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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 (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; for the transiting planetary systems in 2014 January 6, and listed in tablea1.dat. File Summary:
FileName Lrecl Records Explanations
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)
See also: : TEPCat data base Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
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
Note (1): a: eccentricities are taken from Knutson et al. (2014ApJ...785..126K). Note (2): computed from stellar properties (see Section 3).
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 21-May-2015
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