/ftp/cats/J_A+A/519//A10



==========================================================================
J/A+A/519/A10       Radial velocity curve of HD 202206       (Couetdic+, 2010)
The following files can be converted to FITS (extension .fit or fit.gz)
	hd202206.dat
==========================================================================
Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/519/A10
==========================================================================

drwxr-xr-x 12 cats archive 215 Nov 5 2018 [Up] drwxr-xr-x 2 cats archive 257 Jan 12 2023 [TAR file] -rw-r--r-- 1 cats archive 468 Dec 19 2022 .message -r--r--r-- 1 cats archive 4045 Oct 3 2010 ReadMe -r--r--r-- 1 cats archive 2944 Apr 8 2010 hd202206.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/A+A/519/A10 Radial velocity curve of HD 202206 (Couetdic+, 2010) ================================================================================ Dynamical stability analysis of the HD 202206 system and constraints to the planetary orbits. Couetdic J., Laskar J., Correia A.C.M., Mayor M., Udry S. <Astron. Astrophys. 519, A10 (2010)> =2010A&A...519A..10C ================================================================================ ADC_Keywords: Stars, double and multiple ; Planets ; Radial velocities Keywords: stars: individual: HD202206 - planetary systems - methods: numerical - techniques: radial velocities - celestial mechanics Abstract: Long-term, precise Doppler measurements with the CORALIE spectrograph have revealed the presence of two massive companions to the solar-type star HD 202206. Although the three-body fit of the system is unstable, it was shown that a 5:1 mean motion resonance exists close to the best fit, where the system is stable. It was also hinted that stable solutions with a wide range of mutual inclinations and low O-C were possible. We present here an extensive dynamical study of the HD 202206 system, aiming at constraining the inclinations of the two known companions, from which we derive possible value ranges for the companion masses. Description: We consider each inclination and one of the longitudes of ascending node as free parameters. For any chosen triplet of these parameters, we compute a new fit. Then we study the long-term stability in a small (in terms of O-C) neighborhood using Laskar's frequency map analysis. We also introduce a numerical method based on frequency analysis to determine the center of libration mode inside a mean motion resonance. The best orbital solution for the HD202206 is: ------------------------------------------------------------- V0 [km/s] 14.729 +/- 0.001 ------------------------------------------------------------- Inner planet Outer planet ------------------------------------------------------------- P [d] 256.389+/-0.044 1397.445+/-19.056 K [m/s] 564.82+/-1.42 38.08+/-1.21 e 0.431+/-0.001 0.104+/-0.024 a [AU] 0.8053 2.4832 i [deg] 90 90 m [MJup] 16.59 2.179 ------------------------------------------------------------- Objects: ------------------------------------------------ RA (2000) DE Designation(s) ------------------------------------------------ 21 14 57.8 -20 47 21 HD 202206 = HIP 104903 ------------------------------------------------