G02 - New insights into the dynamics of planets in
P-Type motion around binaries
B. Funk, S. Eggl, M. Gyergyovits, R. Schwarz, E. Pilat-Lohinger
Institute for Astronomy - University of Vienna
Name
Mass [MSun]
aBin [AU]
# Planets
a [AU]
HU Aqr A
0.88
0.0039
2
3.6
HU Aqr B
0.2
NN Ser A
0.535
NN Ser B
0.111
HW Vir A
0.485
HW Vir B
0.142
DP Leo A
0.6
DP Leo B
0.1
5.4
0.0043
2
3.39, 3.07
5.38, 5.66
0.004
2
3.62
5.3
0.0027
1
8.2
HU Aqr
HW
Vir
HWVir
HUAqr
60
10
0
50
-10
40
-20
Dynamical studies:
-30
-40
20
]
U
y[A
]
U
y[A
30
-50
10
-60
• Eclipse timing variations – is it possible-70to detect the systems by ETV?
0
-80
-10
-20
-15
-90
-10
-5
0
5
x [AU]
10
15
20
25
-100
-20
0
20
40
x [AU]
60
80
100
120
NN Ser
NN Ser 2b
Ser 2a
• DynamicalNNstability
– are the proposed systems
long-term stable?
8
60
50
6
40
4
30
2
]
U
y[A
]
U
y[A
20
10
-2
0
-4
-10
-6
-20
-30
-60
0
-50
-40
-30
-20
x [AU]
-10
0
10
20
-8
-8
-6
-4
-2
0
x [AU]
2
4
6
8
Conclusion and Outlook
•
The current proposed data lead to unstable motion for two systems
(HU Aqr and HW Vir)
• Taking into account the error bars (best cases) showed, that the
systems HU Aqr, HW Vir are still unstable
• Investigations of inclined orbits of the planets (i = 0° - 50°, ∆i = 10°)
lead also to unstable motion in the systems HU Aqr, HW Vir
•
NN Ser:
– We found unstable and stable motion (for an integration time of 500000
years)
– The same is also valid for inclined orbits
•
Outlook
– The next step will be to investigate how the initial conditions have to be
changed to lead to stable motion of the planets