2013A&A...557A.104B


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.28CET10:47:59

2013A&A...557A.104B - Astronomy and Astrophysics, volume 557A, 104-104 (2013/9-1)

Extended rotating disks around post-AGB stars.

BUJARRABAL V., ALCOLEA J., VAN WINCKEL H., SANTANDER-GARCIA M. and CASTRO-CARRIZO A.

Abstract (from CDS):

There is a group of binary post-AGB stars that show conspicuous near-infrared (NIR) excess, which is usually assumed to arise from hot dust in very compact possibly rotating disks. These stars are surrounded by significantly fainter nebulae than the standard, well studied protoplanetary and planetary nebulae (PPNe, PNe). We aim to identify and study extended rotating disks around these stars and shed light on the role of disks in the formation and shaping of planetary nebulae. We present high-sensitivity mm-wave observations of CO lines in 24 objects of this type. The resulting CO lines are compared with profiles expected to arise from rotating disks from both theoretical and observational grounds. We derive simple formulae that allow us to determine the mass of the CO-emitting gas and estimate its extent. The reliability and uncertainty of the methods are also widely discussed. CO emission is detected in most observed sources, and the line profiles show that the emissions very probably come from disks in rotation. We derive typical values of the disk mass between 10–3 and 10–2M about two orders of magnitude lower than the (total) masses of standard PPNe. The high-detection rate (upper limits being not very significant) clearly confirm that the NIR excess of these stars arises from compact disks in rotation, which are likely the inner parts of those found here. Low-velocity outflows are also found in about eight objects with moderate expansion velocities of ∼10km/s to be compared with the velocities of about 100 km/s often found in standard PPNe. Except for two sources with complex profiles, the outflowing gas in our objects represents a minor nebular component. Our simple estimates of the typical disk sizes yields values ∼0.5-1 arcsec, which is between 5x1015 and 3x1016cm. Estimates of the linear momenta carried by the outflows, which can only be performed in a few well studied objects, also yield moderate values when compared to the linear momenta that can be released by the stellar radiation pressure (contrary, again, to the case of the very massive and fast bipolar outflows in standard PPNe that are strongly overluminous). The mass and dynamics of nebulae around various classes of post-AGB stars differ very significantly, and we can expect the formation of PNe with very different properties.

Abstract Copyright:

Journal keyword(s): stars: AGB and post-AGB - circumstellar matter - radio lines: stars - planetary nebulae: general

VizieR on-line data: <Available at CDS (J/A+A/557/A104): stars.dat list.dat fits/*>

Simbad objects: 34

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Number of rows : 34

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 RAFGL 618 pA* 04 42 53.6245215366 +36 06 53.397219192   16.32   12.59   C-rich 961 0
2 V* RV Tau Mi* 04 47 06.7238218181 +26 10 45.530144720   11.00 9.80     K0 266 0
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15129 1
4 V* DY Ori RV* 06 06 14.9086299520 +13 54 19.144206036   11.709 11.29     ~ 46 0
5 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 723 0
6 V* U Mon RV* 07 30 47.4734611972 -09 46 36.788534824 8.22 7.00 5.82     G8/K0Ib/II 194 0
7 V* AI CMi pA* 07 35 41.1518203544 +00 14 57.987903123   9.83 8.31     G5Iab 51 0
8 V* AR Pup RV* 08 03 01.6539854234 -36 35 47.938553885   10.25 9.55     Rpec 81 0
9 CD-44 4961 pA* 08 56 14.1790943091 -44 43 10.710041643   10.55 9.176     F3e 60 1
10 V* IW Car RV* 09 26 53.3043066360 -63 37 48.939300156   9.07 7.90     F7/8 87 0
11 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2174 0
12 HD 89353 pA* 10 18 07.5892879413 -28 59 31.194541133   5.76 5.53     B9.5Ib/II 288 0
13 V* V709 Car pA* 10 19 16.8819372679 -57 19 25.874710095   12.71 11.28     G8Ia-0 14 0
14 HD 93662 pA* 10 47 38.3963525198 -57 28 02.673468362   7.954 6.248     K5/M0(III) 32 0
15 V* V802 Car pA* 11 02 04.3151180751 -62 09 42.834842337   9.57 8.90 9.38   F2III 49 0
16 V* RU Cen RV* 12 09 23.8147186123 -45 25 34.813401164   9.81 8.70     G1Ie 89 0
17 HD 108015 pA* 12 24 53.5038403586 -47 09 07.498401573   8.379 7.96     F3/5Ib/II 56 0
18 IRAS 15469-5311 pA* 15 50 43.8045787664 -53 20 43.254393089   12.03 10.66     F3 22 0
19 IRAS 15556-5444 pA* 15 59 32.5629835254 -54 53 20.455002850           F8 10 0
20 PN M 2-9 PN 17 05 37.952 -10 08 34.58   12.59 14.7     Be 506 0
21 * 89 Her pA* 17 55 25.1884459710 +26 02 59.970100296 5.36 5.70 5.36 5.06 4.94 F2Ibp 390 0
22 V* V2053 Oph pA* 18 14 49.3842596707 +05 12 55.717076925   11.75 10.28     C 39 0
23 V* AC Her pA* 18 30 16.2374666779 +21 52 00.618442618 8.00 7.79 7.01     F4Ibp 318 0
24 V* R Sct RV* 18 47 28.9509385830 -05 42 18.537825839 8.30 6.67 5.20 4.14 3.37 K4/5pec 296 0
25 BD+03 3950 RV* 19 15 01.1800400072 +03 48 42.640112771   11.16 10.37     F8 32 0
26 BD-02 4931 pA* 19 18 22.7164743400 -02 42 10.880951310   11.55 10.78     B1III 30 0
27 Min 1-92 pA* 19 36 18.9292148675 +29 32 49.838032394 12.13 12.35 11.75 11.54   B0.5IV[e] 236 1
28 HD 187885 pA* 19 52 52.7031438648 -17 01 50.293465852   9.25 8.68 8.32   F2/6Ia 170 0
29 V* QY Sge LP* 20 07 54.6188178294 +18 42 54.520818409   12.57       G0Ie 49 0
30 V* R Sge RV* 20 14 03.7424293833 +16 43 35.028513796   10.17 9.20     G8Ib 79 0
31 V* V1610 Cyg pA* 21 02 18.27 +36 41 37.0           F5Iae 836 1
32 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2349 1
33 IRAS 23304+6147 pA* 23 32 44.7854376478 +62 03 49.083515796   15.36 12.99 12.23 10.50 G2Ia 109 0
34 PN M 2-56 pA* 23 56 36.4101419399 +70 48 18.253127954   19.81 17 17.27 17.64 Be 88 0

    Equat.    Gal    SGal    Ecl

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2021.01.28-10:47:59

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