2007A&A...464..779R


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.16CEST17:53:19

2007A&A...464..779R - Astronomy and Astrophysics, volume 464, 779-785 (2007/3-3)

The eccentricity-mass distribution of exoplanets: signatures of different formation mechanisms?

RIBAS I. and MIRALDA-ESCUDE J.

Abstract (from CDS):

We examine the distributions of eccentricity and host star metallicity of exoplanets as a function of their mass. Planets with Msini>4MJ have an eccentricity distribution consistent with that of binary stars, while planets with Msini≲4MJ are less eccentric than binary stars and more massive planets. In addition, host star metallicities decrease with planet mass. The statistical significance of both of these trends is only marginal with the present sample of exoplanets. To account for these trends, we hypothesize that there are two populations of gaseous planets: the low-mass population forms by gas accretion onto a rock-ice core in a circumstellar disk and is more abundant at high metallicities, and the high-mass population forms directly by fragmentation of a pre-stellar cloud. Planets of the first population form in initially circular orbits and grow their eccentricities later, and may have a mass upper limit from the total mass of the disk that can be accreted by the core. The second population may have a mass lower limit resulting from opacity-limited fragmentation. This would roughly divide the two populations in mass, although they would likely overlap over some mass range. If most objects in the second population form before the pre-stellar cloud becomes highly opaque, they would have to be initially located in orbits larger than ∼30AU, and would need to migrate to the much smaller orbits in which they are observed. The higher mean orbital eccentricity of the second population might be caused by the larger required intervals of radial migration, and the brown dwarf desert might be due to the inability of high-mass brown dwarfs to migrate inwards sufficiently in radius.

Abstract Copyright:

Journal keyword(s): planetary systems - planetary systems: formation - binaries: general - stars: low-mass, brown dwarfs - stars: formation

Simbad objects: 19

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Number of rows : 19

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 HD 18445 SB* 02 57 13.2012231419 -24 58 30.290781613   9.01 7.86     K2V 89 0
2 BD-04 782 SB* 04 15 09.5344264586 -04 25 06.381142715 11.755 10.561 9.332 8.591 7.953 K5V 48 0
3 HD 283750 BY* 04 36 48.2413370074 +27 07 55.898311812   9.354   7.4   K2.5Ve 250 2
4 HD 29587 SB* 04 41 36.3164521477 +42 07 06.420947055 7.940 7.890 7.280 6.74 6.39 G2V 136 1
5 HD 29587b BD? 04 41 36.3177 +42 07 06.493           ~ 9 1
6 HD 89707 SB* 10 20 49.9820182134 -15 28 47.680757393   7.74 7.19     G2VFe-1.5CH-0.8 121 0
7 HD 110833 SB* 12 44 14.5447567445 +51 45 33.372388151   7.98   6.4   K3 141 0
8 HD 112758 ** 12 59 01.5631121408 -09 50 02.648158707 8.737 8.384 7.588 7.163 6.729 G9V 158 1
9 HD 114762 SB* 13 12 19.7467346230 +17 31 01.611425890 7.78         F9VgF8mF4+M6?V 498 1
10 HD 127506 SB* 14 30 44.9753771297 +35 27 13.432952502   9.75   8.834   K3.5V 88 1
11 HD 137510 PM* 15 25 53.2707121018 +19 28 50.529629119   6.872 6.241     G0IV-V 93 0
12 HD 140913 SB* 15 45 07.4493001052 +28 28 11.743016199   8.664 8.053     G0V 83 0
13 HD 168443c Pl 18 20 03.9331764016 -09 35 44.609316076           ~ 85 1
14 HD 169822 SB* 18 26 10.0892926230 +08 46 39.282248976   8.52   7.4   G6V 91 0
15 * 59 Dra PM* 19 09 09.8793494721 +76 33 37.808283506   5.400 5.107     A7V 112 1
16 HD 184860 ** 19 36 45.63937 -10 26 36.3596   9.41 8.40     K2+K7 47 1
17 HD 202206b Pl 21 14 57.7684954746 -20 47 21.162361638           ~ 52 1
18 * eps Ind PM* 22 03 21.6542294981 -56 47 09.537018193   5.75 4.69     K5V 461 0
19 HD 217580 SB* 23 01 51.5437938421 -03 50 55.441795620 9.199 8.428 7.464 6.934 6.482 K3V 89 0

    Equat.    Gal    SGal    Ecl

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2019.10.16-17:53:19

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