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J/ApJ/649/1010      Habitability of known exoplanetary systems    (Jones+, 2006)

Habitability of known exoplanetary systems based on measured stellar properties. Jones B.W., Sleep P.N., Underwood D.R. <Astrophys. J., 649, 1010-1019 (2006)> =2006ApJ...649.1010J
ADC_Keywords: Planets ; Binaries, orbits Keywords: astrobiology - planetary systems - planets and satellites: general Abstract: Habitable planets are likely to be broadly Earth-like in composition, mass, and size. Masses are likely to be within a factor of a few of the Earth's mass. Currently, we do not have sufficiently sensitive techniques to detect Earth-mass planets, except in rare circumstances. It is thus necessary to model the known exoplanetary systems. In particular, we need to establish whether Earth-mass planets could be present in the classical habitable zone (HZ) or whether the giant planets that we know to be present would have gravitationally ejected Earth-mass planets or prevented their formation. We have answered this question by applying computer models to the 152 exoplanetary systems known by 2006 April 18 that are sufficiently well characterized for our analysis. For systems in which there is a giant planet, inside the HZ, which must have arrived there by migration, there are two cases: (1) where the migration of the giant planet across the HZ has not ruled out the existence of Earth-mass planets in the HZ; and (2) where the migration has ruled out existence. For each case, we have determined the proportion of the systems that could contain habitable Earth-mass planets today, and the proportion for which this has been the case for at least the past 1000Myr (excluding any early heavy bombardment). For case 1 we get 60% and 50%, respectively, and for case 2 we get 7% and 7%, respectively. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 112 176 Habitability Outcomes
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Star Name 14 A1 --- n_Name [*] Note for systems with known inclination (1) 16- 20 F5.3 solMass Mstar Star mass 22- 29 A8 --- SpType MK spectral type and class 31- 36 F6.3 mag BC Bolometric correction 37 A1 --- l_Dist Limit flag on Dist 38- 45 F8.3 pc Dist Distance of the star 47- 51 F5.2 mag Vmag V magnitude (2) 54 A1 --- l_HZin Limit flag on HZinner 55- 60 F6.3 AU HZin ? Inner distance of habitable zone 62 A1 --- l_HZout Limit flag on HZouter 63- 70 F8.5 AU HZout ? Outer distance of habitable zone 72 A1 --- Pl Planet designation 76- 81 F6.3 jovMass Mpl Minimum Mass in Jupiter mass (1) 83- 89 F7.5 AU a Semi-major axis (1) 91- 96 F6.4 --- e Ellipticity (1) 98 I1 --- Conf [1,6]? Configuration (3) 100-101 I2 % Hab ? System Habitability Today (%) 102 A1 --- n_Hab [Y/N] (Y)es or (N)o when no percentage probability 104-112 A9 --- SusHab Sustained Habitability?
Note (1): The appropriate magnitude has been used to calculate L. A multiplier of 1.3 has been used to obtain the final three columns, except for planets with stars, denoted with *, for which i0 is known, always >81°, so the minimum mass is used. Note (2): The observed magnitudes of the OGLEs are I, not V, except for OGLE-TR-56. Note (3): There are 6 types of configuration of the habitability zone (HZ) due to the presence of a giant planet: 1,2 = an Earth-like planet could be confined throughout the HZ 3,4,5 = a fraction of the HZ offers confinement 6 = no possibility of confinement in the HZ
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 18-Jul-2008
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