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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 112 176 Habitability Outcomes
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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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?
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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
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 18-Jul-2008