2011A&A...528A.112L


Query : 2011A&A...528A.112L

2011A&A...528A.112L - Astronomy and Astrophysics, volume 528A, 112-112 (2011/4-1)

The HARPS search for southern extra-solar planets. XXVIII. Up to seven planets orbiting HD 10180: probing the architecture of low-mass planetary systems.

LOVIS C., SEGRANSAN D., MAYOR M., UDRY S., BENZ W., BERTAUX J.-L., BOUCHY F., CORREIA A.C.M., LASKAR J., LO CURTO G., MORDASINI C., PEPE F., QUELOZ D. and SANTOS N.C.

Abstract (from CDS):

Low-mass extrasolar planets are presently being discovered at an increased pace by radial velocity and transit surveys, which opens a new window on planetary systems. We are conducting a high-precision radial velocity survey with the HARPS spectrograph, which aims at characterizing the population of ice giants and super-Earths around nearby solar-type stars. This will lead to a better understanding of their formation and evolution, and will yield a global picture of planetary systems from gas giants down to telluric planets. Progress has been possible in this field thanks in particular to the sub-m/s radial velocity precision achieved by HARPS. We present here new high-quality measurements from this instrument. We report the discovery of a planetary system comprising at least five Neptune-like planets with minimum masses ranging from 12 to 25M, orbiting the solar-type star HD 10180 at separations between 0.06 and 1.4AU. A sixth radial velocity signal is present at a longer period, probably caused by a 65-M object. Moreover, another body with a minimum mass as low as 1.4M may be present at 0.02AU from the star. This is the most populated exoplanetary system known to date. The planets are in a dense but still well separated configuration, with significant secular interactions. Some of the orbital period ratios are fairly close to integer or half-integer values, but the system does not exhibit any mean-motion resonances. General relativity effects and tidal dissipation play an important role to stabilize the innermost planet and the system as a whole. Numerical integrations show long-term dynamical stability provided true masses are within a factor ∼3 from minimum masses. We further note that several low-mass planetary systems exhibit a rather ``packed'' orbital architecture with little or no space left for additional planets. In several cases, semi-major axes are fairly regularly spaced on a logarithmic scale, giving rise to approximate Titius-Bode-like (i.e. exponential) laws. These dynamical architectures can be interpreted as the signature of formation scenarios where type I migration and interactions between protoplanets play a major role. However, it remains challenging to explain the presence of so many Neptunes and super-Earths on non-resonant, well-ordered orbits within ∼1-2AU of the central star. Finally, we also confirm the marked dependence of planet formation on both metallicity and stellar mass. Very massive systems are all found around metal-rich stars more massive than the Sun, while low-mass systems are only found around metal-deficient stars less massive than the Sun.

Abstract Copyright:

Journal keyword(s): planets and satellites: detection - stars: individual: HD 10180 - techniques: radial velocities - techniques: spectroscopic

VizieR on-line data: <Available at CDS (J/A+A/528/A112): table1.dat>

Simbad objects: 31

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Number of rows : 31
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 4308 PM* 00 44 39.2675256910 -65 38 58.282490370 7.31 7.193 6.552     G6VFe-0.9 224 1
2 * ups And PM* 01 36 47.84216 +41 24 19.6443 4.70 4.64 4.10 3.64 3.35 F9V 904 1
3 HD 10180 * 01 37 53.5773715933 -60 30 41.485438420   7.95 7.32     G1V 163 2
4 HD 10180h Pl 01 37 53.5773715933 -60 30 41.485438420           ~ 15 1
5 HD 10180f Pl 01 37 53.5773715933 -60 30 41.485438420           ~ 10 1
6 HD 10180e Pl 01 37 53.5773715933 -60 30 41.485438420           ~ 13 1
7 HD 10180g Pl 01 37 53.5773715933 -60 30 41.485438420           ~ 16 1
8 HD 10180d Pl 01 37 53.5773715933 -60 30 41.485438420           ~ 16 1
9 HD 10180c Pl 01 37 53.5773715933 -60 30 41.485438420           ~ 17 1
10 HD 10180b Pl? 01 37 53.5773715933 -60 30 41.485438420           ~ 13 1
11 HD 14810 * 02 22 20.8869808451 -32 57 07.089191891   8.78 8.35     F3V 11 0
12 HD 37124 PM* 05 37 02.4866790656 +20 43 50.834619370   8.35   7.2   G4IV-V 275 2
13 HD 40307 PM* 05 54 04.2409953924 -60 01 24.491747849 8.814 8.097 7.147 6.597 6.119 K2.5V 215 1
14 HD 40307b Pl 05 54 04.2409953924 -60 01 24.491747849           ~ 46 1
15 HD 45364 PM* 06 25 38.4744251424 -31 28 51.428476346   8.82 8.06     G8V 106 1
16 HD 47186 PM* 06 36 08.7879198906 -27 37 20.266866013   8.36 7.63     G6V 115 1
17 CoRoT-7 * 06 43 49.4690410679 -01 03 46.825797768   12.78 11.73 11.36 10.87 K0V 178 1
18 CoRoT-7b Pl 06 43 49.4690410679 -01 03 46.825797768           ~ 366 1
19 HD 69830 PM* 08 18 23.9469692487 -12 37 55.810202572   6.74 5.95     G8:V 477 1
20 HD 74156 PM* 08 42 25.1221445320 +04 34 41.146391815       7.2   G1V 208 2
21 * rho01 Cnc PM* 08 52 35.8113282132 +28 19 50.956901366 7.45 6.82   5.4   K0IV-V 1009 1
22 HD 90156 PM* 10 23 55.2739374820 -29 38 43.906618411 7.758 7.603 6.920 6.534 6.189 G5V 107 1
23 * 61 Vir PM* 13 18 24.3142756 -18 18 40.304648 5.710 5.440 4.740     G6.5V 609 1
24 HD 125612 PM* 14 20 53.5176697825 -17 28 53.488801800   8.93 8.32     G3V 97 1
25 BD-07 4003e Pl 15 19 26.8271336166 -07 43 20.190958776           ~ 68 1
26 BD-07 4003 BY* 15 19 26.8271336166 -07 43 20.190958776 13.403 11.76 10.560 9.461 8.911 M3V 557 2
27 NAME G 139-21b Pl 17 15 18.9337265994 +04 57 50.064695682           ~ 581 1
28 * mu. Ara PM* 17 44 08.7036342277 -51 50 02.591049123   5.85 5.15     G3IV-V 482 2
29 HD 181433 PM* 19 25 09.5672280149 -66 28 07.676289768   9.42 8.38     K3III-IV 107 1
30 HD 202206 PM* 21 14 57.7684954746 -20 47 21.162361638   8.79 8.07     G6V 200 1
31 BD-15 6290 BY* 22 53 16.7323107416 -14 15 49.303409936 12.928 11.749 10.192 9.013 7.462 M3.5V 888 1

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2021.07.31-11:04:18

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