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J/ApJ/835/209  Orbital nature of 81 ellipsoidal red giant binaries  (Nie+, 2017)

The orbital nature of 81 ellipsoidal red giant binaries in the Large Magellanic Cloud. Nie J.D., Wood P.R., Nicholls C.P. <Astrophys. J., 835, 209-209 (2017)> =2017ApJ...835..209N (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Stars, double and multiple ; Stars, giant ; Radial velocities ; Stars, diameters Keywords: binaries: close; Magellanic Clouds; stars: AGB and post-AGB Abstract: In this paper, we collect a sample of 81 ellipsoidal red giant binaries in the Large Magellanic Cloud (LMC), and we study their orbital natures individually and statistically. The sample contains 59 systems with circular orbits and 22 systems with eccentric orbits. We derive orbital solutions using the 2010 version of the Wilson-Devinney code (Wilson & Devinney 1971ApJ...166..605W ; Wilson 1979ApJ...234.1054W, 1990ApJ...356..613W ; Wilson+ 2009, J/ApJ/702/403). The sample is selection-bias corrected, and the orbital parameter distributions are compared to model predictions for the LMC and to observations in the solar vicinity. The masses of the red giant primaries are found to range from about 0.6 to 9M with a peak at around 1.5M, in agreement with studies of the star formation history of the LMC, which find a burst of star formation beginning around 4 Gyr ago. The observed distribution of mass ratios q=m2/m1 is more consistent with the flat q distribution derived for the solar vicinity by Raghavan+ (2010, J/ApJS/190/1) than it is with the solar vicinity q distribution derived by Duquennoy & Mayor (1991A&A...248..485D). There is no evidence for an excess number of systems with equal mass components. We find that about 20% of the ellipsoidal binaries have eccentric orbits, twice the fraction estimated by Soszynski+ (2004, J/AcA/54/347). Our eccentricity evolution test shows that the existence of eccentric ellipsoidal red giant binaries on the upper parts of the red giant branch (RGB) can only be explained if tidal circularization rates are ∼1/100 the rates given by the usual theory of tidal dissipation in convective stars. Description: The I-band light curve data we use are mainly from OGLE II (Udalski+ 1997AcA....47..319U; Soszynski+ 2004, J/AcA/54/347; Szymanski 2005AcA....55...43S), sometimes supplemented by OGLE III data if it is published. The radial velocities are provided by Nie & Wood (2014, J/AJ/148/118) for 79 ellipsoidal variables, by Nicholls+ (2010, J/MNRAS/405/1770) for their 11 ellipsoidal variables, and by Nicholls & Wood (2012, J/MNRAS/421/2616) for their 7 eccentric binaries. The light curve photometry, supplemented by K-band photometry from the Two Micron All Sky Survey (2MASS) catalog (Cutri+ 2003, II/246), provides the K magnitude and the I-K color. We adopted LMC distance modulus (DM) of 18.49 (de Grijs+ 2014AJ....147..122D) and reddening E(B-V)=0.08 (Keller & Wood 2006ApJ...642..834K). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 170 81 Orbital solution for each ellipsoidal variable
See also: II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) J/AJ/119/1448 : Improved properties for cool stars (Houdashelt+, 2000) J/AJ/119/1424 : Color-temperature relations of M giants (Houdashelt+, 2000) J/MNRAS/353/705 : OGLE Variables in Magellanic Clouds (Ita+, 2004) J/AcA/54/347 : IVB mag of LMC ellipsoidal variables (Soszinski+, 2004) J/A+A/484/815 : Scaled solar tracks and isochrones (Bertelli+, 2008) J/AJ/136/1242 : LMC long-period variables from MACHO (Fraser+, 2008) J/ApJ/702/403 : Photometric observations of V1197 Orionis (Wilson+, 2009) J/MNRAS/405/1770 : LMC red giants in E sequence (Nicholls+, 2010) J/ApJS/190/1 : A survey of stellar families (Raghavan+, 2010) J/MNRAS/421/2616 : LMC eccentric ellipsoidal red giant binaries (Nicholls+, 2012) J/ApJ/765/L41 : Asteroseismic classification of KIC objects (Stello+, 2013) J/AJ/148/118 : RV curves of LMC ellipsoidal variables (Nie+, 2014) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1 I1 --- Set [1/4] Sample (1) 3- 20 A18 --- OGLE OGLE II identifier (, J2000) 22- 26 F5.1 d Per [65.7/662.2] Orbital period 28- 31 I4 K Teff [3710/5046] Effective Temperature 33- 38 F6.1 d HJD0 Time of light minimum at superior conjunction; HJD-2450000.0 40- 42 F3.1 d e_HJD0 Uncertainty in HJD0 44- 48 F5.1 km/s Vgamma [212/351] System center of mass radial velocity 50- 52 F3.1 km/s e_Vgamma Uncertainty in Vgamma 54- 57 F4.1 deg i [27.9/90] Inclination (2) 59- 62 F4.1 deg e_i ? Uncertainty in i 64- 68 F5.1 Rsun a [122/601] Semi-major axis, in solar units 70- 73 F4.1 Rsun e_a Uncertainty in a 75- 79 F5.3 --- e [0.05/0.5]?=0 Eccentricity (3) 81- 85 F5.3 --- e_e ? Uncertainty in e 87- 91 F5.3 rad omega [0.3/7.2]? Argument of periastron, ω 93- 97 F5.3 rad e_omega ? Uncertainty in ω 99-103 F5.3 --- q [0.1/1.1] Mass ratio, q 105-109 F5.3 --- e_q Uncertainty in q 111-115 F5.3 --- Omega1 [2.2/6.3] Surface potential, primary, Ω1 117-121 F5.3 --- e_Omega1 Uncertainty in Ω1 123-126 F4.2 Msun Mass1 [0.5/9.4] Mass, primary 128-131 F4.2 Msun e_Mass1 Uncertainty in Mass1 133-136 F4.2 Msun Mass2 [0.09/5] Mass, secondary 138-141 F4.2 Msun e_Mass2 Uncertainty in Mass2 143-147 F5.1 Rsun Rad1 [40/161] Radius, primary 149-153 F5.1 Rsun RadL1 [54/284] Effective Roche lobe radius, primary 155-157 F3.1 Rsun Rad2 [0/3.1] Radius, secondary 159-164 F6.1 Lsun Lum1 [431/6433] Luminosity, primary 166-170 F5.1 Lsun Lum2 [0/807] Luminosity, secondary
Note (1): Sample as follows: 1 = Circular orbits, Nie & Wood (2014, J/AJ/148/118); 2 = Circular orbits, Nicholls et al. (2010, J/MNRAS/405/1770); 3 = Eccentric orbits, Nie & Wood (2014, J/AJ/148/118); 4 = Eccentric orbits, Nicholls & Wood (2012, J/MNRAS/421/2616). Note (2): A value of i=90 is an adopted value (see text). Note (3): Values of e=0.000 apply for systems assumed to have circular orbits.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 31-Aug-2017
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