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Binary Evolution and Its Applications Binary Evolution and its Applications Zhanwen HAN Yunnan Observatories of the CAS Collaborators: X. Chen, L. Li, F. Zhang, B. Wang, X. Meng, D. Jiang, H. Ge, Y. Han, H. Chen, Z. Liu, J. Liu, S. Yu R. Webbink, Ph. Podsiadlowski, A. Lynas-Gray, L. Yungelson, M. Gilfanov, T.E. Wood, G. Stephan, 22-Mar-2018 KIAA 1 1 …… Outline • Binary evolution • Binary-related objects • Evolutionary population synthesis • Future perspectives 22-Mar-2018 KIAA 2 Outline • Binary evolution • Binary-related objects • Evolutionary population synthesis • Future perspectives 22-Mar-2018 KIAA 3 Stellar evolution 22-Mar-2018 KIAA 4 Half of the stars are in binaries 50% in binaries Duchêne & Kraus 2013 , ARA&A 22-Mar-2018 KIAA 5 Binary interaction dominates the evolution of massive stars Sana et al 2012 Sci 22-Mar-2018 KIAA 6 Binary Evolution 22-Mar-2018 KIAA 7 Stable RLOF WD MS 22-Mar-2018 KIAA 8 Dynamically unstable RLOF CE Ejection Merger WD MS 22-Mar-2018 KIAA 9 Binary Evolution Flow Chart 22-Mar-2018 KIAA 10 Binary evolution produces extotic objects Type Ia double BH Double degenerates supernovae Blue stragglers X-ray binaries Bipoar PNe 22-Mar-2018 KIAA 11 Basic problems: Dynamically unstable RLOF Stable RLOF CE CE ejection Merger 22-Mar-2018 KIAA 12 Basic problems: mass transfer stability? CE evolution? 22-Mar-2018 KIAA 13 RLOF Stabilility criterion models • Polytropic model (Hjellming+ 1987, Webbink 1988) • detailed binary evolution calculation model (Pavlovskii+ 2015, 2017) • Adiabatic mass loss model (Ge+ 2010, 2015) 22-Mar-2018 KIAA 14 Mass transfer in Binaries Critical equipotential surface Roche lobe radius： L1 q=M1/M2 Eggleton, 1983, ApJ loser M1 accretor M2 Response of the loser VS Response of the Roche lobe ln R1 ln R1 ln RL th |th | L lnM |RLOF lnM1 ad lnM1 ad 1 ( ad , th ) L Nuclear Timescale MT（driven by nuclear burning） ad L th Thermal timescale MT（driven by recovery of thermal equilibrium） L ad Dynamical timescale MT（constrained by hydrostatic equilibrium only) Stellar Structure Equations in the adiabatic Equations mass loss model hydrostatic equilibrium Mass continuity Adiabatic assumption ln R1 | ad lnM1 ad Energy equations Ge+, 2010 Dynamical timescale MT 22-Mar-2018L ad KIAA 16 Response of a 1.00M⊙ star to adiabatic mass loss 22-Mar-2018 KIAA 17 qc for FGB or AGB donors Ge+, 2015 Ge+, in prep Before: qc~1 CE only AGB Now: from 1.4-5 Radius Log Both CE and RLOF HG MS FGB Non-conservative 22-Mar-2018 KIAA Log Mass 18 Common Envelope Evolution (CEE) 22-Mar-2018 KIAA Ivanova 19 Common Envelope Evolution 抛射 SPH simulations are difficult ! merger ejection 22-Mar-2018 KIAA 20 Common Envelope Evolution Parameterized ! CEE orb E bind E gr thEth E E gr and th are integrated for the envelope 22-Mar-2018 KIAA 21 Outline • Binary evolution • Binary-related objects • Evolutionary population synthesis • Future perspectives 22-Mar-2018 KIAA 22 ELM WDs : Extremely low-mass white dwarfs Brown+, 2010, ApJ gravity 5< log g < 7 8000 K < Teff <22000 K M < 0.25-0.3 M☉ 22-Mar-2018 Effective