2011A&A...532A.135J


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST02:33:33

2011A&A...532A.135J - Astronomy and Astrophysics, volume 532A, 135-135 (2011/8-1)

X Herculis and TX Piscium: two cases of ISM interaction with stellar winds observed by Herschel.

JORISSEN A., MAYER A., VAN ECK S., OTTENSAMER R., KERSCHBAUM F., UETA T., BERGMAN P., BLOMMAERT J.A.D.L., DECIN L., GROENEWEGEN M.A.T., HRON J., NOWOTNY W., OLOFSSON H., POSCH Th., SJOUWERMAN L.O., VANDENBUSSCHE B. and WAELKENS C.

Abstract (from CDS):

The asymptotic giant branch (AGB) stars X Her and TX Psc have been imaged at 70 and 160 µm with the PACS instrument onboard the Herschel satellite, as part of the large MESS (Mass loss of Evolved StarS) guaranteed time key program. The images reveal an axisymmetric extended structure with its axis oriented along the space motion of the stars. This extended structure is very likely to be shaped by the interaction of the wind ejected by the AGB star with the surrounding interstellar medium (ISM). As predicted by numerical simulations, the detailed structure of the wind-ISM interface depends upon the relative velocity between star+wind and the ISM, which is large for these two stars (108 and 55km/s for X Her and TX Psc, respectively). In both cases, there is a compact blob upstream whose origin is not fully elucidated, but that could be the signature of some instability in the wind-ISM shock. Deconvolved images of X Her and TX Psc reveal several discrete structures along the outermost filaments, which could be Kelvin-Helmholtz vortices. Finally, TX Psc is surrounded by an almost circular ring (the signature of the termination shock?) that contrasts with the outer, more structured filaments. A similar inner circular structure seems to be present in X Her as well, albeit less clearly.

Abstract Copyright:

Journal keyword(s): ISM: general - stars: AGB and post-AGB - stars: mass-loss - infrared: stars - stars: carbon

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 NGC 40 PN 00 13 01.0170260109 +72 31 19.032886305   11.63 11.46     [WC8] 588 2
2 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1434 0
3 V* RX Lep AB* 05 11 22.8715425 -11 50 56.722211 8.37 7.14 5.68     M6III 93 0
4 * alf Ori s*r 05 55 10.30536 +07 24 25.4304 4.38 2.27 0.42 -1.17 -2.45 M1-M2Ia-Iab 1464 0
5 V* RS Cnc S* 09 10 38.7978379 +30 57 47.295961 8.65 7.62 5.95 3.06 0.73 M6S 295 0
6 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2133 0
7 V* R Hya Mi* 13 29 42.7818674 -23 16 52.774679 7.26 6.58 4.97 2.27 -0.15 M6-9e 459 0
8 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3715 1
9 QSO B1547+507 QSO 15 49 17.4685620 +50 38 05.788111   18.89 18.74 18.16   ~ 112 1
10 MCG+08-29-036 G 16 02 22.9 +47 14 41   16       ~ 3 0
11 V* X Her AB* 16 02 39.1738474892 +47 14 25.258160301   7.64 6.58     M6III 223 0
12 RAFGL 3068 C* 23 19 12.60744 +17 11 33.1332           C 249 0
13 * 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
14 V* R Cas Mi* 23 58 24.8700291935 +51 23 19.691977266 6.71 6.63 4.80     M6.5-9e 677 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-02:33:33

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