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J/ApJ/832/183  Binary stellar evolution data for Kepler systems  (Kostov+, 2016)

Tatooine's future: the eccentric response of Kepler's circumbinary planets to common-envelope evolution of their host stars. Kostov V.B., Moore K., Tamayo D., Jayawardhana R., Rinehart S.A. <Astrophys. J., 832, 183-183 (2016)> =2016ApJ...832..183K (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Models, evolutionary Keywords: binaries: close; binaries: eclipsing; methods: numerical; planetary systems; stars: individual: (Kepler-47, -1647); techniques: photometric Abstract: Inspired by the recent Kepler discoveries of circumbinary planets orbiting nine close binary stars, we explore the fate of the former as the latter evolve off the main sequence. We combine binary star evolution models with dynamical simulations to study the orbital evolution of these planets as their hosts undergo common-envelope (CE) stages, losing in the process a tremendous amount of mass on dynamical timescales. Five of the systems experience at least one Roche-lobe overflow and CE stage (Kepler-1647 experiences three), and the binary stars either shrink to very short orbits or coalesce; two systems trigger a double-degenerate supernova explosion. Kepler's circumbinary planets predominantly remain gravitationally bound at the end of the CE phase, migrate to larger orbits, and may gain significant eccentricity; their orbital expansion can be more than an order of magnitude and can occur over the course of a single planetary orbit. The orbits these planets can reach are qualitatively consistent with those of the currently known post-CE, eclipse-time variations circumbinary candidates. Our results also show that circumbinary planets can experience both modes of orbital expansion (adiabatic and nonadiabatic) if their host binaries undergo more than one CE stage; multiplanet circumbinary systems like Kepler-47 can experience both modes during the same CE stage. Additionally, unlike Mercury orbiting the Sun, a circumbinary planet with the same semimajor axis can survive the CE evolution of a close binary star with a total mass of 1M. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 113 760 Binary Stellar Evolution (BSE) results for the entire set of simulations for all Kepler systems table5.dat 69 11 Kepler system default initial parameters
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) J/AJ/151/68 : Kepler Mission. VII. Eclipsing binaries in DR3 (Kirk+, 2016) J/ApJ/831/64 : Mass-metallicity relation for giant planets (Thorngren+, 2016) J/MNRAS/455/4136 : Kepler triples (Borkovits+, 2016) J/ApJS/211/2 : Revised properties of Q1-16 Kepler targets (Huber+, 2014) J/A+A/574/A116 : G and K giant stars stellar parameters (Reffert+, 2015) J/ApJ/810/157 : V471 Tau system: RVs and BVRI LCs (Vaccaro+, 2015) J/ApJ/768/127 : Q1-11 Kepler light curve of KIC 4862625 (Schwamb+, 2013) J/ApJ/766/19 : XRB pop. synthesis models in 0<z<20 gal. (Tremmel+, 2013) J/ApJ/764/41 : X-ray binary evolution across cosmic time (Fragos+, 2013) J/MNRAS/428/1656 : Time of minima of HD 181068 (Borkovits+, 2013) J/other/Sci/337.1511 : Kepler-47 transits (Orosz+, 2012) J/other/Nat/481.475 : RVs of Kepler-34b & Kepler-35b (Welsh+, 2012) J/ApJS/190/1 : A survey of stellar families (Raghavan+, 2010) Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 10 A10 --- Name Kepler system name 12- 15 F4.2 Msun MA [0.6/1.6] Primary star, initial mass 17- 20 F4.2 Msun MB [0.2/1.1] Secondary star, initial mass 22- 26 F5.3 [Sun] Z [0.009/0.03] Metallicity 28- 31 F4.1 --- alpha [0.5/10] Common Envelope (CE) efficiency parameter 33- 36 A4 --- TCP Tides model applied (1) 38- 48 A11 --- deKool de Kool CE Model: ON/OFF (always "DE KOOL OFF") (2) 50- 59 F10.4 Myr Time [0/25000] Evolutionary time 61- 65 F5.3 Msun M1 [0/2.5] Current mass, Primary star 67- 71 F5.3 Msun M2 [0/1.1] Current mass, Secondary star 73- 74 I2 --- K1 [1/15] Current Stellar Type, Primary star (3) 76- 77 I2 --- K2 [0/15]? Current Stellar Type, Secondary star (3) 79- 84 F6.3 Rsun a [0/49.3] Binary orbit, abin 86- 90 F5.2 --- e [0/0.6]?=-1 System eccentricity ebin 92- 97 F6.3 --- R1 [0/8.8]?=-1 Fraction of Roche lobe filled, Primary 99-104 F6.3 --- R2 [0/2]?=-1 Fraction of Roche lobe filled, Secondary 106-113 A8 --- Evol Evolutionary Stage (4)
Note (1): Tides model applied as follows: TCP = Tidal Circularization Path. Tides "ON" in BSE; NTCP = No Tidal Circularization Path. Tides "OFF" in BSE. Note (2): The BSE code also allows an alternate CE model to be used, the de Kool CE evolution model (de Kool 1990ApJ...358..189D), which first introduced the CE evolution binding energy factor λ. See section 2. Note (3): Stellar Type (from Table 2) as follows: 0 = Deeply or fully convective low-mass MS star; 1 = Main Sequence star; 2 = Hertzsprung Gap (HG); 3 = First Giant Branch (GB); 4 = Core Helium Burning (CHeB); 5 = First/Early Asymptotic Giant Branch (EAGB); 6 = Second/Thermally Pulsing Asymptotic Giant Branch (TPAGB); 7 = Main Sequence Naked Helium star (HeMS); 8 = Hertzsprung Gap Naked Helium star (HeHG); 9 = Giant Branch Naked Helium Star (HeGB); 10 = Helium White Dwarf (HeWD); 11 = Carbon/Oxygen White Dwarf (COWD); 12 = Oxygen/Neon White Dwarf (ONeWD); 13 = Neutron Star (NS); 14 = Black Hole (BH); 15 = Massless Supernova/Massless Remnant. Note (4): Evolutionary Stage (from Table 3) as follows: INITIAL = Initial configuration; KW CHNGE = Stellar type change; BEG RCHE = Begin Roche lobe overflow; END RCHE = End Roche lobe overflow; CONTACT = Contact system; COELESCE = Coalescence of stars; COMENV = Common-envelope system; GNTAGE = New giant star from CE; appropriate age and initial mass set to match core-mass and stellar mass; NO REMNT = No remnant; MAX TIME = Max evolutionary time reached; end of program; DISRUPT = System is disrupted; BEG SYMB = Begin symbiotic system; END SYMB = End symbiotic system; BEG BSS = Begin blue stragglers.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 11 A11 --- Name Kepler system name 13 A1 --- f_Name [ac] Flag on Name (1) 15- 22 I8 --- KIC [4862625/12644769] Kepler ID number 24- 27 F4.2 Msun M1 [0.6/1.6] Primary mass 29- 34 F6.4 Msun M2 [0.2/1.1] Secondary mass 36- 41 F6.3 d Pbin [7.4/41.1] Binary period 43- 46 F4.2 --- e [0.02/0.6] Binary eccentricity ebin 48- 52 F5.3 [Sun] Z [0.009/0.4] Metallicity Z 53 A1 --- f_Z [b] Flag on Z (1) 55- 61 F7.2 d Pcbp [49.5/1107.6] Circumbinary planet period, PCBP 63- 66 F4.2 --- ecbp [0.01/0.2] Eccentricity of the circumbinary planet, eCBP 68- 69 A2 --- n_ecbp Note on ecbp (2)
Note (1): Flag as follows: a = J. Orosz (2016, private communication). b = BSE allows maximum metallicity of Z=0.03. c = Kepler-1647 Note (2): P1/P2/P3 have 60%/15%/85% probability to become dynamically unstable within 1Myr after the Common Envelope phase.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 27-Feb-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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