2017A&A...603A..67S


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.25CET14:44:31

2017A&A...603A..67S - Astronomy and Astrophysics, volume 603A, 67-67 (2017/7-1)

A pilot search for mm-wavelength recombination lines from emerging ionized winds in pre-planetary nebulae candidates.

SANCHEZ CONTRERAS C., BAEZ-RUBIO A., ALCOLEA J., BUJARRABAL V. and MARTIN-PINTADO J.

Abstract (from CDS):

We report the results from a pilot search for radio recombination line (RRL) emission at millimeter wavelengths in a small sample of pre-planetary nebulae (pPNe) and young PNe (yPNe) with emerging central ionized regions. Observations of the H30α, H31α, H39α, H41α, H48β, H49β, H51β, and H55γ lines at ∼1 and ∼3mm have been performed with the IRAM 30m radio telescope. These lines are excellent probes of the dense inner (≤150au) and heavily obscured regions of these objects, where the yet unknown agents for PN-shaping originate. We detected mm-RRLs in three objects: CRL 618, MWC 922, and M 2-9. For CRL 618, the only pPN with previous published detections of H41α, H35α, and H30α emission, we find significant changes in the line profiles indicating that current observations are probing regions of the ionized wind with larger expansion velocities and mass-loss rate than ∼29yr ago. In the case of MWC 922, we observe a drastic transition from single-peaked profiles at 3mm (H39α and H41α) to double-peaked profiles at 1mm (H31α and H30α), which is consistent with maser amplification of the highest frequency lines; the observed line profiles are compatible with rotation and expansion of the ionized gas, probably arranged in a disk+wind system around a ∼5-10M central mass. In M 2-9, themm-RRL emission appears to be tracing a recent mass outburst by one of the stars of the central binary system. We present the results from non-LTE line and continuum radiative transfer models, which enables us to constrain the structure, kinematics, and physical conditions (electron temperature and density) of the ionized cores of our sample. We find temperatures Te∼6000-17000K, mean densities ne∼105-108cm–3, radial density gradients ne∝r–α(n) with α(n)∼2-3.5, and motions with velocities of ∼10-30km/s in the ionized wind regions traced by these mm-wavelength observations. We deduce mass-loss rates of MpAGB~=10–6-10–7M/yr, which are significantly higher than the values adopted by stellar evolution models currently in use and would result in a transition from the asymptotic giant branch to the PN phase faster than hitherto assumed.

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: AGB and post-AGB - circumstellar matter - stars: winds, outflows - stars: mass-loss - radio lines: general - HII regions - HII regions

VizieR on-line data: <Available at CDS (J/A+A/603/A67): list.dat fits/*>

Simbad objects: 15

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Number of rows : 15

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 RAFGL 618 pA* 04 42 53.6245215366 +36 06 53.397219192   16.32   12.59   C-rich 945 0
2 NAME Mon R2 IRS 2 * 06 07 45.83 -06 22 53.5           B0 99 0
3 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 709 0
4 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2162 0
5 PN M 2-9 PN 17 05 37.952 -10 08 34.58   12.59 14.7     Be 494 0
6 Hen 3-1475 PN 17 45 14.1763468506 -17 56 46.890631888   13.84 12.87     B7e 186 0
7 Ass Ser OB 1 As* 18 21 -14.4           ~ 69 0
8 EM* MWC 922 Be* 18 21 16.059408 -13 01 25.68432     13.80 13.65   B[e] 82 0
9 Hen 2-437 PN 19 32 57.5 +26 52 41   16.3 15     ~ 90 1
10 Min 1-92 pA* 19 36 18.9292148675 +29 32 49.838032394 12.13 12.35 11.75 11.54   B0.5IV[e] 235 1
11 EM* MWC 349A * 20 32 45.5290328485 +40 39 36.647044678           ~ 142 0
12 LS II +34 26 PN 20 48 16.6322434531 +34 27 24.342089070 10.48 11.11 10.9     B1.5Ia/Iabe 66 0
13 NAME Cepheus A SFR 22 56 17.9 +62 01 49           ~ 692 2
14 NAME Cep A HW 2 Y*O 22 56 17.9 +62 01 49           B0.5 191 0
15 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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2020.01.25-14:44:31

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