2014A&A...570A.113M


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.13CEST11:33:27

2014A&A...570A.113M - Astronomy and Astrophysics, volume 570A, 113-113 (2014/10-1)

Large-scale environments of binary AGB stars probed by Herschel. II. Two companions interacting with the wind of π1 Gruis.

MAYER A., JORISSEN A., PALADINI C., KERSCHBAUM F., POURBAIX D., SIOPIS C., OTTENSAMER R., MECINA M., COX N.L.J., GROENEWEGEN M.A.T., KLOTZ D., SADOWSKI G., SPANG A., CRUZALEBES P. and WAELKENS C.

Abstract (from CDS):

The Mass loss of Evolved StarS (MESS) sample observed with PACS on board the Herschel Space Observatory revealed that several asymptotic giant branch (AGB) stars are surrounded by an asymmetric circumstellar envelope (CSE) whose morphology is most likely caused by the interaction with a stellar companion. The evolution of AGB stars in binary systems plays a crucial role in understanding the formation of asymmetries in planetary nebulae (PNe), but at present, only a handful of cases are known where the interaction of a companion with the stellar AGB wind is observed. We probe the environment of the very evolved AGB star π1 Gruis on large and small scales to identify the triggers of the observed asymmetries. Observations made with Herschel/PACS at 70µm and 160µm picture the large-scale environment of π1 Gru. The close surroundings of the star are probed by interferometric observations from the VLTI/AMBER archive. An analysis of the proper motion data of Hipparcos and Tycho-2 together with the Hipparcos Intermediate Astrometric Data help identify the possible cause for the observed asymmetry. The Herschel/PACS images of π1 Gru show an elliptical CSE whose properties agree with those derived from a CO map published in the literature. In addition, an arc east of the star is visible at a distance of 38'' from the primary. This arc is most likely part of an Archimedean spiral caused by an already known G0V companion that is orbiting the primary at a projected distance of 460 au with a period of more than 6200yr. However, the presence of the elliptical CSE, proper motion variations, and geometric modelling of the VLTI/AMBER observations point towards a third component in the system, with an orbital period shorter than 10yr, orbiting much closer to the primary than the G0V star.

Abstract Copyright:

Journal keyword(s): stars: AGB and post-AGB - binaries: general - circumstellar matter - stars: winds, outflows - stars: individual: π1 Gruis - infrared: stars

VizieR on-line data: <Available at CDS (J/A+A/570/A113): list.dat images/*>

Simbad objects: 14

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Number of rows : 14

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 V* R Scl C* 01 26 58.0946233986 -32 32 35.437732667 17.26 9.59 5.72 3.69 2.30 C-N5+ 299 0
2 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1443 0
3 V* TX Cam Mi* 05 00 51.1569959503 +56 10 54.093107078       14.02   M9-9.5 329 0
4 V* UU Aur C* 06 36 32.8375658812 +38 26 43.833646997   7.89 5.25 3.31 1.90 C-N5- 290 1
5 V* R Leo Mi* 09 47 33.4839808805 +11 25 43.823283729 9.22 8.94 7.53 3.39 0.12 M7-9e 872 1
6 V* RW LMi C* 10 16 02.2834693816 +30 34 18.977096332       15.27   C4,3e 380 0
7 V* V Hya C* 10 51 37.2614060865 -21 15 00.339641553   12.23 6.80     C-N:6 342 0
8 V* X Her AB* 16 02 39.1738474892 +47 14 25.258160301   7.64 6.58     M6III 223 0
9 V* W Aql S* 19 15 23.3581458294 -07 02 50.308513461   12.72 10.14     S6/6e 206 0
10 * lam Gru PM* 22 06 06.8856828 -39 32 36.065850   5.843 4.458     K3III 57 0
11 * pi.01 Gru S* 22 22 44.2112214756 -45 56 52.780402708 10.52 8.62 6.55 3.19 0.52 S5,7: 159 0
12 RAFGL 3068 C* 23 19 12.60744 +17 11 33.1332           C 252 0
13 V* R Aqr Sy* 23 43 49.4629939776 -15 17 04.184232557   8.823 7.683 9.37   M6.5-8.5e 740 0
14 * 19 Psc C* 23 46 23.5126056542 +03 29 12.505415198 10.95 7.62 5.02 3.19 1.82 C-N6 432 0

    Equat.    Gal    SGal    Ecl

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2020.08.13-11:33:27

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