temperature 23 Period distribution Observations I.The ELM Survey (Brown, Kilic et al. 2009--, SAO, 6.5 m MMT) • 88 ELM WDs, of which 76 being in binaries • Half of the observed binaries will merge in less than 6Gyr Brown et al. 2016, ApJ II. The WASP Project Maxted et al. • The 1st sample: 1SWASP J024743.37-251549.2 ( 2011 MNRAS) • Multiple-period pulsations (2013, Nature) • 17 EL CVn-type binaries (2014, MNRAS) III.Kepler transit • The first two：KOI-74, KOI-81 (van Kerkwijk+,2010) occultation • 7 objects in total (Rappaport+,2015, Guo+, 2017) Light Curve KOI-74 VI. ELM in MSPs (>10) Istrate+, 2014, 2016 22-Mar-2018 KIAA 24 The pre-ELM WD instability strip Diven by He++,He+, H+ 1SWASP J024743.37-251549.2 l=0 l=1 Corsico+, 2016, A&A l=2 CO-core Maxted+, 2013, Nature ZZ Ceti stars KIC 9164561 CO-core ZZ Ceti stars Zhang,X.+, 2016, ApJ 22-Mar-2018 KIAA Gianninas+, 2016, ApJ 25 Formation of extremely low-mass WDs Binary Evolution common envelope ejection stable mass transfer Beyond but very close to the bifurcation period 22-Mar-2018 KIAA 26 ELM WD mass VS orbital period (for 62 double degenerates) Z. Li,+ 22-Mar-2018 ELMKIAA WD Mass 27 EL CVn-type Binaries A/F dwarf star + proto-He WD Maxted et al. 2014 , MNRAS The hot small companion: extremely low mass （~0.2Msun) transit in an evolutionary phase that should be rare observed The hot small companion 17 EL CVn-type binaries have been found has been occulted. by Maxted et al. from the WASP observations. 22-Mar-2018 KIAA 28 The formation of EL CVn-type binaries Parameter space Chen X. et al 2017 , MNRAS, 464, 1874 Evolutionary tracks Predictions: More EL CVn-type binaries will be found in the Galaxy. The are more likely in the thin disk. 22-Mar-2018 KIAA 29 (The peak mass for the progenitors is in ~1.1-1.3Msun) Predictions of the model Introduction for the model Space density : in line with Chen et al. 22-Mar-2018 Position : as suggested/predictedKIAA by Chen et al. 30 KIC 8262223 Z. Guo, D. Gies, R. Mstson et al (2017, ApJ) ellipsoidal deep eclipses ● delta Scuti pulsation ● 31 Eclipsing Binary Millisecond Pulsars Discovered by Fermi Two distinct populations The masses of the companions are very low, then they should be small. How to produce the eclipses ?ta periods between 0.1 and de Both populations have orbital periods between 0.1 and 1.0 days, 22their-Mar-2018 companion masses differKIAA by an order of magnitude.Why?32 Chen H., Chen X., Tauris, Han, 2013, ApJ, 775, 27 Pulsar irradiation and evaporation of the companions are crucial for the formation of eclipsing MSPs The determining factor for the producing the two populations is the efficiency of the irradiation process. 22-Mar-2018 KIAA 33 widely accepted in this field Dick Manchester 《Physics of neutron stars and Related objects》（2017, JApA, 38, 42）： 22-Mar-2018 KIAA 34 SNe Ia Thermonuclear Explosions of CO WDs at ~1.4Msun carbon ignition under degenerate conditions thermonuclear runaway 51 incineration and complete destruction of the star 10 ergs 22-Mar-2018 KIAA 35 Phillips Relation (Phillips, 1993): empirical Luminosity 22-Mar-2018 KIAA time 36 SNe Ia as distance indicators 22-Mar-2018 KIAA 37 Accretion of WDs The mass of CO WDs at birth is less than ~1.1Msun . (~0.6Msun) Accretion is necessary for final explosions . How to accrete ? and when to explode ? 