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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:4
UID:UW-Physics-Event-5451
DTSTART:20200623T203000Z
DURATION:PT1H0M0S
DTSTAMP:20260415T023555Z
LAST-MODIFIED:20200622T142204Z
LOCATION:https://berkeley.zoom.us/j/91922781599
SUMMARY:On the minimum radius of very massive neutron stars\, Network 
 in Neutrinos\, Nuclear Astrophysics\, and Symmetries (N3AS) Seminar\, 
 Sophia Han\, Ohio U.
DESCRIPTION:Prospects of establishing the radii of massive neutron sta
 rs in PSR
\nJ1614-2230 and PSR J0740+6620 from NICER and Chandra obser
 vatories hold
\nthe potential to constrain the equation of state (EoS)
  of matter to
\ndensities well beyond those encountered in canonical s
 tars of mass ¡­ 1.4
\nM¢Á. In this work\, we investigate the relat
 ion between the radii of very
\nmassive neutron stars up to the maximu
 m mass\, Mmax\, supported by dense
\nmatter EoSs. Results from models 
 with hadronic matter are contrasted with
\nthose that include a first-
 order hadron-to-quark phase transition. We find
\nthat a lower bound o
 n Mmax with an upper bound on the radius of massive
\npulsars serves t
 o rule out too soft quark matter\, and an upper bound on
\nMmax with a
  lower bound on the radius of massive pulsars strongly
\ndisfavors a t
 ransition into too-stiff quark matter appearing at low
\ndensities. Th
 e complementary role played by radius inferences from future
\ngravita
 tional wave events of inspiraling binary neutron stars is also
\nbrief
 ly discussed.
URL:https://www.physics.wisc.edu/events/?id=5451
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