BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//CERN//INDICO//EN
BEGIN:VEVENT
SUMMARY:A continuous wave window into neutron star structure
DTSTART;VALUE=DATE-TIME:20261107T093000Z
DTEND;VALUE=DATE-TIME:20261107T100000Z
DTSTAMP;VALUE=DATE-TIME:20261023T124343Z
UID:indico-contribution-2976@indico.itp.ac.cn
DESCRIPTION:Speakers: Ayush Hazarika (International Centre for Theoretical
  Physics Asia-Pacific (ICTP-AP)\, University of Chinese Academy of Science
 s)\nEvery rapidly spinning neutron star with slight asymmetry would broadc
 ast a continuous hum of gravitational waves (GW). None of these signals ha
 s been detected yet\, but the silence itself is measurable: searches now s
 et upper limits on the GW amplitude of dozens of known pulsars\, and for a
  growing subset those limits dig below the energy budget available from th
 e stars’ own spin-down. We ask what this kind of data\, can say about th
 e interior of a neutron star. The amplitude of the continous signal depend
 s on how much matter the star carries in its deformation and how that matt
 er is distributed\, its moment of inertia\, which in turn is fixed by the 
 unknown equation of state of dense matter. This opens a route to the neutr
 on star mass-radius relation that is fully independent of the X-ray pulse-
 profile and binary-merger measurements that anchor current constraints. We
  build a hierarchial Bayesian pipeline that propagates simulated amplitude
  limits\, treated consistently as non-detections\, through stellar-structu
 re calculations to the mass-radius plane\, marginalizing over the unknown 
 deformations of the pulsar population. Rather than claiming a new measurem
 ent\,\nwe chart the sensitivity frontier: how deep continuous-wave searche
 s must go before they begin to weigh in on dense matter on their own.\n\nh
 ttps://indico.itp.ac.cn/event/417/contributions/2976/
LOCATION:
URL:https://indico.itp.ac.cn/event/417/contributions/2976/
END:VEVENT
END:VCALENDAR