Long-term precise Doppler measurements with the CORALIE spectrograph reveal
the presence of a second planet orbiting the solar-type star HD202206. The
radial-velocity combined fit yields companion masses of m_2\sini = 17.4 M_Jup
and 2.44 M_Jup, semi-major axes of a = 0.83 AU and 2.55 AU, and eccentricities
of e = 0.43 and 0.27, respectively. A dynamical analysis of the system further
shows a 5/1 mean motion resonance between the two planets. This system is of
particular interest since the inner planet is within the brown-dwarf limits
while the outer one is much less massive. Therefore, either the inner planet
formed simultaneously in the protoplanetary disk as a superplanet, or the outer
Jupiter-like planet formed in a circumbinary disk. We believe this singular
planetary system will provide important constraints on planetary formation and
migration scenarios.Comment: 9 pages, 14 figures, accepted in A&A, 12-May-200

A. C. M. Correia

D. Naef

D. Queloz

F. Pepe

Flower

Halbwachs

J. Laskar

Laskar

Laughlin

M. Mayor

Mayor

Mazeh

N. C. Santos

Nelson

S. Udry

Santos

Schaerer

Udry

English

arXiv

International audienceWe report precise Doppler measurements of HD 142022 obtained during the past six years with the CORALIE echelle spectrograph at La Silla Observatory together with a few additional observations made recently with the HARPS echelle spectrograph. Our radial velocities reveal evidence of a planetary companion with an orbital period P=1928+53-39 days, an eccentricity e=0.53+0.23-0.18, and a velocity semiamplitude K=92+102-29 m s-1. The inferred companion minimum mass is M_2 sin{i}=5.1+2.6-1.5 {M}_Jup and the semimajor axis a=3.03 ± 0.05 AU. Only one full orbital revolution has been monitored yet, and the periastron passage could not be observed since the star was too low on the horizon. The eccentricity and velocity semiamplitude remain therefore quite uncertain and the orbital solution is preliminary. HD 142022 is a chromospherically inactive K0 dwarf, metal rich relative to the Sun, and is the primary component of a wide binary. HD 142022 b is thus a new "planet in binary" candidate, and its high eccentricity might be due to secular interactions with the distant stellar companion

Eggenberger, A.

Mayor, M.

Naef, D.

Pepe, F.

Queloz, D.

Santos, N. C.

Udry, S.

Lovis, C.

Hal - Université Grenoble Alpes

The CORALIE survey for southern extrasolar planets. XIV. HD 142022 b: a long-period planetary companion in a wide binary

HAL: Hyper Article en Ligne

International audienceLong-term precise Doppler measurements with the CORALIE spectrograph reveal the presence of a second planet orbiting the solar-type star HD 202206. The radial-velocity combined fit yields companion masses of m2sin i=17.4 MJup and 2.44 MJup, semi-major axes of a=0.83 AU and 2.55 AU, and eccentricities of e=0.43 and 0.27, respectively. A dynamical analysis of the system further shows a 5/1 mean motion resonance between the two planets. This system is of particular interest since the inner planet is within the brown-dwarf limits while the outer one is much less massive. Therefore, either the inner planet formed simultaneously in the protoplanetary disk as a superplanet, or the outer Jupiter-like planet formed in a circumbinary disk. We believe this singular planetary system will provide important constraints on planetary formation and migration scenarios

Correia, Alexandre C. M.

Udry, Stéphane

Mayor, Michel

Laskar, Jacques

Naef, Dominique

Pepe, Francesco

Queloz, Didier

Santos, Nuno C.

HAL-OBSPM

The CORALIE survey for southern extra-solar planets. XIII. A pair of planets around HD 202206 or a circumbinary planet?

HAL-INSU

We report precise Doppler measurements of HD 142022 obtained 
 during the past six years with the CORALIE echelle spectrograph at La Silla 
 Observatory together with a few additional observations made recently with
 the HARPS echelle spectrograph. Our radial velocities reveal evidence of a planetary companion 
 with an orbital period $P=1928^{+53}_{-39}$ days, an eccentricity 
 $e=0.53^{+0.23}_{-0.18}$, and a velocity semiamplitude $K=92^{+102}_{-29}$ m s-1. The inferred companion minimum mass is $M_2\sin{i}=5.1^{+2.6}_{-1.5}~{M}_{\rm Jup}$ 
 and the semimajor axis $a=3.03$ ± 0.05 AU. 
 Only one full orbital revolution has been monitored yet, and the 
 periastron passage could not be observed since the star was too low on the
 horizon. The eccentricity and velocity semiamplitude remain therefore quite 
 uncertain and the orbital solution is preliminary. 
 HD 142022 is a chromospherically inactive K0 dwarf, metal rich relative to
 the Sun, and is the primary component of a wide binary. HD 142022 b 
 is thus a new “planet in binary” candidate, and its high eccentricity might 
 be due to secular interactions with the distant stellar companion

A pair of planets around HD 202206 or a circumbinary planet?

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