2024NatAs...8..308D

Query : 2024NatAs...8..308D

2024NatAs...8..308D - Nature Astronomy, 8, 308-327 (2024/March-0)

Chemical tracers of a highly eccentric AGB-main-sequence star binary.

DANILOVICH T., MALFAIT J., VAN DE SANDE M., MONTARGES M., KERVELLA P., DE CEUSTER F., COENEGRACHTS A., MILLAR T.J., RICHARDS A.M.S., DECIN L., GOTTLIEB C.A., PINTE C., DE BECK E., PRICE D.J., WONG K.T., BOLTE J., MENTEN K.M., BAUDRY A., DE KOTER A., ETOKA S., GOBRECHT D., GRAY M., HERPIN F., JESTE M., LAGADEC E., MAES S., McDONALD I., MARINHO L., MULLER H.S.P., PIMPANUWAT B., PLANE J.M.C., SAHAI R., WALLSTROM S.H.J., YATES J. and ZIJLSTRA A.

Abstract (from CDS):

Binary interactions have been proposed to explain a variety of circumstellar structures seen around evolved stars, including asymptotic giant branch (AGB) stars and planetary nebulae. Studies resolving the circumstellar envelopes of AGB stars have revealed spirals, disks and bipolar outflows, with shaping attributed to interactions with a companion. Here we use a combined chemical and dynamical analysis to reveal a highly eccentric and long-period orbit for W Aquilae, a binary system containing an AGB star and a main-sequence companion. Our results are based on anisotropic SiN emission, the detections of irregular NS and SiC emission towards the S-type star, and density structures observed in the CO emission. These features are all interpreted as having formed during periastron interactions. Our astrochemistry-based method can yield stringent constraints on the orbital parameters of long-period binaries containing AGB stars, and will be applicable to other systems.


Abstract Copyright: 2023 The Author(s), under exclusive licence to Springer Nature Limited

Journal keyword(s):

Simbad objects: 16

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Number of rows : 16
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 IRC +10011 OH* 01 06 25.9879717848 +12 35 52.896392052   20.7   18.26 14.01 M8 436 0
2 V* R Scl C* 01 26 58.0939182720 -32 32 35.439234828 17.26 9.59 5.72 3.69 2.30 C-N5+ 354 0
3 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1586 0
4 V* IK Tau OH* 03 53 28.8924743304 +11 24 21.895183368 16.99 14.463 16.171 14.101   M7-11 675 0
5 * L02 Pup AB* 07 13 32.3185436236 -44 38 22.951891964 7.90 6.66 5.10 2.49 0.07 M5IIIe 230 0
6 IRC +10216 C* 09 47 57.40632 +13 16 43.5648           C9,5e 2455 0
7 V* V Hya C* 10 51 37.2615873024 -21 15 00.333928044   12.23 6.80 7.42   C-N:6 391 0
8 WOS 48 C* 15 23 05.0730770544 -51 25 58.762691652   17.85 16.66 14.51 10.18 C 150 1
9 PN M 2-9 PN 17 05 37.96152 -10 08 32.5068           ~ 532 0
10 V* AH Sco s*r 17 11 17.0194487616 -32 19 30.714035556   10.03 8.10     M5Ia-Iab 145 0
11 V* VX Sgr s*r 18 08 04.0442790744 -22 13 26.600899044 11.72 9.41 6.52 3.90 2.11 M8.5Ia 622 0
12 M 57 PN 18 53 35.0967659112 +33 01 44.883287544   15.405 15.769 15.901 16.062 DA(O?) 868 2
13 V* W Aql S* 19 15 23.3572741560 -07 02 50.333886492   12.72 10.14 10.21   S6/6e 251 0
14 IRC -10529 OH* 20 10 27.8731455576 -06 16 13.758742596         15.49 M: 153 0
15 * pi.01 Gru S* 22 22 44.2083897000 -45 56 52.791160956 10.52 8.62 6.55 3.19 0.52 S5,7: 216 0
16 RAFGL 3068 C* 23 19 12.60744 +17 11 33.1332           C 288 1

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