2011A&A...528A..39M


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.28CET07:12:46

2011A&A...528A..39M - Astronomy and Astrophysics, volume 528A, 39-39 (2011/4-1)

The influence of binarity on dust obscuration events in the planetary nebula M 2-29 and its analogues.

MISZALSKI B., MIKOLAJEWSKA J., KOEPPEN J., RAUCH T., ACKER A., COHEN M., FREW D.J., MOFFAT A.F.J., PARKER Q.A., JONES A.F. and UDALSKI A.

Abstract (from CDS):

The central star of the planetary nebula (CSPN) M 2-29 shows an extraordinary R Coronae Borealis-like fading event in its optical lightcurve. The only other CSPN to show these events are CPD-56°8032 (Hen 3-1333) and V651 Mon (NGC 2346). Dust cloud formation in the line of sight appears responsible but the exact triggering mechanism is not well understood. Understanding how planetary nebulae (PNe) trigger dust obscuration events may help understand the same process in a wide range of objects including Population-I WC9 stars, symbiotic stars and perhaps asymptotic giant branch (AGB) stars with long secondary periods (LSPs). A binary scenario involving an eccentric, wide companion that triggers dust formation via interaction at periastron is a potential explanation that has been suggested for LSP variables. Model fits to the lightcurves of CPD-56°8032 and M 2-29 show the dust forms in excess of 70AU at the inner edge of a dust disk. In the case of CPD-56°8032 this radius is far too large to coincide with a binary companion trigger, although a binary may have been responsible for the formation of the dust disk. We find no direct evidence to support previous claims of binarity in M 2-29 either from the OGLE lightcurve or deep medium-resolution VLT FLAMES spectroscopy of the CSPN. We classify the CSPN as Of(H) with Teff=50±10 kK and log g=4.0±0.3. We find a mean distance of 7.4±1.8kpc to M 2-29 at which the MV=-0.9mag CSPN could potentially hide a subgiant luminosity or fainter companion. A companion would help explain the multiple similarities with D'-type symbiotic stars whose outer nebulae are thought to be bona-fide PNe. The 7.4 kpc distance, oxygen abundance of 8.3 dex and Galactic coordinates (l=4.0, b=-3.0) prove that M 2-29 is a Galactic Bulge PN and not a Halo PN as commonly misconceived.

Abstract Copyright:

Journal keyword(s): planetary nebulae: individual: PN G004.0-03.0 - stars: AGB and post-AGB - binaries: symbiotic

Simbad objects: 19

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Number of rows : 19

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 V* V471 Per Al* 01 58 49.6642388419 +52 53 48.460982843   14.06 13.08     G2Ib 169 1
2 V* R Vol C* 07 05 36.2092864981 -73 00 52.021676008   14.24 8.70     Ce 79 0
3 NGC 2346 PN 07 09 22.5216571385 -00 48 23.611157830   11.76 11.58     A5V 555 0
4 V* RX Pup Sy* 08 14 12.3036011353 -41 42 29.086820756   12.39 9.00     M5.5 192 1
5 EM* AS 201 PN 08 31 42.8825036476 -27 45 31.541479213   13 11.80     F9III 86 0
6 EGB 6 PN 09 52 58.9867703345 +13 44 34.624573201   15.692 15.999 16.137 16.300 DAO.5 84 0
7 BD+25 2534 HS* 12 37 23.5157891619 +25 03 59.871049394 9.117 10.26 10.59 10.642 10.809 sdB1(k) 210 0
8 V* AE Cir RC* 14 44 51.3303507341 -69 23 34.598549201     13.00     ~ 23 0
9 HD 330036 Em* 15 51 15.92914 -48 44 58.5409   13.09 11.28     F5III-IV 152 1
10 CPD-56 8032 PN 17 09 00.86008 -56 54 48.0957 11.24 11.48 11.04     [WC10] 250 0
11 NGC 6302 PN 17 13 44.339 -37 06 10.95   7.1 10.10     ~ 760 1
12 PN M 1-37 PN 18 05 25.81 -28 22 04.3     14.70     [WC11]? 119 0
13 PN M 2-29 PN 18 06 40.9054663929 -26 54 56.372778872   15.24 14.29 15.15 15.905 ~ 122 0
14 HVC 002.9-06.2-88 HVC 18 16.9 -29 29           ~ 3 0
15 HVC 004.8-06.2+206 HVC 18 21.0 -27 52           ~ 3 0
16 PN M 4-12 PN 19 13 05.239 +15 46 39.80           ~ 78 0
17 NGC 6826 PN 19 44 48.1500835472 +50 31 30.250916761   10.21 9.6     O6fp 701 0
18 V* CI Cyg Al* 19 50 11.8344401438 +35 41 03.000692799   11.97 9.90     Bep+M5III 407 0
19 NAME Galactic Bulge reg ~ ~           ~ 3459 0

    Equat.    Gal    SGal    Ecl

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2020.10.28-07:12:46

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