.3) luminous compact star-forming galaxies (LCGs) with high LyC escape fractions\nusing HST/COS observations. I will present these new results\, and the Lyman-alpha emission from these galaxies\,\nconfirming our theoretical predictions.\nFinally\, I will propose another complementary Lyman-alpha signature for LyC leakage\, discussing theoretical predictions\non the Lyman-alpha spatial extend of LyC emitters: LyC leakers should have no/faint Lyman-alpha halos.
URL:https://www.oa-roma.inaf.it/event/escape-of-lyman-photons-from-galaxies/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160412T114500
DTEND;TZID=Europe/Rome:20160412T124500
DTSTAMP:20260404T192452
CREATED:20160405T045429Z
LAST-MODIFIED:20160405T045429Z
UID:4663-1460461500-1460465100@www.oa-roma.inaf.it
SUMMARY:Escape of Lyman photons from galaxies
DESCRIPTION:One of the key questions in observational cosmology is the identification of the sources responsible for cosmic\nreionization. The general consensus is that a population of faint low-mass galaxies must be responsible for the\nbulk of the ionizing photons. However\, until recently\, attempts at identifying individual galaxies showing\nLyman continuum (LyC) leakage have only found very few such galaxies\, both at high and low redshifts.\nWe recently proposed a new indirect diagnostic for LyC leakage based on the shape of the Lyman-alpha line\,\nthat I will first review (Verhamme+15).\nA breakthrough was recently achieved by our team (Izotov et al. 2016a\,b)\, detecting LyC emission in\nlow-redshift (z~0.3) luminous compact star-forming galaxies (LCGs) with high LyC escape fractions\nusing HST/COS observations. I will present these new results\, and the Lyman-alpha emission from these galaxies\,\nconfirming our theoretical predictions.\nFinally\, I will propose another complementary Lyman-alpha signature for LyC leakage\, discussing theoretical predictions\non the Lyman-alpha spatial extend of LyC emitters: LyC leakers should have no/faint Lyman-alpha halos.
URL:https://www.oa-roma.inaf.it/event/escape-of-lyman-photons-from-galaxies-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160405T114500
DTEND;TZID=Europe/Rome:20160405T124500
DTSTAMP:20260404T192452
CREATED:20160317T061919Z
LAST-MODIFIED:20160317T061919Z
UID:544-1459856700-1459860300@www.oa-roma.inaf.it
SUMMARY:The final wind: stars in retirement
DESCRIPTION:Catastrophic mass loss is at the heart of 90% of all stellar\ndeath. Low and intermediate mass stars lose their hydrogen envelope\nwhile on the Asymptotic Giant Branch stars. At the end\, there is\ninsufficient hydrogen left and the star rapidly evolves into a white\ndwarf\, briefly illuminating a planetary nebula on the way. The ejected\ngas can be used to study the superwind\, the nuclear burning and dredge\nup processes in the star\, and even (with some difficulties) the star\nformation histories of the dying stellar population. In this talk I\nwill discuss the planetary nebulae of the Galactic bulge\, briefly\nmention AGB stars in globular clusters\, and finally discuss the origin\nof the mysterious AGB J-type stars\, believed to be the cause of the\nA+B grains in the proto-solar system.
URL:https://www.oa-roma.inaf.it/event/the-final-wind-stars-in-retirement/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160405T114500
DTEND;TZID=Europe/Rome:20160405T124500
DTSTAMP:20260404T192452
CREATED:20160317T061919Z
LAST-MODIFIED:20160317T061919Z
UID:4657-1459856700-1459860300@www.oa-roma.inaf.it
SUMMARY:The final wind: stars in retirement
DESCRIPTION:Catastrophic mass loss is at the heart of 90% of all stellar\ndeath. Low and intermediate mass stars lose their hydrogen envelope\nwhile on the Asymptotic Giant Branch stars. At the end\, there is\ninsufficient hydrogen left and the star rapidly evolves into a white\ndwarf\, briefly illuminating a planetary nebula on the way. The ejected\ngas can be used to study the superwind\, the nuclear burning and dredge\nup processes in the star\, and even (with some difficulties) the star\nformation histories of the dying stellar population. In this talk I\nwill discuss the planetary nebulae of the Galactic bulge\, briefly\nmention AGB stars in globular clusters\, and finally discuss the origin\nof the mysterious AGB J-type stars\, believed to be the cause of the\nA+B grains in the proto-solar system.
URL:https://www.oa-roma.inaf.it/event/the-final-wind-stars-in-retirement-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
END:VCALENDAR