BEGIN:VCALENDAR
VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:0
UID:UW-Physics-Event-4807
DTSTART:20180426T203000Z
DTEND:20180426T220000Z
DTSTAMP:20260417T100043Z
LAST-MODIFIED:20180412T155136Z
LOCATION:4421 Sterling Hall\, Coffee and cookies 3:30 PM. Talk starts 
 at 3:45 PM
SUMMARY:Star formation\, polarization\, and magnetic fields in the ALM
 A era\, Astronomy Colloquium\, Chat Hull\, NAOJ Fellow\, NAO of Japan\
 , NAPJ Chile Observatory\, Joint Alma Observatory
DESCRIPTION:<br>
\nThe results from the ALMA polarization system have 
 begun both to expand and to confound our understanding of the role of 
 the magnetic field in low-mass star formation.  After a brief motivati
 on via CARMA\, SMA\, and other polarization observations from the prio
 r decade\, I will discuss new ALMA results\, including the highest res
 olution and highest sensitivity polarization images made to date of tw
 o very young\, Class 0 protostellar sources.  These new observations a
 chieve ~140 AU resolution\, allowing us to probe polarization -- and t
 hus magnetic field orientation -- in the innermost regions surrounding
  the protostars.  First is a Class 0 protostellar source in Serpens kn
 own as Ser-emb 8\, where a comparison with cutting-edge\, moving-mesh 
 AREPO simulations suggests that cloud-scale turbulence -- not a large-
 scale magnetic field preserved from the source's natal cloud -- is dic
 tating the magnetic field morphology immediately surrounding the proto
 star.  In contrast\, in the second source\, known as Serpens SMM1\, th
 e magnetic field has clearly been shaped by the bipolar outflow emanat
 ing from the central source -- a situation that is quite different fro
 m the turbulence-dominated morphology of Ser-emb 8.  Finally\, I will 
 show recent observations of polarization toward IM Lup\, a much more e
 volved\, Class II protoplanetary disk.  In the case of IM Lup\, consis
 tent with previous observations of other disks\, the polarization appe
 ars to be due to scattering by dust grains\, thus complicating the sea
 rch for magnetic fields in disks\, but opening up a new window into du
 st grain growth and evolution.
URL:https://www.physics.wisc.edu/events/?id=4807
END:VEVENT
END:VCALENDAR