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X-WR-CALNAME:Osservatorio Astrofisico di Catania
X-ORIGINAL-URL:https://www.oact.inaf.it
X-WR-CALDESC:Eventi per Osservatorio Astrofisico di Catania
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DTSTART:20230101T000000
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BEGIN:VEVENT
DTSTART;TZID=UTC:20240212T113000
DTEND;TZID=UTC:20240212T120000
DTSTAMP:20240206T101358Z
CREATED:20240206T101354Z
LAST-MODIFIED:20240206T101358Z
UID:15576-1707737400-1707739200@www.oact.inaf.it
SUMMARY:Investigating the link between protoplanets\, disk substructures and disk winds
DESCRIPTION:Recording: https://www.oact.inaf.it/seminars/ \nDATE:  Monday\, February 12\, 11:30 a.m. \nORGANIZER: INAF OACT \nLOCATION: AULA OVEST (INAF-OACT) + remote \nLink for the remote audience:https://meet.google.com/wvf-uwxo-oyj \nSPEAKER: Dr. Justyn Campbell-White (ESO-Garching) \nABSTRACT: \nProtoplanetary disks are now routinely observed around young stars but the planets they produce remain elusive to detect. So far\, we have only one confirmed direct detection of protoplanets in the disk of PDS 70\, with some tentative results (e.g. AB Aur). Yet disk structures are found almost ubiquitously across the sample of resolved disks. We are investigating the potential relationship between inner disk winds and outflows (traced by optical emission lines\, such as [OI])\, and the presence and type of disk substructures. We aim to determine whether or not the various substructures are the direct results of protoplanet formation. \nI will present new results from recent and archival observations of PDS 70. In order to investigate such connections between winds\, substructures and planets\, we turn to the one system where we have certainly detected the planets. We have carefully applied established techniques to the high-resolution spectra to reveal previously unseen forbidden emission profiles. These results suggest a significant wind originating from the inner disk. We compare these results and measurements of the mass accretion rate and disk properties to those of other weakly accreting young stars and those with transition disks. \nWe are also carrying out this investigation for the PENELLOPE/ULLYSES sample of ~80 young stars. This complements existing surveys of such winds/outflows\, whilst allowing for further exploration of the relation to disk substructures\, towards a more complete statistical survey. \n  \nA few rules:— in case of large in-person attendance\, attendees may be asked to wear a face mask— before joining\, make sure you are using your institutional inaf.it account if you have one (otherwise we will grant you permission to join)— please do not forget to mute your microphone and switch off your webcam when access the virtual room— for questions leave a message in the chat\, the answers at the end of the webinar— the seminar will be recorded\, so if you are interested in it\, please contact us to get the link to the registration.
URL:https://www.oact.inaf.it/event/investigating-the-link-between-protoplanets-disk-substructures-and-disk-winds/
LOCATION:Sede A. Riccò\, Via Santa Sofia 78\, Catania
CATEGORIES:Eventi & Seminari
ATTACH;FMTTYPE=image/jpeg:https://www.oact.inaf.it/wp-content/uploads/2024/02/JCW_INAF_02_2024_page-0001.jpg
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DTSTART;TZID=UTC:20240130T113000
DTEND;TZID=UTC:20240130T120000
DTSTAMP:20240124T084338Z
CREATED:20240123T222903Z
LAST-MODIFIED:20240124T084338Z
UID:15478-1706614200-1706616000@www.oact.inaf.it
SUMMARY:RU Lup: the accretion environment of a prototypical Classical T Tauri star
DESCRIPTION:Recording: https://www.oact.inaf.it/seminars/ \nDATE:  Tuesday\, January 30\, 11:30 a.m. \nORGANIZER: INAF OACT \nLOCATION: AULA OVEST (INAF-OACT) + remote \nLink for the remote audience:https://meet.google.com/wvf-uwxo-oyj \nSPEAKER: Dr. Antonio Armeni (Tuebingen University) \nABSTRACT: \nWhile it is well established that Classical T Tauri stars accrete material from a circumstellar disk through magnetic fields\, the physics regulating the processes in the inner (0.1 AU) disk is still not well understood. With its long observational history and its rich emission line spectrum\, RU Lup is a prime example to study this environment. \nRU Lup is a monitoring target within the ULLYSES survey for Classical T Tauri stars. Optical spectroscopic observations with CHIRON and ESPRESSO were obtained simultaneously with the two epochs of the ULLYSES monitoring program for RU Lup. \nIn this talk\, I will discuss the main results obtained by analyzing this collection of data\, supplemented by the two TESS observations and the archival AAVSO photometry of RU Lup.Using the high resolution ESPRESSO spectra\, we improved the measurements of the stellar parameters\, especially the projected rotational velocity (vsini).We determined the veiling fraction for the ESPRESSO spectra\, showing that the veiling consists of two components: a continuum emission likely originating in the accretion shock and line emission that fills in the photospheric absorption lines.We detected a periodic modulation in the narrow component (NC) of the He I 5876 line with a period that is compatible with the stellar rotation period\, indicating the presence of a compact region on the stellar surface that we identified as the footprint of the accretion shock. Although the brightness of RU Lup changed drastically both on daily and yearly timescales\, this region is overall stable over the 3 years covered by the observations.An analysis of the high-cadence TESS light curves revealed quasi-periodic oscillations (QPO) on timescales shorter than the stellar rotation period. This suggests that the accretion disk in RU Lup extends inward of the corotation radius and the star accretes through a magnetic boundary layer (MBL). The rich metallic emission line spectrum of RU Lup might be characteristic of this accretion regime. \n  \n  \nA few rules:— in case of large in-person attendance\, attendees may be asked to wear a face mask— before joining\, make sure you are using your institutional inaf.it account if you have one (otherwise we will grant you permission to join)— please do not forget to mute your microphone and switch off your webcam when access the virtual room— for questions leave a message in the chat\, the answers at the end of the webinar— the seminar will be recorded\, so if you are interested in it\, please contact us to get the link to the registration.
URL:https://www.oact.inaf.it/event/ru-lup-the-accretion-environment-of-a-prototypical-classical-t-tauri-star/
LOCATION:Sede A. Riccò\, Via Santa Sofia 78\, Catania
CATEGORIES:Eventi & Seminari
ATTACH;FMTTYPE=image/jpeg:https://www.oact.inaf.it/wp-content/uploads/2024/01/RU_Lup_cover_page-0001.jpg
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