2010A&A...510A..30M


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.24CEST18:19:47

2010A&A...510A..30M - Astronomy and Astrophysics, volume 510, A30-30 (2010/2-1)

Evidence of grain growth in the disk of the bipolar proto-planetary nebula M 1-92.

MURAKAWA K., UETA T. and MEIXNER M.

Abstract (from CDS):

We investigate the dust grain size and dust shell structure of the bipolar proto-planetary nebula M1-92. We performed radiative transfer modeling of the dust shells of M1-92. Our models consists of a disk and bipolar lobes that are surrounded by an AGB shell, each component having different dust characteristics. The model parameters were constrained with the previously obtained spectral energy distribution, the intensity images, the polarization images based on HST/NICMOS archived data as well as the previous radio observations in the CO emission line. Our model geometries with the optically thick disk and lobes with a hollow structure reproduce the bright bipolar lobes of M1-92. The upper limit of the grain size amaxin the lobes is estimated to be 0.5µm from the polarization value in the bipolar lobe. The amaxvalue of the disk is constrained with the disk mass (0.2M), which was estimated from a previous CO emission line observation. We find a good model with amax=1000.0µm, which provides an approximated disk mass of 0.15M. Even taking into account uncertainties such as the gas-to-dust mass ratio, a significantly larger dust of amax>100.0µm, comparing to the dust in the lobe, is expected. We also estimated the disk inner radius, the disk outer radius, the mass-loss rate, and the envelope mass to be 30R*(=9AU), 4500AU, 7.5x10–6[v_exp km/s]M☉_/yr, and 4M_☉, respectively, where vexp is the expansion velocity. If the dust existing in the lobes in large separations from the central star undergoes little dust processing, the dust sizes preserves the ones in the dust formation. Submicron-sized grains are found in many objects besides M∼1-92, suggesting that the size does not depend much on the object properties, such as initial mass of the central star and chemical composition of the stellar system. On the other hand, the grain sizes in the disk do. Evidence of large grains has been reported in many bipolar PPNs, including M1-92. This result suggests that disks play an important role in grain growth.

Abstract Copyright:

Journal keyword(s): keywords: stars: AGB and post-AGB - planetary nebulae: individual: M1-92 - radiative transfer - polarization

Simbad objects: 12

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Number of rows : 12

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 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 723 0
2 V* BM Gem C* 07 20 59.0073994507 +24 59 58.090785507     11.50     C-J5- 140 1
3 IRAS 09371+1212 pA* 09 39 53.96 +11 58 52.6           K7II/III 157 0
4 RAFGL 6815S pA* 17 18 19.8316623567 -32 27 21.376880888           G2I 148 0
5 V* AC Her pA* 18 30 16.2374666779 +21 52 00.618442618 8.00 7.79 7.01     F4Ibp 317 0
6 OH 17.7 -2.0 pA* 18 30 30.703 -14 28 57.04           ~ 135 1
7 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
8 HD 331319 pA* 19 49 29.5621075420 +31 27 16.247184491 10.4 10.196 9.52     F3Ibe 88 0
9 MSB 38 C* 20 36 07.3863551706 +60 05 26.037276961   13.98 9.86 10.3   C-J4+ 116 0
10 V* V1610 Cyg pA* 21 02 18.27 +36 41 37.0           F5Iae 835 1
11 IRAS 22036+5306 pA* 22 05 30.29 +53 21 32.8   19.2       F4III 74 0
12 HD 235858 pA* 22 29 10.3755939027 +54 51 06.341145584   11.40 9.52 8.47 7.34 G5Ia 238 0

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2020.10.24-18:19:47

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