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PRODID:-//Osservatorio Astronomico di Roma - ECPv6.15.18//NONSGML v1.0//EN
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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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TZID:Europe/Rome
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DTSTART:20180325T010000
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DTSTART:20181028T010000
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DTSTART:20190331T010000
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DTSTART:20191027T010000
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DTSTART:20200329T010000
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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190205T114500
DTEND;TZID=Europe/Rome:20190205T124500
DTSTAMP:20260407T094504
CREATED:20180731T173932Z
LAST-MODIFIED:20180731T173932Z
UID:4274-1549367100-1549370700@www.oa-roma.inaf.it
SUMMARY:colloqium - Eva Villaver
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/colloqium-eva-villaver/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190205T114500
DTEND;TZID=Europe/Rome:20190205T124500
DTSTAMP:20260407T094504
CREATED:20180731T173932Z
LAST-MODIFIED:20190114T134429Z
UID:4762-1549367100-1549370700@www.oa-roma.inaf.it
SUMMARY:From AGB stars to Planetary Nebulae: what the ISM\, stellar rotation\, and companions can do
DESCRIPTION:Asymptotic giant branch (AGB) stars lose their envelopes by means of heavy mass-loss rates. Besides the mass-loss process itself there are other mechanisms that influence the evolution of the star and of what we see as Planetary Nebulae. Among them are the interaction of the ejecta with the interstellar medium (ISM)\, the inclusion of stellar rotation and/or the presence of a companion. I will present our simulation of the interaction process between AGB stars and  the ISM. I will show what we can expect for the planetary nebula formation when we include rotation in stellar evolution models and finally I will describe how these stars are influenced by the presence of external companions
URL:https://www.oa-roma.inaf.it/event/colloqium-eva-villaver-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190212T114500
DTEND;TZID=Europe/Rome:20190212T124500
DTSTAMP:20260407T094504
CREATED:20181010T170838Z
LAST-MODIFIED:20190122T090137Z
UID:4775-1549971900-1549975500@www.oa-roma.inaf.it
SUMMARY:Stellar Populations in Local and high redshift Universe
DESCRIPTION:Synthetic stellar libraries are quite popular to constrain the stellar pop-\nulations (age and metallicity distribution) of unresolved systems like high redshift galaxies.\nHowever\, they are typically based on theoretical Spectral Energy Distributions (SEDs).\nIt is important to build up empirical synthetic stellar li-\nbraries\, calibrated on local systems and\ncovering a broad range in ages (globular clusters\, old open clusters)\,\nchemical compositions (iron\, alpha\, CNO) and dynamical properties (nearby\ndwarf galaxies)\, able to improve our SED fitting codes to deeply investigate\nhigh redshift galaxies.\nTo do that\, I am taking advantages of a sample of 65 Galactic globular clus-\nters (GGCs) for which we have accurate and homogeneous optical photometry\nbased on space (ACS at HST\, innermost regions) and ground-based\n(up to the tadial radius).\nIn particular\, I will present the results on the study of the Horizontal Branch\n(HB) morphology for 64 GGCs in our sample.\nI will introduce a very new photometric morphology index based\non the cumulative density function of the stars along the HB\,\nuseful to investigate the well known “second\nparameter problem” affecting age estimations and so\, stellar libraries.\nI will also discuss the results of the analysis on galaxy\nevolution through the Galaxy Stellar Mass Function (GSMF) up to redf-\nshift 4\, obtained combining all the five CANDELS fields (GOODS-South\,\nGOODS-North\, EGS\, COSMOS\, UDS)\, the Frontier Fields Parallels (Abell 2744\,\nMACSJ0416\, MACSJ0717\, MACSJ1149) and the Ultravista/COSMOS\nfield. Stellar masses have been estimated fitting the photometry to syn-\nthetic models: these surveys are characterized by multi-wavelength (deep\noptical/near-infrared/mid-infrared) coverage (CANDELS)\, very high limiting magnitudes\n(Frontier Fields) and large areas (UltraVista)\, allowing to explore the GSMF\nfrom low masses to the high-mass end.