22-Mar-2018 KIAA 38 Maximum CO WD mass at birht: 1.1Msol Chen+ 2014, MNRAS When does C ignition occur ? Tmax ↑ while keeping ρ constant. Mwd=0.8Msol tb tc tcool=10^8 yrs tcool=10^9yrs CO WD structure during accretion Chen+ 2014 22-Mar-2018 KIAA 40 Progenitor models of SNe Ia Single-degenerate (SD) channel: accreting from non-degenerate companion CO WD + MS CO WD + RG CO WD + He Star Double-degenerate (DD) channel: Two CO WDs with a combined mass greater than 1.4Msun merge CO WD + CO WD Credit: GSFC/Dana Berry 22-Mar-2018 KIAA 41 Helium donor channel (WD+He) Wang+ 2009, 2010 Birthrate Time delay Properties of Progenitors Properties of remnant stars …… Sun MW centre US 708 Explain young SNe Ia Hypervelocity star 22-Mar-2018 Geier+, 2015, Science 42 SN Ia rates for single star burst Wang+ 2010 Observations: Totani+ 2008 22-Mar-2018 KIAA 43 Stellar mass double BHs Massive binary evolution is the key scenario for their formation CE evolution Contact binary evolutin GC dynamics ~218 Gpc-3yr-1 ~10 Gpc-3yr-1 ~6.5 Gpc-3yr-1 ~1000 yr-1by second LIGO ~500 yr-1 by second LIGO VFTS 352: 29 Msun+29 Msun with P=1.12 d 44 Observation Theory 22-Mar-2018 KIAA 45 Distributions of masses, mass ratios, orbital periods of Galactic DWDs with BPS approach double WDs M1 M2 M1 log(P) q Han 1998 log(P) 22-Mar-2018 KIAA 46 Spectral density of GW amplitude LISA 22-Mar-2018 KIAA 47 Resolvable DWDs with LISA S/N=5 S/N=1 Liu+ 2009, ApJ 22-Mar-2018 KIAA 48 Resolvable NS+WD,NS+NS, BH+NS,BH+BH with eLISA eLISA LISA 22-Mar-2018 KIAA Liu+ 2014 49 Blue stragglers Temperature Temperature HR diagram 22-Mar-2018 KIAA 50 Chen+ Sills+ 22-Mar-2018 KIAA 51 Two blue stragglers sequences in M30 Ferraro+, 2009, Nature ZAMS Binary evolution collision 22-Mar-2018 KIAA 52 Binary evolution may produce both of the sequences Blue sequence Red sequences 22-Mar-2018 KIAA 53 Blue stragglers with BPS Red points: observed BSs in M30 Red circles: addition BSs Jiang+, 2017, ApJ 22-Mar-2018 KIAA 54 hot subdwarf stars RHB BHB He L hot subdwarfs EHB M ~ 0.5M⊙ T Menv 0.02M⊙ Extreme Horizontal Branch stars 22-Mar-2018 KIAA 55 Binary model: stable RLOF 22-Mar-2018 KIAA 56 Binary model: CE ejection 22-Mar-2018 KIAA 57 Binary model: He WD merger 22-Mar-2018 KIAA 58 The model can reproduce: • (Log P, Mcomp) • (Teff, log g) • P • Log (g/Teff^4) • Mass function • Birthrate • Number density • Fraction of sdB+MS • Fraction of close sdB binaries • …… 22-Mar-2018 KIAA 59 Predictions: sdB binaries with long orbital periods Larger mass range 22-Mar-2018 KIAA 60 Outline • Binary evolution • Binary-related objects • Evolutionary population synthesis • Future perspectives 22-Mar-2018 KIAA 61 What is EPS? Evolutionary Population Synthesis (EPS) is an approach to derive the physical parameters of stellar populations of galaxies from the Spectral Energy Distributions(SEDs) observed.
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