2022A&A...666A..40B


Query : 2022A&A...666A..40B

2022A&A...666A..40B - Astronomy and Astrophysics, volume 666A, 40 (2022/10-1)

The structure of jets launched from post-AGB binary systems.

BOLLEN D., KAMATH D., VAN WINCKEL H., DE MARCO O., VERHAMME O., KLUSKA J. and WARDLE M.

Abstract (from CDS):


Context. In this paper, we focus on post-asymptotic giant branch (post-AGB) binaries and study the interaction between the different components of these complex systems. These components comprise the post-AGB primary, a main sequence secondary, a circumbinary disk, as well as a fast bipolar outflow (jet) launched by the companion. We obtained well-sampled time series of high resolution optical spectra over the last decade and these spectra provide the basis of our study.
Aims. We aim to use the time-series data to quantify the velocity and density structure of the jets in nine of these post-AGB binaries. This complements our earlier work and this amounts to the analyses of 16 jet-launching systems in total.
Methods. The jet is detected in absorption, at superior conjunction, when the line of sight towards the primary goes through the bipolar cone. Our spectral time series scan the jets during orbital motion. Our spatio-kinematic model is constrained by these dynamical spectra. We complement this with a radiative-transfer model in which the Balmer series are used to derive total mass-loss rates in the jets.
Results. The jets are found to be wide (> 30°) and display an angle-dependent density structure with a dense and slower outer region near the jet cone and a fast inner part along the jet symmetry axes. The deprojected outflow velocities confirm that the companions are main sequence companions. The total mass-loss rates are large (10–8 - 10–5 M yr–1), from which we can infer that the mass-accretion rates onto the companion star must be high as well. The circumbinary disk is likely the main source for the accretion disk around the companion. All systems with full disks that start near the sublimation radius show jets, whereas for systems with evolved transition disks this lowers to a detection rate of 50%. Objects without an infrared excess do not show jets.
Conclusions. We conclude that jet creation in post-AGB binaries is a mainstream process. Our geometric spatio-kinematic model is versatile enough to model the variety of spectral time series. The interaction between the circumbinary disks and the central binary provide the needed accretion flow, but the presence of a circumbinary disk does not seem to be the only prerequisite to launch a jet.

Abstract Copyright: © D. Bollen et al. 2022

Journal keyword(s): stars: AGB and post-AGB - binaries: spectroscopic - circumstellar matter - stars: mass-loss - ISM: jets and outflows - accretion, accretion disks

Simbad objects: 22

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Number of rows : 22
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 BD+46 442 * 01 45 47.0311634664 +46 49 00.937724124   10.02 9.46     F2III 27 0
2 V* TW Cam pA* 04 20 47.6363454312 +57 26 28.522779504 12.12 11.42 10.08 9.29   G8Ib 71 0
3 V* RV Tau RV* 04 47 06.7239850584 +26 10 45.532913268   11.00 9.80     K3Ibe 279 1
4 V* AY Lep pA* 05 22 59.4229189104 -20 32 53.048251464   10.52 9.48     ~ 32 0
5 V* DY Ori WV* 06 06 14.9085939696 +13 54 19.118975940   12.956 11.503 11.030   ~ 51 1
6 V* SU Gem Mi* 06 14 00.0252211992 +27 42 12.186889416   11.70 10.19 11.92   F8/G0Ib 51 0
7 IRAS 06165+3158 LP? 06 19 50.6236629912 +31 56 58.174574928           ~ 9 0
8 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 765 0
9 V* V382 Aur pA* 06 37 52.4269199856 +53 31 01.958446992   9.585 9.295 9.078   F7IV: 133 0
10 V* PS Gem pA* 07 03 39.6305052432 +10 46 13.068774048   7.76 7.37     A0 120 0
11 V* V421 CMa pA* 07 16 08.2750036896 -23 27 01.536458868   11.16 10.73     F5 31 0
12 V* U Mon RV* 07 30 47.4711645432 -09 46 36.757477488 8.22 7.00 5.82     G8/K0Ib/II 206 0
13 HD 137569 pA* 15 26 20.8172517192 +14 41 36.321520992   7.86 7.91     B9Iab:p 103 0
14 * 89 Her pA* 17 55 25.1883476136 +26 02 59.968457664 5.36 5.70 5.36 5.06 4.94 F2Ibp 411 0
15 V* AC Her RV* 18 30 16.2373118976 +21 52 00.599340000 8.00 7.79 7.01     F4Ibp 340 0
16 BD+03 3950 RV* 19 15 01.1800830552 +03 48 42.641057988   11.16 10.37     F8 39 0
17 V* V677 Lyr LP* 19 15 12.1372704744 +39 42 50.490059760   10.75 10.13   10.441 F2IIe 28 0
18 V* EP Lyr RV* 19 18 19.5570243336 +27 51 03.082292928   11.22 9.96 10.14   G2II 87 1
19 V* HP Lyr pA* 19 21 39.0673459320 +39 56 08.202817716   11.12 10.38 10.15 9.615 A3Ia/Iab 59 1
20 V* AU Peg WV* 21 24 00.2421322416 +18 16 43.777873164   9.993 9.355 9.203   F8 101 0
21 V* HM Aqr pA* 22 35 27.5260668720 -17 15 26.894587392 9.31 9.08 8.90     A0III 111 0
22 BD+39 4926 pA* 22 46 11.2272974832 +40 06 26.309865960   9.621 9.357 9.374   A0IIp 126 0

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