URL:https://www.oa-roma.inaf.it/event/colloquium-marianna-torelli-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190212T114500
DTEND;TZID=Europe/Rome:20190212T124500
DTSTAMP:20260407T094504
CREATED:20181010T170838Z
LAST-MODIFIED:20181010T170838Z
UID:4438-1549971900-1549975500@www.oa-roma.inaf.it
SUMMARY:Colloquium - Marianna Torelli
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/colloquium-marianna-torelli/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190214T114500
DTEND;TZID=Europe/Rome:20190214T124500
DTSTAMP:20260407T094504
CREATED:20181106T174714Z
LAST-MODIFIED:20181106T174714Z
UID:4817-1550144700-1550148300@www.oa-roma.inaf.it
SUMMARY:colloquium - Giuseppe Tanzella-Nitti
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/colloquium-giuseppe-tanzella-nitti/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190219T114500
DTEND;TZID=Europe/Rome:20190219T124500
DTSTAMP:20260407T094504
CREATED:20180907T101417Z
LAST-MODIFIED:20190118T055424Z
UID:4767-1550576700-1550580300@www.oa-roma.inaf.it
SUMMARY:Star formation in the Local Group
DESCRIPTION:Using Hubble Space Telescope (HST) observations\, we have identified and\ncharacterised almost 50\,000 pre-main sequence (PMS) stars in several\nstar-forming regions in the Milky Way and Magellanic Clouds. These objects\nare still undergoing active mass accretion\, as revealed by excess emission\nin the Halpha band. Detailed knowledge of the extinction law in these\nfields\, which we derive directly from the observations\, allows us to\naccurately obtain stellar physical parameters (temperature\, luminosity\,\nage\, mass\, and mass accretion rate). This is presently the largest and\nmost homogeneous sample of PMS objects\, on which we are conducting the\nfirst comprehensive and systematic study of the PMS phase\, spanning a wide\nrange of masses (0.5-4 Msun)\, metallicities (0.1-1 Zsun) and ages (0.5-30\nMyr). \nI will discuss how star formation has proceeded in these regions over\nmultiple recent bursts and how the accretion process depends on the\nphysical properties of the individual stars and of the environment. We\nhave discovered an important dependence of the mass accretion rate on\nmetallicity: mass accretion rates for stars of the same mass and age are\nsystematically higher in the Magellanic Clouds than in the Milky Way and\nare expected to have been equally high at redshift z~2\, when star\nformation was at its peak in the Universe. I will also show a surprising\nanti-correlation between the variability and intensity of the Halpha\nexcess: this suggests a discrete and clumpy nature for the accretion\nprocess and reveals that the characteristic mass of the infalling parcels\nof gas is comparable to that of the moons of giant planets in the solar\nsystem. \nTo close\, I will illustrate how we plan to thoroughly verify these results\nspectroscopically and to extend them to lower mass objects and to more\nextinguished environments through already planned guaranteed-time\nobservations with the James Webb Space Telescope. Our measurements will\nprovide\, for the first time\, quantitative information on the nature\,\nexcitation\, and kinematics of the infalling gas in these dense environments.
URL:https://www.oa-roma.inaf.it/event/colloquium-by-guido-de-marchi-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190219T114500
DTEND;TZID=Europe/Rome:20190219T124500
DTSTAMP:20260407T094504
CREATED:20180907T101417Z
LAST-MODIFIED:20180907T101417Z
UID:4371-1550576700-1550580300@www.oa-roma.inaf.it
SUMMARY:colloquium - Guido De Marchi
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/colloquium-by-guido-de-marchi/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190226T114500
DTEND;TZID=Europe/Rome:20190226T124500
DTSTAMP:20260407T094504
CREATED:20181105T103706Z
LAST-MODIFIED:20190219T062329Z
UID:4807-1551181500-1551185100@www.oa-roma.inaf.it
SUMMARY:When the going get tough... or: observation and laboratory work for life searching in other worlds
DESCRIPTION:“…if we never search\, the chance of success is zero”. This was the conclusion in the seminal paper of G. Cocconi and P. Morrison in 1959 about the search for life. Since then\, a lot of progress in technology and a lot of exciting results in astrophysics have been reached. Today\, we know that\, out of there\, there are more than 4000 new worlds showing a large diversity in their size and orbital characteristics. In the midst of all these strange new worlds\, a very promising type of them\, the super Earths\, seems to be ubiquitous in the Galaxy. Moreover\, in fashion there are super Earths orbiting M stars. But\, such an odd couple could host life? And if it can\, how to find it?
URL:https://www.oa-roma.inaf.it/event/colloquium-sandeep-haridasu/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
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