J/ApJ/764/18 Characteristic frequencies of giant exoplanets (Le Bihan+, 2013)
Pulsation frequencies and modes of giant exoplanets.
Le Bihan B., Burrows A.
<Astrophys. J., 764, 18 (2013)>
=2013ApJ...764...18L 2013ApJ...764...18L
ADC_Keywords: Models ; Planets
Keywords: methods: numerical; planets and satellites: fundamental parameters;
planets and satellites: general; planets and satellites: interiors
Abstract:
We calculate the eigenfrequencies and eigenfunctions of the acoustic
oscillations of giant exoplanets and explore the dependence of the
characteristic frequency ν0 and the eigenfrequencies on several
parameters: the planet mass, the planet radius, the core mass, and the
heavy element mass fraction in the envelope. We provide the
eigenvalues for degree l up to 8 and radial order n up to 12. For the
selected values of l and n, we find that the pulsation
eigenfrequencies depend strongly on the planet mass and radius,
especially at high frequency. We quantify this dependence through the
calculation of the characteristic frequency ν0 which gives us an
estimate of the scale of the eigenvalue spectrum at high frequency.
For the mass range 0.5MJ≤MP≤15MJ, and fixing the planet radius
to the Jovian value, we find that ν0∼164.0x(MP/MJ)0.48µHz,
where MP is the planet mass and MJ is Jupiter's mass. For the
radius range from 0.9 to 2.0RJ, and fixing the planet's mass to the
Jovian value, we find that ν0∼164.0x(RP/RJ)-2.09µHz,
where RP is the planet radius and RJ is Jupiter's radius. We
explore the influence of the presence of a dense core on the pulsation
frequencies and on the characteristic frequency of giant exoplanets.
We find that the presence of heavy elements in the envelope affects
the eigenvalue distribution in ways similar to the presence of a dense
core. Additionally, we apply our formalism to Jupiter and Saturn and
find results consistent with both the observational data of
Gaulme et al. (2011A&A...531A.104G 2011A&A...531A.104G) and previous theoretical work.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table6.dat 32 170 Characteristic frequency ν0 for a set of
coreless models using the estimated radius and
mass of detected giant exoplanets
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See also:
J/A+A/565/A55 : CoRoT 105906206 frequencies analysis (da Silva+, 2014)
J/A+A/543/A45 : Planets around metal-poor stars (Mortier+, 2012)
J/ApJ/727/102 : On the frequency of Jupiter analogs (Wittenmyer+, 2011)
J/ApJ/697/544 : Planets orbiting metal-poor dwarfs. II. (Sozzetti+, 2009)
http://www.exoplanet.eu/ : The Extrasolar Planets Encyclopaedia
Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Name Planet designation
14- 18 F5.3 Rjup Rad [0.7/2.1] Planet radius (1)
20- 25 F6.3 Mjup Mass [0.1/30] Planet mass (1)
27- 32 F6.2 uHz nu0 [33.5/815.6] Characteristic frequency ν0 (2)
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Note (1): Estimated radii and masses have been taken from
http://www.exoplanet.eu/
Note (2): We calculate the characteristic frequency ν0 for each object,
using the techniques and models developed and described in Sections 2
and 3. The characteristic frequency ν0 (in µHz) is defined in
Provost et al. (1993A&A...274..595P 1993A&A...274..595P) using the equation (5) detailed
in section 3.1. The helium mass fraction is fixed at 0.25 in the
entire envelope and no core is added.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 23-Oct-2014