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PROBLEMS
IN GASEOUS HYDRODYNAMICS
MICHAŁ RÓŻYCZKANICOLAUS COPERNICUS ASTRONOMICAL CENTER
WARSAW, POLAND
PLANETARY NEBULAE AS ASTRONOMICAL TOOLSGDAŃSK, 28.06.2005
1. THE TEMPLATE:
2. PIECES OF THE PUZZLE:
TALK PLAN
• THE GENERIC NEBULA• ...AND SOME EXTRA FLAVOURS
• INTRODUCTION: 1-D HYDRO• 2-D WORLD• 3-D WORLD • SMALL-SCALE FEATURES• MHD
THE GENERIC NEBULA
SPHERICAL HALO
ORDERLY RINGS
A BIG MESS INSIDE
THE GENERIC NEBULA ...
VERY HOT GAS
(„HOT CAVITY”)
INTRODUCTION: 1-D HYDRO
forward shock
contact surface
reverse shock
shocked wind 1
shocked wind 2
free wind 1
freewind 2
CONTACT SURFACE FRAME
forward shock
contact surface
reverse shock
shocked wind 1
shocked wind 2
free wind 1
freewind 2
CONTACT SURFACE FRAME
forward shock
contact surface
reverse shock
shocked wind 1
shocked wind 2
free wind 1
freewind 2
FREE WIND 2 FRAME (=AMBIENT MEDIUM FRAME)
free fast wind
shocked fast wind
free AGB wind
shocked AGB wind
forward shock
reverse shock
contact surface
INTRODUCTION: 1-D HYDRO
INTRODUCTION: 1-D HYDRO
Balick, B. & Frank, A. 2002; ARAA 40, 439
fs
fsd
R
V
)()( Tn
T
Tn
e
e
e2th
th
thc
.
ll
a
wAfs t
LR
5
35
1
0
2
2
1www VML .
laa RR 0)(
)(adiabatic cd
INTRODUCTION: 1-D HYDRO
Balick, B. & Frank, A. 2002; ARAA 40, 439
www VM .
ll
a
wRfs tR
4
24
1
0
)(radiative cd
laa RR 0)(
fs
fsd
R
V
)()( Tn
T
Tn
e
e
e2th
th
thc
.
2-D WORLD: BASICS
10
2q
0
0
)(
)/(
)(),( FRR l0aa
ROTATION
BINARY INTERACTIONS
MAGNETIC FIELDS
Icke V. 1988; A&A 202, 177
2
1
0 )(2
1
hbfs P
t
RFOR SMALL DEPARTURES FROM SPHERICAL SYMMETRY:
reverse shock
forward shock
contact surface
shocked AGB wind
free AGB wind
shocked fast wind
free fast wind
2-D WORLD: BASICS
2-D WORLD: SHAPING - BIPOLARS
Garcia-Segura,G. et al. 1999; ApJ 517, p.767
Mslow=10-5 M/yr.
Mfast =10-7 M/yr.
q = 0.1veq
vpl
Vpl/ Veq = 3
2-D WORLD: COLLIMATION, JETS-I
Blandford, R. & Rees, M. 1974; MNRAS 169, 395 Norman, M., Smarr, L., Smith, M., & Wilson, J. 1981; ApJ 247, 52
Frank, A. & Mellema, G. 1996; ApJ 472, 684
2-D WORLD: COLLIMATION, JETS-I
3
Mw = 10-7 M/yr
Vw = 200 km/s
adiabatic
.
RS
CS
FS
Frank, A. & Mellema, G. 1996; ApJ 472, 684
2-D WORLD: COLLIMATION, JETS-I
Mw = 10-7 M/yr
Vw = 200 km/s
adiabatic
q = 70
.
a = 2.4 AU a = 12.6 AU
RG star: M*=1M; R*=0.7 AUsecondary: M*=0.6 M
RG wind: 10-6 M/yrfast wind: 10-8 M/yr; 103 km/s
3-D WORLD: BINARY, DENSE WIND SHAPING
Gawryszczak, A., Mikołajewska, J. & Różyczka, M. 2002; A&A 385, 205
3-D WORLD: BINARY, DENSE WIND SHAPING
Gawryszczak, A., Mikołajewska, J. & Różyczka, M. 2002; A&A 385, 205
Courtesy: Doris Folini & Rolf Walder
http://www.astro.phys.ethz.ch/staff/walder/
3-D WORLD: BINARY, DISK FORMATION
RW HyaRED GIANT: M=1.6M, R=1013 cm, M=10-7 M/yr WHITE DWARF: M=0.48 M, a=21013 cm
.
