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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20230523T170000
DTEND;TZID=Atlantic/Canary:20230523T180000
UID:iactalks-1698
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1698
CREATED:2023-05-23T17:00:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:IAU G5:  A Gaia view of magnetic activity and rotation of low-mass 
 stars
DESCRIPTION:IAU G5:  A Gaia view of magnetic activity and rotation of low-m
 ass stars\nDr. Alessandro Lanzafame\n\n Gaia all-sky scanning an
 d multi-epoch photometric and spectroscopic observations offer unprecedent
 ed opportunities to detect and characterise magnetic activity and rotation
  of low-mass stars. In the second Gaia data release, rotation pe
 riod and rotational modulation amplitude for ≈150,000 low-mass stars
  were provided from the analysis of the first 22-month of data collection.
  The third Gaia data release, based on the analysis of the first
  34 months of data collection, contains rotational modulation data for &as
 ymp;500,00 low-mass stars and an activity index for ≈2 million low-m
 ass stars, this latter derived from the analysis of the CaII infrared trip
 let (IRT) observed by the RVS instrument. These constitute the largest cat
 alogues of magnetic activity and rotational period to date. Such a large n
 umber of all-sky measurements represents a gold mine for studies related t
 o stellar rotation, magnetic activity, and mass accretion. The analysis of
  the period-amplitude diagram of the rotational modulation has already pro
 vided evidence of distinct magneto-rotational regimes in the early phase o
 f stellar evolution and of rapid transitions between them. Such evidence c
 hallenges a dependence on rotation only and suggests an important role of 
 the rotational history in the early phase of the magneto-rotational evolut
 ion. The activity index derived from the CaII IRT clearly show three regim
 es, confirming suggestions made by previous authors on much smaller datase
 ts. For the first time, a dramatic change in the activity distribution is 
 found for Teff < 3500 K, with a dominance of low activity stars close t
 o the transition between partially- and fully-convective stars and a rise 
 in activity down into the fully-convective regime.
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