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 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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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)
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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 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.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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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)
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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.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 27-Feb-2017