3-D WORLD: BINARY, DENSE WIND SHAPING
SYMBIOTIC BINARYCOOL STAR: M=1.4M, R=1013 cm, M=310-8 M/yr HOT STAR: M=0.6 M, a=31013 cm, M=410-9 M/yr
..
HIGH
LOW
Courtesy: Doris Folini & Rolf Walder http://www.astro.phys.ethz.ch/staff/walder/
3-D WORLD: BINARY, COMMON ENVELOPE EVOLUTION
Movies by Eric Sandquist;http://mintaka.sdsu.edu/faculty/erics/web/
red giant: 1 M with a 0.45 M core
companion: 0.35 M
3-D WORLD: BINARY, COMMON ENVELOPE EVOLUTION
Eric Sandquist;http://mintaka.sdsu.edu/faculty/erics/web/
3-D WORLD: BINARY, COMMON ENVELOPE EVOLUTION
De Marco, O. Et al. 2003; RevMexAA S.Conf. 18,24
1130 days170 days
2310 days 3250 days
AGB star
core 0.56 M
envelope 0.69 M
radius 1.85 AU
companion
mass 0.1 M
timesscale 9 yr
mass lost 4 %
AGB star
core 0.56 M
envelope 0.69 M
radius 1.85 AU
companion
mass 0.1 M
synchronous
timesscale 9 yr
mass lost 25 %
AGB star
core 0.60 M
envelope 0.44 M
radius 3.00 AU
companion
mass 0.1 M
timesscale 18 yr
mass lost 84 %
SMALL-SCALE FEATURES: COOLING INSTABILITY; R-T INSTABILITY
Movie: courtesy Doris Folini & Rolf Walder http://www.astro.phys.ethz.ch/staff/walder/
SMALL-SCALE FEATURES: RAYLEIGH-TAYLOR INSTABILITY
Movie: courtesy ASC / Alliances Center for Astrophysical Thermonuclear Flashes http://flash.uchicago.edu/website/research/gallery/home.py
g lighter fluid
denserfluid
density schematic:
simulation time: 3.1 sec
density range: 0.5 – 2.5 g/cm3
isotropic thermal pressure
nonisotropic ram pressure
SMALL-SCALE FEATURES: THIN SHELL INSTABILITY I
Vishniac, E. 1983; ApJ 274, 152
SMALL-SCALE FEATURES: THIN SHELL INSTABILITY I
shocked AGB wind
shocked fast wind
free AGB wind
forward shock
SMALL-SCALE FEATURES: THIN SHELL INSTABILITY II
Vishniac, E. 1994; ApJ 428, 186
nonisotropic ram pressure
nonisotropic ram pressure
SPHERICAL SYMMETRY: IONIZATION INSTABILITIES (?)
SPHERICAL SYMMETRY: RAYLEIGH-TAYLOR INSTABILITY
AXIAL SYMMETRY: KELVIN-HELMHOLTZ INSTABILITY
SMALL-SCALE FEATURES: THIN SHELL INSTABILITY II
Movie: courtesy Doris Folini & Rolf Walder http://www.astro.phys.ethz.ch/staff/walder/
SMALL-SCALE FEATURES: THIN SHELL INSTABILITY II
John Blondinhttp://wonka.physics.ncsu.edu/~blondin/aas196/page33.html
SMALL-SCALE FEATURES: IONIZED SHELL INSTABILITY
Garcia-Segura,G. et al. 1999; ApJ 517, p.767
Mslow=10-5 M/yr.
Mfast =10-7 M/yr.
Fion =1046 /s
MHD: WEAK FIELD, TOROIDAL PINCH ON RADIATIVELY DRIVEN WIND
Różyczka, M. & Franco, J. 1996; ApJ 469, p.L127
( B(2R*) = 2G )
Różyczka, M. & Franco, J. 1996; ApJ 469, p.L127
MHD: WEAK FIELD, TOROIDAL PINCH ON RADIATIVELY DRIVEN WIND
Różyczka, M. & Franco, J. 1996; ApJ 469, p.L127
MHD: WEAK FIELD, TOROIDAL PINCH ON MAGNETICALLY DRIVEN WIND
M* = 1 M
R* = 4.5 AU
spherical wind Mw = 10-6 M/yr
at R* toroidal field
of 0.1, 1 or 5 G
MHD: STRONG FIELD; „MAGNETIC EXPLOSION”
Matt, S. 2003; arXiv:astro-ph/0308548
dipole field anchored in the core; envelope ejected if
v*vAve−2 > 0.1
to match pPNe fields of 105–108 G are needed
MHD: STRONG FIELD; „MAGNETIC EXPLOSION”
Matt, S. 2003; arXiv:astro-ph/0308548
dipole field anchored in the core; envelope ejected if
v*vAve−2 > 0.1
to match pPNe fields of 105–108 G are needed