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SUMMARY:Magnetized accretion disks around Kerr black holes with scalar hai
 r
DTSTART;VALUE=DATE-TIME:20181213T113000Z
DTEND;VALUE=DATE-TIME:20181213T123000Z
DTSTAMP;VALUE=DATE-TIME:20260813T205002Z
UID:indico-contribution-10237@indico.ific.uv.es
DESCRIPTION:Speakers: Sergio Gimeno-Soler (UV)\nTesting the true nature of
  black holes – the no-hair hypothesis – will become increasingly more 
 precise in the next few years as new observational data is collected in bo
 th the gravitational wave channel and the electromagnetic channel. In this
  talk we will consider numerically generated spacetimes of Kerr black hole
 s with synchronised scalar hair and build stationary models of magnetized 
 thick disks (or tori) around them. Our approach assumes that the disks are
  not self-gravitating\, they obey a polytropic equation of state\, the dis
 tribution of their specific angular momentum is constant\, and they are ma
 rginally stable. Moreover\, contrary to existing approaches in the literat
 ure\, our models are thermodinamically relativistic\, as the specific enth
 alpy of the fluid can adopt values significantly larger than unity. We stu
 dy the dependence of the morphology and properties of the accretion tori o
 n the type of black hole considered\, from purely Kerr black holes with va
 rying degrees of spin parameter. Comparisons between the disk properties f
 or both types of black holes are presented. The sequences of magnetized\, 
 equilibrium disks models discussed in this study can be used as initial da
 ta for numerical relativity codes to investigate their dynamical (non-line
 ar) stability and used in tandem with ray-tracing codes to obtain syntheti
 c images of black holes (i.e. shadows) in astrophysically relevant situati
 ons where the light source is provided by an emitting accretion disk.\n\nh
 ttps://indico.ific.uv.es/event/3559/contributions/10237/
LOCATION:Campus Burjassot 4-4-4426 - Seminari Física Teòrica
URL:https://indico.ific.uv.es/event/3559/contributions/10237/
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