2018A&A...620A..85O


C.D.S. - SIMBAD4 rel 1.7 - 2020.06.03CEST01:49:39

2018A&A...620A..85O - Astronomy and Astrophysics, volume 620A, 85-85 (2018/12-1)

Orbital properties of binary post-AGB stars.

OOMEN G.-M., VAN WINCKEL H., POLS O., NELEMANS G., ESCORZA A., MANICK R., KAMATH D. and WAELKENS C.

Abstract (from CDS):

Binary post-asymptotic giant branch (post-AGB) stars are thought to be the products of a strong but poorly understood interaction during the AGB phase. The aim of this contribution is to update the orbital elements of a sample of galactic post-AGB binaries observed in a long-term radial-velocity monitoring campaign by analysing these systems in a homogeneous way. Radial velocities are computed from high signal-to-noise spectra via a cross-correlation method. The radial-velocity curves are fitted by using both a least-squares algorithm and a Nelder-Mead simplex algorithm. We use a Monte Carlo method to compute uncertainties on the orbital elements. The resulting mass functions are used to derive a companion mass distribution by optimising the predicted to the observed cumulative mass-function distributions, after correcting for observational bias. As a result, we derive and update orbital elements for 33 galactic post-AGB binaries, among which 3 are new orbits. The orbital periods of the systems range from 100 to about 3000 days. Over 70% (23 out of 33) of our binaries have significant non-zero eccentricities ranging over all periods. Their orbits are non-circular even though the Roche-lobe radii are smaller than the maximum size of a typical AGB star and tidal circularisation should have been strong when the objects were on the AGB. We derive a distribution of companion masses that is peaked around 1.09M with a standard deviation of 0.62M. The large spread in companion masses highlights the diversity of post-AGB binary systems. Post-AGB binaries are often chemically peculiar, showing in their photospheres the result of an accretion process of circumstellar gas devoid of refractory elements. We find that only post-AGB stars with high effective temperatures (>5500K) in wide orbits are depleted in refractory elements, suggesting that re-accretion of material from a circumbinary disc is an ongoing process. It appears, however, that depletion is inefficient for the closest orbits irrespective of the actual surface temperature.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: AGB and post-AGB - binaries: spectroscopic - circumstellar matter

VizieR on-line data: <Available at CDS (J/A+A/620/A85): table1.dat rv/*>

Status at CDS:  

Simbad objects: 35

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Number of rows : 35

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 BD+46 442 * 01 45 47.0309135946 +46 49 00.940007737   10.02 9.46     F2III 17 0
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5617 1
3 V* TW Cam pA* 04 20 47.6362030815 +57 26 28.517663334 12.12 11.42 10.08 9.29   G8Ib 62 0
4 V* AY Lep pA* 05 22 59.4223189375 -20 32 53.046745853   10.52 9.48     ~ 22 0
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14752 1
6 V* DY Ori RV* 06 06 14.9086299520 +13 54 19.144206036   11.709 11.29     ~ 44 0
7 IRAS 06165+3158 * 06 19 50.6234720193 +31 56 58.181120564           ~ 5 0
8 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 714 0
9 V* V382 Aur pA* 06 37 52.4275241570 +53 31 01.954746267   9.54 9.04     F7IV: 117 0
10 IRAS 06452-3456 * 06 47 01.1373048381 -34 59 55.884330870           ~ 3 0
11 V* ST Pup pA* 06 48 56.4137309745 -37 16 33.336632924   10.47 9.28 9.89 9.29 G2I 80 0
12 V* PS Gem pA* 07 03 39.6306725638 +10 46 13.076555664   7.76 7.37     A0 105 0
13 V* V421 CMa pA* 07 16 08.2750839195 -23 27 01.536617548   11.16 10.73     F5 21 0
14 V* U Mon RV* 07 30 47.4734611972 -09 46 36.788534824 8.22 7.00 5.82     G8/K0Ib/II 192 0
15 CD-44 4961 pA* 08 56 14.1790943091 -44 43 10.710041643   10.55 9.176     F3e 56 1
16 IRAS 09144-4933 RV* 09 16 09.6357192580 -49 46 12.091844704     11.1     M4/S? 17 0
17 HD 89353 pA* 10 18 07.5892879413 -28 59 31.194541133   5.76 5.53     B9.5Ib/II 286 0
18 V* V802 Car pA* 11 02 04.3151180751 -62 09 42.834842337   9.57 8.90 9.38   F2III 48 0
19 V* RU Cen RV* 12 09 23.8147186123 -45 25 34.813401164   9.81 8.70     G1Ie 86 0
20 V* SX Cen RV* 12 21 12.5740806517 -49 12 41.059392756   10.11 9.60     B5III 65 0
21 HD 108015 pA* 12 24 53.5038403586 -47 09 07.498401573   8.379 7.96     F3/5Ib/II 55 0
22 V* EN TrA pA* 14 57 00.6830179855 -68 50 22.901317885   9.42 8.70     F2Ib 64 0
23 IRAS 15469-5311 pA* 15 50 43.8045787663 -53 20 43.254393089   12.03 10.66     F3 21 0
24 V* V1333 Sco pA* 16 26 20.3836937817 -34 17 12.912826289   12.38 11.41     F8 16 0
25 CD-48 11445 pA* 17 07 36.6576312333 -48 19 08.476517172   12.33 10.55     G2p(R) 28 0
26 V* V340 Ser RV* 17 30 46.9250020324 -11 22 08.314111714   10.51 9.68     F2/3II 31 0
27 * 89 Her pA* 17 55 25.1884459710 +26 02 59.970100296 5.36 5.70 5.36 5.06 4.94 F2Ibp 385 0
28 V* AC Her pA* 18 30 16.2374666779 +21 52 00.618442618 8.00 7.79 7.01     F4Ibp 315 0
29 BD+03 3950 RV* 19 15 01.1800400072 +03 48 42.640112771   11.16 10.37     F8 31 0
30 V* V677 Lyr LP* 19 15 12.1374762768 +39 42 50.489355356   10.75 10.13   10.441 F2IIe 19 0
31 V* EP Lyr pA* 19 18 19.5565673262 +27 51 03.077324082   11.22 9.96 10.14   G2II 76 1
32 BD-02 4931 pA* 19 18 22.7164743400 -02 42 10.880951310   11.55 10.78     B1III 29 0
33 V* HP Lyr pA* 19 21 39.0675162741 +39 56 08.200273318   11.12 10.38 10.15 9.615 A3Ia/Iab 49 1
34 V* HM Aqr pA* 22 35 27.5256072315 -17 15 26.885199823 9.31 9.08 8.90     A0III 99 0
35 BD+39 4926 pA* 22 46 11.2279685924 +40 06 26.304627650   9.43 9.29     B8 113 0

    Equat.    Gal    SGal    Ecl

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2020.06.03-01:49:39

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