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X-ORIGINAL-URL:https://www.oa-roma.inaf.it
X-WR-CALDESC:Eventi per Osservatorio Astronomico di Roma
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DTSTART:20170326T010000
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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180306T114500
DTEND;TZID=Europe/Rome:20180306T124500
DTSTAMP:20260407T012148
CREATED:20171016T082612Z
LAST-MODIFIED:20171016T082612Z
UID:3643-1520336700-1520340300@www.oa-roma.inaf.it
SUMMARY:An experiment in Astrobiology: exploring the climate parameter space of rocky planets
DESCRIPTION:Astrobiology is a relatively new and fast-growing science\, whose main\ncharacteristic is to need expertises from different science fields.\nI’ll show how the climate of a planet influences its abitability.\nAstronomers from OATs\, climatologists from CNR and experts in\ndatabases from OATs joined their efforts to build a fast\, simplified\,\nyet effective climate model and database for extra-solar planets. I\nwill describe\nthe model\, its main feature\, its validation\, its application to a\nspecific exo-planet (Kepler 452b). I will then show how such a model\ncan be used to explore a huge parameter space and build a database\nthat can be used to characterize classes of habitable planets. I will\npoint out how this particular case is an good example of\nHigh-Throughput  Computing (HTC). Our database can also be used\, e.g.\,\nas a tool to get a first estimate of the habitability of a newly\ndiscovered rocky planet.\nThen I will describe possible future developements of such a research\nline\, including the study of the effect of the biosphere itself on the\nhabitability.
URL:https://www.oa-roma.inaf.it/event/seminar-by-giuseppe-murante/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180306T114500
DTEND;TZID=Europe/Rome:20180306T124500
DTSTAMP:20260407T012148
CREATED:20171016T082612Z
LAST-MODIFIED:20171016T082612Z
UID:4735-1520336700-1520340300@www.oa-roma.inaf.it
SUMMARY:An experiment in Astrobiology: exploring the climate parameter space of rocky planets
DESCRIPTION:Astrobiology is a relatively new and fast-growing science\, whose main\ncharacteristic is to need expertises from different science fields.\nI’ll show how the climate of a planet influences its abitability.\nAstronomers from OATs\, climatologists from CNR and experts in\ndatabases from OATs joined their efforts to build a fast\, simplified\,\nyet effective climate model and database for extra-solar planets. I\nwill describe\nthe model\, its main feature\, its validation\, its application to a\nspecific exo-planet (Kepler 452b). I will then show how such a model\ncan be used to explore a huge parameter space and build a database\nthat can be used to characterize classes of habitable planets. I will\npoint out how this particular case is an good example of\nHigh-Throughput  Computing (HTC). Our database can also be used\, e.g.\,\nas a tool to get a first estimate of the habitability of a newly\ndiscovered rocky planet.\nThen I will describe possible future developements of such a research\nline\, including the study of the effect of the biosphere itself on the\nhabitability.
URL:https://www.oa-roma.inaf.it/event/seminar-by-giuseppe-murante-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180314T114500
DTEND;TZID=Europe/Rome:20180314T124500
DTSTAMP:20260407T012148
CREATED:20171128T072427Z
LAST-MODIFIED:20171128T072427Z
UID:3780-1521027900-1521031500@www.oa-roma.inaf.it
SUMMARY:Drag and drift - decoupling of the dust and gas phases in astrophysical flows
DESCRIPTION:Simulating the dynamics of gas and dust in various astrophysical contexts is a topic of intense research. It includes simulations of the turbulent interstellar medium (ISM)\, active galactic nuclei (AGN)\, proto-planetary discs\, and dusty stellar winds. I will focus on the ISM and dust-driven stellar winds\, however\, and only briefly mention a few other examples.\nUsing high-resolution (1024^3) simulations of homogeneous isothermal hydrodynamic turbulence\, including a multi-disperse population of 10^7 dust grains imbedded in the gas\, one may assess the efficiency of condensation\, destruction and coagulation in molecular clouds. Due to hydrodynamic drag\, large grains will decouple from a turbulent gas flow\, while small grains will tend to follow the motions of the gas. Dust grains of various sizes will also cluster and increase the rate of grain-grain interaction. This may in turn lead to turbulence-driven coagulation and fragmentation.\nIn a stellar-wind context the decoupling between gas and dust is often called “drift”\, which is referring to the fact that the two phases may develop different mean-flow velocities. In a spherically-symmetric setting\, a mean-flow model of drift is fairly simple. But there are significant 3D effects\, as well as instabilities\, which we must take into account. For instance\, dust grains of various sizes will cluster and increase the rate of grain-grain interaction. Moreover\, due to spatial separation of dust and gas\, condensation is likely less effective than in a velocity-coupled case. There are several implications for dust-driven stellar winds which arise from this. One is that the momentum-transfer efficiency (from dust to gas) of large grains may be low as they cluster where the gas is not; another is that the sublimation rate increases as grains are more exposed to the radiation field.
