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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
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TZID:Europe/Rome
BEGIN:DAYLIGHT
TZOFFSETFROM:+0100
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TZNAME:CEST
DTSTART:20150329T010000
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TZOFFSETTO:+0100
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DTSTART:20151025T010000
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DTSTART:20160327T010000
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DTSTART:20161030T010000
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DTSTART:20170326T010000
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DTSTART:20171029T010000
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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160503T114500
DTEND;TZID=Europe/Rome:20160503T124500
DTSTAMP:20260408T173954
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:20260408T173954
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:20160510T114500
DTEND;TZID=Europe/Rome:20160510T124500
DTSTAMP:20260408T173954
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:20260408T173954
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:20160517T114500
DTEND;TZID=Europe/Rome:20160517T124500
DTSTAMP:20260408T173954
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:20260408T173954
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:20160520T200000
DTEND;TZID=Europe/Rome:20160520T230000
DTSTAMP:20260408T173954
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:20260408T173954
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:20160524T114500
DTEND;TZID=Europe/Rome:20160524T124500
DTSTAMP:20260408T173954
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:20260408T173954
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:20160531T114500
DTEND;TZID=Europe/Rome:20160531T124500
DTSTAMP:20260408T173954
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:20260408T173954
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
END:VCALENDAR