HD 128311
14 36 00.5607
+09 44 47.4536
16.6
0.828
0.73
7.51
8.441
6.895
6.425
5.772
5.30
5.142
0.08
K0V
HD 128311 b
TYC 910-165-1 b
Gaia DR2 1176209886733406592 b
HIP 71395 b
GJ 3860 b
Confirmed planets
1.83
460.1
0.30
-76.2
259.2
63.8
This planetary system is most likely in a 2:1 mean motion resonance. The inner planet orbits the star exactly twice during one orbit of the outer planet. This is a very stable configuration. Mean motion resonances help us to understand the formation of multiplanteray systems. The existense of this resonance is a strong indication that interactions with the protoplanetary disk migrated the planets to their current positions. A detailed analysis of the HD 128311 system shows that there also had to be non-adiabatic effects during the migration phase such as a third planet (Sandor and Kley 2006) or turbulence in the protoplanetary disk (Rein and Papaloizou 2009).
RV
15/01/08
2002
177.7
HD 128311 c
TYC 910-165-1 c
Gaia DR2 1176209886733406592 c
HIP 71395 c
GJ 3860 c
Confirmed planets
3.20
910.7
0.12
-19.7
184.2
63.8
This planetary system is most likely in a 2:1 mean motion resonance. The inner planet orbits the star exactly twice during one orbit of the outer planet. This is a very stable configuration. Mean motion resonances help us to understand the formation of multiplanteray systems. The existense of this resonance is a strong indication that interactions with the protoplanetary disk migrated the planets to their current positions. A detailed analysis of the HD 128311 system shows that there also had to be non-adiabatic effects during the migration phase such as a third planet (Sandor and Kley 2006) or turbulence in the protoplanetary disk (Rein and Papaloizou 2009).
RV
15/01/08
2005
140.7
HD 128311
TYC 910-165-1
Gaia DR2 1176209886733406592
HIP 71395
GJ 3860
4965.0
Boötes