URL:https://www.oa-roma.inaf.it/event/seminar-by-lars-mattsson/
LOCATION:RM
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180314T114500
DTEND;TZID=Europe/Rome:20180314T124500
DTSTAMP:20260407T012148
CREATED:20171128T072427Z
LAST-MODIFIED:20171128T072427Z
UID:4739-1521027900-1521031500@www.oa-roma.inaf.it
SUMMARY:Drag and drift - decoupling of the dust and gas phases in astrophysical flows
DESCRIPTION:Simulating the dynamics of gas and dust in various astrophysical contexts is a topic of intense research. It includes simulations of the turbulent interstellar medium (ISM)\, active galactic nuclei (AGN)\, proto-planetary discs\, and dusty stellar winds. I will focus on the ISM and dust-driven stellar winds\, however\, and only briefly mention a few other examples.\nUsing high-resolution (1024^3) simulations of homogeneous isothermal hydrodynamic turbulence\, including a multi-disperse population of 10^7 dust grains imbedded in the gas\, one may assess the efficiency of condensation\, destruction and coagulation in molecular clouds. Due to hydrodynamic drag\, large grains will decouple from a turbulent gas flow\, while small grains will tend to follow the motions of the gas. Dust grains of various sizes will also cluster and increase the rate of grain-grain interaction. This may in turn lead to turbulence-driven coagulation and fragmentation.\nIn a stellar-wind context the decoupling between gas and dust is often called “drift”\, which is referring to the fact that the two phases may develop different mean-flow velocities. In a spherically-symmetric setting\, a mean-flow model of drift is fairly simple. But there are significant 3D effects\, as well as instabilities\, which we must take into account. For instance\, dust grains of various sizes will cluster and increase the rate of grain-grain interaction. Moreover\, due to spatial separation of dust and gas\, condensation is likely less effective than in a velocity-coupled case. There are several implications for dust-driven stellar winds which arise from this. One is that the momentum-transfer efficiency (from dust to gas) of large grains may be low as they cluster where the gas is not; another is that the sublimation rate increases as grains are more exposed to the radiation field.
URL:https://www.oa-roma.inaf.it/event/seminar-by-lars-mattsson-2/
LOCATION:RM
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180327T114500
DTEND;TZID=Europe/Rome:20180327T124500
DTSTAMP:20260407T012148
CREATED:20180307T142645Z
LAST-MODIFIED:20180307T142645Z
UID:4064-1522151100-1522154700@www.oa-roma.inaf.it
SUMMARY:Bright and dustiest stars in the JWST era: powerful tools to constrain the recent star formation history
DESCRIPTION:With the advent of the JWST\, the horizon of our knowledgies will be amazingly enlarged\, providing an unprecedent look of a large volume of galaxies with a broad properties range. This will be possible in the IR domain where the extinction is low and bright cool evolved stars have their emission peak. This is the case of asymptotic giant branch stars (AGB)\, luminous objects and main dust producers for the galaxy. We present how the large release of AGB+dust evolutionary models developed in the last years\, will enable a detailed study of these sources in different systems. The distribution of these objects in the IR colour-magnitude diagrams is a powerful instrument to determine the recent star formation history of the galaxy in detail.
URL:https://www.oa-roma.inaf.it/event/bright-and-dustiest-stars-in-the-jwst-era-powerful-tools-to-constrain-the-recent-star-formation-history/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180327T114500
DTEND;TZID=Europe/Rome:20180327T124500
DTSTAMP:20260407T012148
CREATED:20180307T142645Z
LAST-MODIFIED:20180307T142645Z
UID:4747-1522151100-1522154700@www.oa-roma.inaf.it
SUMMARY:Bright and dustiest stars in the JWST era: powerful tools to constrain the recent star formation history
DESCRIPTION:With the advent of the JWST\, the horizon of our knowledgies will be amazingly enlarged\, providing an unprecedent look of a large volume of galaxies with a broad properties range. This will be possible in the IR domain where the extinction is low and bright cool evolved stars have their emission peak. This is the case of asymptotic giant branch stars (AGB)\, luminous objects and main dust producers for the galaxy. We present how the large release of AGB+dust evolutionary models developed in the last years\, will enable a detailed study of these sources in different systems. The distribution of these objects in the IR colour-magnitude diagrams is a powerful instrument to determine the recent star formation history of the galaxy in detail.
URL:https://www.oa-roma.inaf.it/event/bright-and-dustiest-stars-in-the-jwst-era-powerful-tools-to-constrain-the-recent-star-formation-history-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
END:VCALENDAR