LindaHolyoke Mentor:Dr.ErikSchnetter MeganMiller - PowerPoint PPT Presentation

Linda
Holyoke
 
Mentor:
Dr.
Erik
Schnetter
 Megan
Miller
 
Mentor:
Dr.
Peter
Diener



Brief
Overview
  Black
Holes
and
Neutron
Stars
  Gravitational
Waves
and
Gamma‐Rays
  General
Relativity/Methods
  Purpose
of
Research
  Research
Goals


[1]


Black
Holes
and
Neutron
Stars
 Formation:
massive
star
 collapse
–
Supernova!!
 Black
Hole
 Neutron
Star
 Mass
 >3
solar
masses
 1.4~3
solar
masses
 Density
 ∞
 2~4
x
10^14
times
ρ sun
 Escape
Velocity
 ∞
 33%
speed
of
light
 [2]


Black
Hole
Geometry
 [3]


Gravitational
Waves

 






 

 
 
  What
they
are
–
in
theory?
  Why
do
we
care?
  
What
do
we
think
will
create
them?
  How
do
we
detect
them?

  LIGO
(Laser

 Interferometer
Gravitational
 Wave
Observatory)
 [4]


Gamma‐Rays
  Long
Gamma‐Ray
Bursts
vs.
Short
Gamma‐ Ray
Bursts
(SGRB)
  SGRB
mechanisms:




NS‐NS
collision
 BH‐NS
encounter
  Most
energetic

 events
in
universe
 [5]
 
 



General
Relativity
  Why
we
need
to
consider
it?
  Curvature
of
Space‐time
  Einstein
Toolkit
/
Cactus


Project
Goals
 Black
Hole
–
Black
Hole:
 1) Will
two
black
holes
in
parabolic
orbit
create
 gravitational
waves
that
are
detectable?

 2) Depending
on
the
size,
how
far
away
can
we
 detect
gravitational
waves?


Project
Goals
 Neutron
Star
–
Black
Hole:
 1) Will
the
neutron
star
form
an
accretion
disk
 around
the
black
hole?
 2) Will
this
disk
survive
as
long
as
the
duration
 of
observed
SGRBs?


Initial
Conditions
 Periastron
Distance
 Initial
Configuration
 Black
Hole
–
Black
Hole
 Black
Hole
–
Neutron
Star
 Mass
1
(solar
masses)
 0.5
 4.51


 Mass
2
(solar
masses)
 0.5
 1.4
 Initial
separation
(km)
 100
 100
 Periastron
distance
(km)
 2.21
 20.1


Initial
Conditions
 Results:
 Black
Hole
–

 Black
Hole
–
 Black
Hole
 Neutron
Star
 Mass
1
 Mass
2
 Mass
1
 Mass
2
 x
–position

(km)
 50
 ‐50
 24
 ‐76
 ‐2.66*10 7
 8.56*10 7
 v x 

(m/s)
 ‐2.55*10 7
 2.55*10 7
 ‐3.84*10 6
 1.33*10 7
 v y 
(m/s) 
 3.84*10 6
 ‐4.29*10 7
 v total
 
(m/s) 
 2.58*10 7
 2.58*10 7
 2.97*10 7
 9.58*10 7


Upcoming
Weeks
  Setup
Parameter
File
  Start
Simulations
  Hope
for
the
best
  Fix
errors
and
rerun
  Adjust
initial
conditions
based
on
results
of
 first
simulations


Works
Cited
 Illustrations:

 [1]
http://imagine.gsfc.nasa.gov/docs/science/know_l1/supernovae.html
 [2]
 http://spacefellowship.com/wp‐content/uploads/2009/07/ supernova_p0901xx_01hr‐300x200.jpg
 [3]
 http://theory.uwinnipeg.ca/users/gabor/black_holes/images/ slide8.gif
 [4]
http://www.phys.ufl.edu/~price/binary‐wave.jpg
 [5]
 http://www.nasa.gov/images/content/ 55961main_MM_image_feature_132_jw4.jpg


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