J/MNRAS/445/4395 Fundamental properties of giant gas planets (Yildiz+, 2014)
On the structure and evolution of planets and their host stars - effects of
various heating mechanisms on the size of giant gas planets.
Yildiz M., Celik Orhan Z., Kayhan C., Turkoglu G.E.
<Mon. Not. R. Astron. Soc., 445, 4395-4405 (2014)>
=2014MNRAS.445.4395Y 2014MNRAS.445.4395Y (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Stars, masses ;
Effective temperatures
Keywords: planets and satellites: interiors - planet-star interactions -
stars: evolution - stars: interior - stars: late type
Abstract:
It is already stated in the previous studies that the radius of the
giant planets is affected by stellar irradiation. The confirmed
relation between radius and incident flux depends on planetary mass
intervals. In this study, we show that there is a single relation
between radius and irradiated energy per gram per second (l-),
for all mass intervals. There is an extra increase in radius of
planets if l- is higher than 1100 times energy received by the
Earth (l{earth}). This is likely due to dissociation of
molecules. The tidal interaction as a heating mechanism is also
considered and found that its maximum effect on the inflation of
planets is about 15 percent. We also compute age and heavy element
abundances from the properties of host stars, given in the TEPCat
catalogue (Southworth). The metallicity given in the literature is as
[Fe/H]. However, the most abundant element is oxygen, and there is a
reverse relation between the observed abundances [Fe/H] and [O/Fe].
Therefore, we first compute [O/H] from [Fe/H] by using observed
abundances, and then find heavy element abundance from [O/H]. We also
develop a new method for age determination. Using the ages we find, we
analyse variation of both radius and mass of the planets with respect
to time, and estimate the initial mass of the planets from the
relation we derive for the first time. According to our results, the
highly irradiated gas giants lose 5 percent of their mass in every
1Gyr.
Description:
The data are taken from the TEPCat data base (Southworth 2011;
www.astro.keele.ac.uk/jkt/tepcat/) for the transiting planetary
systems in 2014 January 6, and listed in tablea1.dat.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 121 184 Fundamental properties of the giant gas planets and
their host stars (the data are taken from TEPCat)
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See also:
www.astro.keele.ac.uk/jkt/tepcat : TEPCat data base
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Planet Planet name
15- 18 F4.2 Msun Mass Host star mass
20- 23 F4.2 Rsun Rad Host star radius
25- 28 I4 K Teff Host star effective temperature
30- 35 F6.4 AU a Semi-major axis
37- 43 F7.3 d Per Period
45- 50 F6.3 --- e Eccentricity
51 A1 --- n_e [a] Note on e (1)
53- 57 F5.2 Mjup Mp Planetary mass
59- 62 F4.2 Rjup Rp Planetary radius
64- 67 I4 K Teq ?=- Equilibrium temperature
69- 72 I4 --- FI Incident flux (in Earth units)
74- 77 I4 --- e_FI rms uncertainty on FI (in Earth units)
79- 83 I5 --- l- Energy received per unit mass per unit time
(in l0 units)
85- 88 I4 --- e_l- rms uncertainty on l- (in l0 units)
90- 93 F4.1 [10-7W] log(dE/dt) ? Rate of energy dissipation due to tidal
interaction
95- 98 F4.1 [10-7W] e_log(dE/dt) ? rms uncertainty on log(dE/dt)
101-104 F4.1 Gyr Age ? Age (2)
106-109 F4.1 Gyr e_Age ? rms uncertainty on Age
111-115 F5.3 --- Z0 Metallicity (2)
117-121 F5.3 --- e_Z0 rms uncertainty on Z0
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Note (1): a: eccentricities are taken from Knutson et al. (2014ApJ...785..126K 2014ApJ...785..126K).
Note (2): computed from stellar properties (see Section 3).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 21-May-2015