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PRODID:UW-Madison-Physics-Events
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SEQUENCE:0
UID:UW-Physics-Event-8222
DTSTART:20230314T230000Z
DURATION:PT1H0M0S
DTSTAMP:20260414T055038Z
LAST-MODIFIED:20230309T163709Z
LOCATION:Join Zoom Meeting https://berkeley.zoom.us/j/91230714547  Mee
 ting ID: 912 3071 4547
SUMMARY:Neutron star mass and radius constrained from the magnetar QPO
 s\, Network in Neutrinos\, Nuclear Astrophysics\, and Symmetries (N3AS
 ) Seminar\, Hajime Sotani
DESCRIPTION:Quasi-periodic oscillations (QPOs) observed in giant flare
  from the magnetar\, which is a strongly magnetized neutron star\, are
  crucial information for extracting the neutron star properties. To th
 eoretically explain the QPOs newly observed in GRB 200415A\, we system
 atically examine the crustal torsional oscillations. Then\, we find th
 at the observed QPOs can be identified with several overtones of crust
 al oscillations\, if the value of the combination of the nuclear satur
 ation parameters\, $\\varsigma$\, is well-selected\, depending on the 
 neutron star mass and radius. Thus\, we can inversely constrain the ne
 utron star mass and radius for GRB 200415A by comparing to the appropr
 iate range of $\\varsigma$ expected with the fiducial value of nuclear
  saturation parameters obtained from the terrestrial experiments. We f
 urther make the neutron star mass and radius constraint more severe by
  assuming that the neutron star radius is almost the same as that for 
 the neutron star model\, whose central density is twice the nuclear sa
 turation density. The resultant neutron star models are consistent wit
 h the constraints obtained from the other astronomical and experimenta
 l observations.<br>\n** Please note the special time of 6 PM CDT **
URL:https://www.physics.wisc.edu/events/?id=8222
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